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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.02404">arXiv:1503.02404</a> <span> [<a href="https://arxiv.org/pdf/1503.02404">pdf</a>, <a href="https://arxiv.org/ps/1503.02404">ps</a>, <a href="https://arxiv.org/format/1503.02404">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stv413">10.1093/mnras/stv413 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variation of the ultraviolet extinction law across the Taurus-Auriga star forming complex. A GALEX based study </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+A+I+G">Ana I. Gomez de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Santiago%2C+J">Javier Lopez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Martinez%2C+F">Fatima Lopez-Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+N">Nestor Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">Elisa de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">Manuel Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1503.02404v1-abstract-short" style="display: inline;"> The Taurus-Auriga molecular complex (TMC) is the main laboratory for the study of low mass star formation. The density and properties of interstellar dust are expected to vary across the TMC. These variations trace important processes such as dust nucleation or the magnetic field coupling with the cloud. In this article, we show how the combination of near ultraviolet (NUV) and infrared (IR) photo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02404v1-abstract-full').style.display = 'inline'; document.getElementById('1503.02404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02404v1-abstract-full" style="display: none;"> The Taurus-Auriga molecular complex (TMC) is the main laboratory for the study of low mass star formation. The density and properties of interstellar dust are expected to vary across the TMC. These variations trace important processes such as dust nucleation or the magnetic field coupling with the cloud. In this article, we show how the combination of near ultraviolet (NUV) and infrared (IR) photometry can be used to derive the strength of the 2175 脜 bump and thus any enhancement in the abundance of small dust grains and PAHs in the dust grains size distribution. This technique is applied to the envelope of the TMC, mapped by the GALEX All Sky Survey (AIS). UV and IR photometric data have been retrieved from the GALEX-AIS and the 2MASS catalogues. NUV and K-band star counts have been used to identify the areas in the cloud envelope where the 2175 脜 bump is weaker than in the diffuse ISM namely, the low column density extensions of L1495, L1498 and L1524 in Taurus, L1545, L1548, L1519, L1513 in Auriga and L1482-83 in the California region. This finding agrees with previous results on dust evolution derived from Spitzer data and suggests that dust grains begin to decouple from the environmental galactic magnetic field already in the envelope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02404v1-abstract-full').style.display = 'none'; document.getElementById('1503.02404v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.05223">arXiv:1502.05223</a> <span> [<a href="https://arxiv.org/pdf/1502.05223">pdf</a>, <a href="https://arxiv.org/ps/1502.05223">ps</a>, <a href="https://arxiv.org/format/1502.05223">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201219095">10.1051/0004-6361/201219095 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analysis of combined radial velocities and activity of BD+20 1790: evidence supporting the existence of a planetary companion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Obispo%2C+M">M. Hern谩n-Obispo</a>, <a href="/search/astro-ph?searchtype=author&query=Tuomi%2C+M">M. Tuomi</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lvez-Ortiz%2C+M+C">M. C. G谩lvez-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Golovin%2C+A">A. Golovin</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+J+R">J. R. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+H+R+A">H. R. A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Kane%2C+S+R">S. R. Kane</a>, <a href="/search/astro-ph?searchtype=author&query=Pinfield%2C+D">D. Pinfield</a>, <a href="/search/astro-ph?searchtype=author&query=Jenkins%2C+J+S">J. S. Jenkins</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+P">P. Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada-Escud%C3%A9%2C+G">G. Anglada-Escud茅</a>, <a href="/search/astro-ph?searchtype=author&query=Marsden%2C+S+C">S. C. Marsden</a>, <a href="/search/astro-ph?searchtype=author&query=Catal%C3%A1n%2C+S">S. Catal谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffers%2C+S+V">S. V. Jeffers</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">E. de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%A9s%2C+A">A. Garc茅s</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+M+I">M. I. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Gorlova%2C+N">N. Gorlova</a>, <a href="/search/astro-ph?searchtype=author&query=Andreev%2C+M">M. Andreev</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1502.05223v1-abstract-short" style="display: inline;"> This paper presents the simultaneous Bayesian analysis of the radial velocity and activity indices for the K5Ve active star BD+20 1790, that was proposed to host a close-in massive planet by Hern谩n-Obispo et al. (2010). The Bayesian analysis supports the hypothesis of a planetary companion. We present a new orbital solution after removing the two main contributions to the stellar jitter, one that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.05223v1-abstract-full').style.display = 'inline'; document.getElementById('1502.05223v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.05223v1-abstract-full" style="display: none;"> This paper presents the simultaneous Bayesian analysis of the radial velocity and activity indices for the K5Ve active star BD+20 1790, that was proposed to host a close-in massive planet by Hern谩n-Obispo et al. (2010). The Bayesian analysis supports the hypothesis of a planetary companion. We present a new orbital solution after removing the two main contributions to the stellar jitter, one that varies with the photometric period and another that varies with the synodic period of the star+planet system. We use a new method to determine these jitter components, considering them as a second and third signals in the system. A discussion on possible magnetic star-planet-interaction is included, based on the Bayesian analysis of the activity indices. We propose two possible sources for flare events of this star: one related to the geometry of the system and the relative movement of the star+planet, and a second one purely stochastic source that is related to the evolution of stellar active regions. Also, we observe for the first time the magnetic field of the star, from spectropolarimetric data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.05223v1-abstract-full').style.display = 'none'; document.getElementById('1502.05223v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 18 figures, accepted for publication at A\&A (!2 January 2015)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.3002">arXiv:1412.3002</a> <span> [<a href="https://arxiv.org/pdf/1412.3002">pdf</a>, <a href="https://arxiv.org/ps/1412.3002">ps</a>, <a href="https://arxiv.org/format/1412.3002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0067-0049/216/2/26">10.1088/0067-0049/216/2/26 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A GALEX based search for the sparse young stellar population in the Taurus-Aurigae star forming region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+A+I+G">Ana I. Gomez de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Santiago%2C+J">Javier L贸pez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Mart%C3%ADnez%2C+F">F谩tima L贸pez-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+N">N茅stor S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+P">Paola Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">Elisa de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">Manuel Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=Gestoso%2C+J+Y">Javier Ya帽ez Gestoso</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1412.3002v1-abstract-short" style="display: inline;"> In this work, we identify 63 bona fide new candidates to T Tauri stars (TTSs) in the Taurus-Auriga region using as baseline its ultraviolet excess. The initial data set has been defined from the GALEX all sky survey (AIS). The GALEX satellite obtained images in the near ultraviolet (NUV) and far ultraviolet (FUV) bands where the TTSs show a prominent excess, compared with main sequence or giants s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.3002v1-abstract-full').style.display = 'inline'; document.getElementById('1412.3002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.3002v1-abstract-full" style="display: none;"> In this work, we identify 63 bona fide new candidates to T Tauri stars (TTSs) in the Taurus-Auriga region using as baseline its ultraviolet excess. The initial data set has been defined from the GALEX all sky survey (AIS). The GALEX satellite obtained images in the near ultraviolet (NUV) and far ultraviolet (FUV) bands where the TTSs show a prominent excess, compared with main sequence or giants stars. GALEX AIS surveyed the Taurus-Auriga molecular complex, as well as, a fraction of the California Nebula and the Perseus complex; bright sources and the dark clouds themselves are avoided. The properties of the TTSs in the ultraviolet (GALEX), optical (UCAC4) and infrared (2MASS) have been defined using as qualification sample the TTSs observed with the International Ultraviolet Explorer. The candidates have been identified by means of a mixed ultraviolet-optical-infrared excess set of colors; it is found that the color-color diagram FUV-NUV versus J-K is ideally suited for this purpose. From an initial sample of 163,313 bona-fide NUV sources, a final list with 63 new candidates to TTSs in the region has been produced. The search procedure has been validated by its ability to detect all known TTSs in the area surveyed: 31 TTSs. Also, it is shown that the weak-lined TTSs are located in a well defined stripe in the FUV-NUV versus J-K diagram. Moreover, we provide in this work a list of TTSs photometric standards for future GALEX-based studies of the young stellar population in star forming regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.3002v1-abstract-full').style.display = 'none'; document.getElementById('1412.3002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astrophysical Journal Supp. Series, accepted (Dec 3rd 2014)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1002.1663">arXiv:1002.1663</a> <span> [<a href="https://arxiv.org/pdf/1002.1663">pdf</a>, <a href="https://arxiv.org/ps/1002.1663">ps</a>, <a href="https://arxiv.org/format/1002.1663">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200913437">10.1051/0004-6361/200913437 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-resolution spectroscopic survey of late-type stars: chromospheric activity, rotation, kinematics, and age </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopez-Santiago%2C+J">J. Lopez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Galvez-Ortiz%2C+M+C">M. C. Galvez-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo-Chacon%2C+I">I. Crespo-Chacon</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez-Arnaiz%2C+R+M">R. M. Martinez-Arnaiz</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1002.1663v1-abstract-short" style="display: inline;"> Aims: We present a compilation of spectroscopic data from a survey of 144 chromospherically active young stars in the solar neighborhood which may be used to investigate different aspects of the formation and evolution of the solar neighborhood in terms of kinematics and stellar formation history. The data have already been used by us in several studies. With this paper, we make all these data a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.1663v1-abstract-full').style.display = 'inline'; document.getElementById('1002.1663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1002.1663v1-abstract-full" style="display: none;"> Aims: We present a compilation of spectroscopic data from a survey of 144 chromospherically active young stars in the solar neighborhood which may be used to investigate different aspects of the formation and evolution of the solar neighborhood in terms of kinematics and stellar formation history. The data have already been used by us in several studies. With this paper, we make all these data accessible to the scientific community for future studies on different topics. Methods: We performed spectroscopic observations with echelle spectrographs to cover the entirety of the optical spectral range simultaneously. Standard data reduction was performed with the IRAF ECHELLE package. We applied the spectral subtraction technique to reveal chromospheric emission in the stars of the sample. The equivalent width of chromospheric emission lines was measured in the subtracted spectra and then converted to fluxes using equivalent width-flux relationships. Radial and rotational velocities were determined by the cross-correlation technique. Kinematics, equivalent widths of the lithium line 6707.8 angstroms and spectral types were also determined. Results: A catalog of spectroscopic data is compiled: radial and rotational velocities, space motion, equivalent widths of optical chromospheric activity indicators from Ca II H & K to the calcium infrared triplet and the lithium line in 6708 angstroms. Fluxes in the chromospheric emission lines and R'HK are also determined for each observation of star in the sample. We used these data to investigate the emission levels of our stars. The study of the Halpha emission line revealed the presence of two different populations of chromospheric emitters in the sample, clearly separated in the log F(Halpha)/Fbol - (V-J) diagram. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1002.1663v1-abstract-full').style.display = 'none'; document.getElementById('1002.1663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 February, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A. 56 pages, 7 pages. Online material: 4 tables and 27 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1001.0662">arXiv:1001.0662</a> <span> [<a href="https://arxiv.org/pdf/1001.0662">pdf</a>, <a href="https://arxiv.org/ps/1001.0662">ps</a>, <a href="https://arxiv.org/format/1001.0662">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1002/asna.200911337">10.1002/asna.200911337 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Finding the most variable stars in the Orion Belt with the All Sky Automated Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">Jose A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">E. de Castro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1001.0662v1-abstract-short" style="display: inline;"> We look for high-amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS-3 Photometric V-band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5 deg centred on the bright st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1001.0662v1-abstract-full').style.display = 'inline'; document.getElementById('1001.0662v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1001.0662v1-abstract-full" style="display: none;"> We look for high-amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS-3 Photometric V-band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5 deg centred on the bright star Alnilam (eps Ori) in the centre of the Orion Belt. We identify 32 highly-variable stars, of which 16 had not been reported to vary before. They are mostly variable young stars and candidates (16) and background giants (8), but there are also field cataclysmic variables, contact binaries, and eclipsing binary candidates. Of the young stars, which typically are active Herbig Ae/Be and T Tauri stars with Halpha emission and infrared flux excess, we discover four new variables and confirm the variability status of another two. Some of them belong to the well known sigma Orionis cluster. Besides, six of the eight giants are new variables, and three are new periodic variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1001.0662v1-abstract-full').style.display = 'none'; document.getElementById('1001.0662v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomische Nachrichten, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0912.2773">arXiv:0912.2773</a> <span> [<a href="https://arxiv.org/pdf/0912.2773">pdf</a>, <a href="https://arxiv.org/ps/0912.2773">ps</a>, <a href="https://arxiv.org/format/0912.2773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/200811000">10.1051/0004-6361/200811000 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of a massive planet candidate orbiting the young active K5V star BD+20 1790 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Obispo%2C+M">M. Hern谩n-Obispo</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lvez-Ortiz%2C+M+C">M. C. G谩lvez-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Anglada-Escud%C3%A9%2C+G">G. Anglada-Escud茅</a>, <a href="/search/astro-ph?searchtype=author&query=Kane%2C+S+R">S. R. Kane</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+J+R">J. R. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">E. de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0912.2773v1-abstract-short" style="display: inline;"> BD+20 1790 is a young active, metal-rich, late-type K5Ve star. We have undertaken a study of stellar activity and kinematics for this star over the past few years. Previous results show a high level of stellar activity, with the presence of prominence-like structures, spots on the surface and strong flare events, despite the moderate rotational velocity of the star. In addition, radial velocity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2773v1-abstract-full').style.display = 'inline'; document.getElementById('0912.2773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0912.2773v1-abstract-full" style="display: none;"> BD+20 1790 is a young active, metal-rich, late-type K5Ve star. We have undertaken a study of stellar activity and kinematics for this star over the past few years. Previous results show a high level of stellar activity, with the presence of prominence-like structures, spots on the surface and strong flare events, despite the moderate rotational velocity of the star. In addition, radial velocity variations with a semi-amplitude of up to 1 km/s were detected. We investigated the nature of these radial velocity variations, in order to determine whether they are due to stellar activity or the reflex motion of the star induced by a companion. We have analysed high-resolution echelle spectra and also two-band photometry was obtained to produce the light curve and determine the photometric period. Based upon the analysis of the bisector velocity span, as well as spectroscopic indices of chromospheric indicators and taking into account the photometric analysis, we report that the best explanation for the RV variation is the presence of a sub-stellar companion. The Keplerian fit of the RV data yields a solution for a close-in massive planet with an orbital period of 7.78 days. The presence of the close-in massive planet could also be an interpretation for the high level of stellar activity detected. Since the RV data are not part of a planet search program, we can consider our results as a serendipitous evidence of a planetary companion. To date, this is the youngest main sequence star for which a planetary candidate has been reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0912.2773v1-abstract-full').style.display = 'none'; document.getElementById('0912.2773v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 December, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 14 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0903.4814">arXiv:0903.4814</a> <span> [<a href="https://arxiv.org/pdf/0903.4814">pdf</a>, <a href="https://arxiv.org/ps/0903.4814">ps</a>, <a href="https://arxiv.org/format/0903.4814">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/137/6/5012">10.1088/0004-6256/137/6/5012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray variability of sigma Orionis young stars with ROSAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+J+A">J. A. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Santiago%2C+J">J. Lopez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=de+Castro%2C+E">E. de Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0903.4814v1-abstract-short" style="display: inline;"> We used the Aladin Virtual Obsrvatory tool and High Resolution Imager ROSAT archival data to search for X-ray variability in scale of days in 23 young stars in the sigma Orionis cluster and a background galaxy. Five stars displayed unambiguous flares and had probabilities p_var >> 99% of being actual variables. Two of the detected flares were violent and long-lasting, with maximum duration of si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.4814v1-abstract-full').style.display = 'inline'; document.getElementById('0903.4814v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0903.4814v1-abstract-full" style="display: none;"> We used the Aladin Virtual Obsrvatory tool and High Resolution Imager ROSAT archival data to search for X-ray variability in scale of days in 23 young stars in the sigma Orionis cluster and a background galaxy. Five stars displayed unambiguous flares and had probabilities p_var >> 99% of being actual variables. Two of the detected flares were violent and long-lasting, with maximum duration of six days and amplitude of eight times above the quiescent level. We classified another four stars as possible X-ray variables, including the binary system formed by the B2Vp star sigma Ori E and its close late-type companion. This makes a minimum frequency of high-amplitude X-ray variability in excess of a day of 39% among sigma Orionis stars. The incidence of this kind of X-ray variability seems to be lower among classical T Tauri stars with mid-infrared flux excesses than among fast-rotating, disk-less young stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.4814v1-abstract-full').style.display = 'none'; document.getElementById('0903.4814v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">AJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0901.1634">arXiv:0901.1634</a> <span> [<a href="https://arxiv.org/pdf/0901.1634">pdf</a>, <a href="https://arxiv.org/ps/0901.1634">ps</a>, <a href="https://arxiv.org/format/0901.1634">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/137/4/3965">10.1088/0004-6256/137/4/3965 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength optical observations of two chromospherically active binary systems: V789 Mon and GZ Leo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lvez%2C+M+C">M. C. G谩lvez</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Figueroa%2C+M+J">M. J. Fern谩ndez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0901.1634v1-abstract-short" style="display: inline;"> This paper describes a multiwavelengh optical study of chromospheres in two X-ray/EUV selected active binary stars with strong H_alpha emission, V789 Mon (2RE J0725-002) and GZ Leo (2RE J1101+223). The goal of the study is to determine radial velocities and fundamental stellar parameters in chromospherically active binary systems in order to include them in the activity-rotation and activity-age… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1634v1-abstract-full').style.display = 'inline'; document.getElementById('0901.1634v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0901.1634v1-abstract-full" style="display: none;"> This paper describes a multiwavelengh optical study of chromospheres in two X-ray/EUV selected active binary stars with strong H_alpha emission, V789 Mon (2RE J0725-002) and GZ Leo (2RE J1101+223). The goal of the study is to determine radial velocities and fundamental stellar parameters in chromospherically active binary systems in order to include them in the activity-rotation and activity-age relations. We carried out high resolution echelle spectroscopic observations and applied spectral subtraction technique in order to measure emission excesses due to chromosphere. The detailed study of activity indicators allowed us to characterize the presence of different chromospheric features in these systems and enabled to include them in a larger activity-rotation survey. We computed radial velocities of the systems using cross correlation with the radial velocity standards. The double-line spectral binarity was confirmed and the orbital solutions improved for both systems. In addition, other stellar parameters such as: spectral types, projected rotational velocities (vsini), and the equivalent width of the lithium LiI 6707.8 AA absorption line were determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0901.1634v1-abstract-full').style.display = 'none'; document.getElementById('0901.1634v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 18 pages, 10 figures. Available at http://www.ucm.es/info/Astrof/invest/actividad/actividad_pub.html Accepted for publication in: Astronomical Journal (AJ)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0706.3665">arXiv:0706.3665</a> <span> [<a href="https://arxiv.org/pdf/0706.3665">pdf</a>, <a href="https://arxiv.org/ps/0706.3665">ps</a>, <a href="https://arxiv.org/format/0706.3665">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20067015">10.1051/0004-6361:20067015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength optical observations of chromospherically active binary systems V. FF UMa (2RE J0933+624): a system with orbital period variation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lvez%2C+M+C">M. C. G谩lvez</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Figueroa%2C+M+J">M. J. Fern谩ndez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0706.3665v1-abstract-short" style="display: inline;"> This is the fifth paper in a series aimed at studying the chromospheres of active binary systems using several optical spectroscopic indicators to obtain or improve orbital solution and fundamental stellar parameters. We present here the study of FF UMa (2RE J0933+624), a recently discovered, X-ray/EUV selected, active binary with strong H_alpha emission. The objectives of this work are, to find… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.3665v1-abstract-full').style.display = 'inline'; document.getElementById('0706.3665v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0706.3665v1-abstract-full" style="display: none;"> This is the fifth paper in a series aimed at studying the chromospheres of active binary systems using several optical spectroscopic indicators to obtain or improve orbital solution and fundamental stellar parameters. We present here the study of FF UMa (2RE J0933+624), a recently discovered, X-ray/EUV selected, active binary with strong H_alpha emission. The objectives of this work are, to find orbital solutions and define stellar parameters from precise radial velocities and carry out an extensive study of the optical indicators of chromospheric activity. We obtained high resolution echelle spectroscopic observations during five observing runs from 1998 to 2004. We found radial velocities by cross correlation with radial velocity standard stars to achieve the best orbital solution. We also measured rotational velocity by cross-correlation techniques and have studied the kinematic by galactic space- velocity components (U, V, W) and Eggen criteria. Finally, we have determined the chromospheric contribution in optical spectroscopic indicators, from Ca II H & K to Ca II IRT lines, using the spectral subtraction technique. We have found that this system presents an orbital period variation, higher than previously detected in other RS CVn systems. We determined an improved orbital solution, finding a circular orbit with a period of 3.274 days. We derived the stellar parameters, confirming the subgiant nature of the primary component and obtained rotational velocities (vsini), of 33.57 km/s and 32.38 km/s for the primary and secondary components respectively. From our kinematic study, we can deduce its membership to the Castor moving group. Finally, the activity study has given us a better understanding of the possible mechanisms that produce the orbital period variation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.3665v1-abstract-full').style.display = 'none'; document.getElementById('0706.3665v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 16 pages, 18 figures. Available at http://www.ucm.es/info/Astrof/invest/actividad/actividad_pub.html Accepted for publication in: Astronomy & Astrophysics (A&A)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0204490">arXiv:astro-ph/0204490</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0204490">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0204490">ps</a>, <a href="https://arxiv.org/format/astro-ph/0204490">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20020644">10.1051/0004-6361:20020644 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength optical observations of chromospherically active binary systems. IV. The X-ray/EUV selected binary BK Psc (2RE J0039+103) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galvez%2C+M+C">M. C. Galvez</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Santiago%2C+J">J. Lopez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0204490v1-abstract-short" style="display: inline;"> We present high resolution echelle spectra taken during four observing runs from 1999 to 2001 of the recently X-ray/EUV selected chromospherically active binary BK Psc (2RE J0039+103). Our observations confirm the single-lined spectroscopic binary(SB1) nature of this system and allow us to obtain, for the first time,the orbital solution of the system as in the case of a SB2 system. We have deter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0204490v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0204490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0204490v1-abstract-full" style="display: none;"> We present high resolution echelle spectra taken during four observing runs from 1999 to 2001 of the recently X-ray/EUV selected chromospherically active binary BK Psc (2RE J0039+103). Our observations confirm the single-lined spectroscopic binary(SB1) nature of this system and allow us to obtain, for the first time,the orbital solution of the system as in the case of a SB2 system. We have determined precise radial velocities of both components: for the primary by using the cross correlation technique, and for the secondary by using its chromospheric emission lines. We have obtained a circular orbit with an orbital period of 2.1663 days, very close to its photometric period of 2.24 days (indicating synchronous rotation). The spectral type (K5V) we determined for our spectra and the mass ratio (1.8) and minimum masses (Msin^{3}i) resulting from the orbital solution are compatible with the observed K5V primary and an unseen M3V secondary. Using this spectral classification, the projected rotational velocity (vsini, of 17.1 km/s}) obtained from the width of the cross-correlation function and the data provided by Hipparcos, we have derived other fundamental stellar parameters. The kinematics and the non-detection of the LiI line indicate that it is an old star. The analysis of the optical chromospheric activity indicators from the CaII H & K to CaII IRT lines, by using the spectral subtraction technique, indicates that both components of the binary system show high levels of chromospheric activity. H_alpha emission above the continuum from both components is a persistent feature of this system during the period 1999 to 2001 of our observations as well as in previous observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0204490v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0204490v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 April, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 13 pages, 5 figures tar'ed gzip'ed. Full postscript (text and figures) available at http://www.ucm.es/info/Astrof/pub_dmg.html Accepted for publication in: Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0106537">arXiv:astro-ph/0106537</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0106537">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0106537">ps</a>, <a href="https://arxiv.org/format/astro-ph/0106537">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1046/j.1365-8711.2001.04781.x">10.1046/j.1365-8711.2001.04781.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Late-type stars members of young stellar kinematic groups - I. Single stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Santiago%2C+J">J. Lopez-Santiago</a>, <a href="/search/astro-ph?searchtype=author&query=Galvez%2C+M+C">M. C. Galvez</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0106537v1-abstract-short" style="display: inline;"> This is the first paper of a series aimed at studying the properties of late-type stars members of young stellar kinematic groups. We concentrate our study on classical young moving groups as: Local Association (Pleiades moving group, 20 - 150 Myr), IC 2391 supercluster (35 Myr), Ursa Major group (Sirius supercluster, 300 Myr), and Hyades supercluster (600 Myr); as well as on recently identified… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106537v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0106537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0106537v1-abstract-full" style="display: none;"> This is the first paper of a series aimed at studying the properties of late-type stars members of young stellar kinematic groups. We concentrate our study on classical young moving groups as: Local Association (Pleiades moving group, 20 - 150 Myr), IC 2391 supercluster (35 Myr), Ursa Major group (Sirius supercluster, 300 Myr), and Hyades supercluster (600 Myr); as well as on recently identified groups as: Castor moving group (200 Myr). In this paper we have compiled a preliminary list of single late-type stars possible members of some of these young stellar kinematic groups. Stars have been selected from previously established members of stellar kinematic groups based on photometric and kinematic properties as well as from candidates based on other criteria as their level of chromospheric activity, rotation rate, lithium abundance. Precise measurements of proper motions and parallaxes taken from Hipparcos Catalogue, as well as from Tycho-2 Catalogue, and published radial velocity measurements are used to calculate the Galactic space motions (U, V, W) and to apply the Eggen's kinematic criteria in order to determine the membership of the selected stars to the different groups. Additional criteria using age-dating methods for late-type stars will be applied in forthcoming papers of this series. A further study of the list of stars compiled here could lead to a better understanding of the chromospheric activity and their age evolution as well as of the star formation history in the solar neighbourhood. In addition, these stars are also potential search targets for direct imaging detection of sub-stellar companions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106537v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0106537v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 June, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2001. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 10 pages, 3 figures tar'ed gzip'ed. Full postscript (text and figures) available at http://www.ucm.es/info/Astrof/MB88.ps.gz Tables and catalogue of stars available at http://www.ucm.es/info/Astrof/skg/skg_catalogue.html Accepted for publication in: Monthly Notices of the Royal Astronomical Society (MNRAS)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc.328:45,2001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0007041">arXiv:astro-ph/0007041</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0007041">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0007041">ps</a>, <a href="https://arxiv.org/format/astro-ph/0007041">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/aas:2000359">10.1051/aas:2000359 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength optical observations of chromospherically active binary systems. III. High resolution echelle spectra from Ca II H&K to Ca II IRT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=Latorre%2C+A">A. Latorre</a>, <a href="/search/astro-ph?searchtype=author&query=Sanz-Forcada%2C+J">J. Sanz-Forcada</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0007041v1-abstract-short" style="display: inline;"> This is the third paper of a series aimed at studying the chromosphere of active binary systems using the information provided for several optical spectroscopic features. High resolution echelle spectra including all the optical chromospheric activity indicators from the Ca II H & K to Ca II IRT lines are analysed here for 16 systems. The chromospheric contribution in these lines has been determ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007041v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0007041v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0007041v1-abstract-full" style="display: none;"> This is the third paper of a series aimed at studying the chromosphere of active binary systems using the information provided for several optical spectroscopic features. High resolution echelle spectra including all the optical chromospheric activity indicators from the Ca II H & K to Ca II IRT lines are analysed here for 16 systems. The chromospheric contribution in these lines has been determined using the spectral subtraction technique. Very broad wings have been found in the subtracted H_alpha profile of the very active star HU Vir. These profiles are well matched using a two-component Gaussian fit (narrow and broad) and the broad component can be interpreted as arising from microflaring. Red-shifted absorption features in the H_alpha line have been detected in several systems and excess emission in the blue wing of FG UMa was also detected. These features indicate that several dynamical processes, or a combination of them, may be involved. Using the E(H_alpha)/E(H_beta) ratio as a diagnostic we have detected prominence-like extended material viewed off the limb in many stars of the sample, and prominences viewed against the disk at some orbital phases in the dwarfs OU Gem and BF Lyn. The He I D_3 line has been detected as an absorption feature in mainly all the giants of the sample. Total filling-in of the He I D_3, probably due to microflaring activity, is observed in HU Vir. Self-absorption with red asymmetry is detected in the Ca II H & K lines of the giants 12 Cam, FG UMa and BM CVn. All the stars analysed show clear filled-in Ca II IRT lines or even notable emission reversal. The small values of the E(8542)/E(8498) ratio we have found indicate Ca II IRT emission arises from plage-like regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0007041v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0007041v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 July, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 38 pages, 25 figures. Full postscript (text and figures) available at http://www.ucm.es/info/Astrof/pub_dmg.html To be published in Astronomy & Astrophysics Supp. S</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9912161">arXiv:astro-ph/9912161</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9912161">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9912161">ps</a>, <a href="https://arxiv.org/format/astro-ph/9912161">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Chromospherically active binaries members of young stellar kinematic groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=Latorre%2C+A">A. Latorre</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9912161v1-abstract-short" style="display: inline;"> We present a kinematic study of a large sample of chromospherically active binaries (CAB) in order to determine their membership to representative young disk stellar kinematic groups: the Local Association (Pleiades moving group, 20 - 150 Myr), Ursa Mayor group (Sirius supercluster, 300 Myr), Hyades supercluster (800 Myr), IC 2391 supercluster (35 Myr) and Castor moving group (200 Myr). Precise… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9912161v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9912161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9912161v1-abstract-full" style="display: none;"> We present a kinematic study of a large sample of chromospherically active binaries (CAB) in order to determine their membership to representative young disk stellar kinematic groups: the Local Association (Pleiades moving group, 20 - 150 Myr), Ursa Mayor group (Sirius supercluster, 300 Myr), Hyades supercluster (800 Myr), IC 2391 supercluster (35 Myr) and Castor moving group (200 Myr). Precise measurements of proper motions and parallaxes taken from Hipparcos Catalogue and published radial velocity measurements are used to calculate Galactic space motions (U, V, W) in order to determine the membership of the selected stars to the different stellar kinematic groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9912161v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9912161v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 December, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 1999. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 6 pages, 4 figures. Also available at http://www.ucm.es/info/Astrof/cabs_yskg.html to be published in ASP Conf. Ser., The 11th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, (October 4th - 8th, 1999, Puerto de la Cruz, Tenerife, Spain), R. Garcia Lopez, R. Rebolo, M.R. Zapatero Osorio (eds.)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9905244">arXiv:astro-ph/9905244</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9905244">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9905244">ps</a>, <a href="https://arxiv.org/format/astro-ph/9905244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> The age-mass relation for chromospherically active binaries: III. Lithium depletion in giant components </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R+J+G">R. J. Garcia Lopez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9905244v1-abstract-short" style="display: inline;"> We present a study of the lithium abundances of a sample of evolved components of Chromospherically Active Binary Systems. We show that a significant part of them have lithium excesses, independently of their mass and evolutionary stage. Therefore, it can be concluded that Li abundance does not depend on age for giant components of CABS. These overabundances appear to be closely related to the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9905244v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9905244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9905244v1-abstract-full" style="display: none;"> We present a study of the lithium abundances of a sample of evolved components of Chromospherically Active Binary Systems. We show that a significant part of them have lithium excesses, independently of their mass and evolutionary stage. Therefore, it can be concluded that Li abundance does not depend on age for giant components of CABS. These overabundances appear to be closely related to the stellar rotation, and we interpret them as a consequence of the transfer of angular momentum from the orbit to the rotation as the stars evolve in and off the Main Sequence, in a similar way as it happens in the dwarf components of the same systems and in the Tidally Locked Binaries belonging to the Hyades and M67. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9905244v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9905244v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 1999; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 1999. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron.Astrophys.377:739,1998 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9809119">arXiv:astro-ph/9809119</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9809119">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9809119">ps</a>, <a href="https://arxiv.org/format/astro-ph/9809119">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Multiwavelength optical observations of the chromospherically active binary system MS Ser </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sanz-Forcada%2C+J">J. Sanz-Forcada</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9809119v1-abstract-short" style="display: inline;"> We present here a continuation of our ongoing project of multiwavelength optical observations aimed at studying the chromosphere of active binary systems using the information provided for several optical spectroscopic features that are formed at different heights in the chromosphere (Montes et al. 1997, 1998; Sanz-Forcada et al. 1998). In this contribution we focus our study on the preliminar a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9809119v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9809119v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9809119v1-abstract-full" style="display: none;"> We present here a continuation of our ongoing project of multiwavelength optical observations aimed at studying the chromosphere of active binary systems using the information provided for several optical spectroscopic features that are formed at different heights in the chromosphere (Montes et al. 1997, 1998; Sanz-Forcada et al. 1998). In this contribution we focus our study on the preliminar analysis of the active binary system MS Ser. We have taken H$伪$ and H$尾$ spectra in 1995 with the Coude Spectrograph at 2.2m telescope in Calar Alto, and high resolution SOFIN echelle spectra (covering H_alpha, H_beta, Na I D_{1} and D_{2}, He I D_{3}, Mg I b triplet, Ca II H & K, and Ca II infrared triplet lines) in 1998 with the 2.56m Nordic Optical Telescope (NOT) in La Palma. A strong emission in the Ca II H & K and Ca II IRT lines, coming from the primary component (recently classified as K2IV) is observed. One of the Ca II H & K spectra (at orbital phase near quadrature) reveals that the secondary (G8V) also exhibit a small emission. A near complete and variable filling-in of the H_alpha and H_beta is obtained after the application of the spectral subtraction technique. We detect also some seasonal variations between these two observing runs and in comparation with our previous Ca II H & K observations taken in 1993 (Montes et al. 1995). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9809119v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9809119v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 1998; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1998. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Latex file with 5 figures tar'ed gzip'ed. Full postscript (text & figures) available at http://www.ucm.es/OTROS/Astrof/pub_dmg.html, to be published in ASP Conf. Ser., Solar and Stellar Activity: Similarities and Differences (meeting dedicated to Brendan Byrne, Armagh 2-4th Sep. 1998) C.J. Butler and J.G. Doyle, eds</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9703199">arXiv:astro-ph/9703199</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9703199">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9703199">ps</a>, <a href="https://arxiv.org/format/astro-ph/9703199">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> The Age-Mass Relation for Chromospherically Active Binaries. II. Lithium Depletion in Dwarf Components </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Navascues%2C+D+B+y">D. Barrado y Navascues</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R+J+G">R. J. Garcia Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9703199v1-abstract-short" style="display: inline;"> We present an extensive study of lithium abundances in dwarf components of chromospherically active binary stars (CABS). Since most of these binaries have known radii, masses and ages, this kind of data is especially useful for comparisons with theoretical models which try to explain the Li depletion phenomenon. We show that a significant part of these stars have clear Li overabundances. These e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9703199v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9703199v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9703199v1-abstract-full" style="display: none;"> We present an extensive study of lithium abundances in dwarf components of chromospherically active binary stars (CABS). Since most of these binaries have known radii, masses and ages, this kind of data is especially useful for comparisons with theoretical models which try to explain the Li depletion phenomenon. We show that a significant part of these stars have clear Li overabundances. These excesses are evident when comparing our sample of CABS with binary and single stars belonging to open clusters of different ages, namely Pleiades, Hyades, NGC752, M67 and NGC188. The Li excesses are more conspicuous for masses in the range 0.75-0.95 Mo, indicating that the rate of Li depletion has been less pronounced in CABS than in single stars. This phenomenon is interpreted in the context of transport of angular momentum from the orbit to the stellar rotation due to tidal effects. Other explanations, however, can not be ruled out. This is the case of transport of material induced by internal gravity waves, which could be inhibited due to the presence of strong magnetic fields associated with the effective dynamo in CABS. The confirmed existence of a relation between Li and fluxes in CaII H&K lines can also be accommodated within both scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9703199v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9703199v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 March, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 1997. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, LATEX file. Astronomy and Astrophysics style macro (l-aa.sty). Accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9609203">arXiv:astro-ph/9609203</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9609203">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9609203">ps</a>, <a href="https://arxiv.org/format/astro-ph/9609203">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/aas:1997170">10.1051/aas:1997170 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Library of high and mid-resolution spectra in the CaII H & K, H{alpha}, H{beta}, NaI D{1}, D{2}, and HeI D{3} line regions of F, G, K and M field stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+E+L">E. L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9609203v1-abstract-short" style="display: inline;"> In this work we present spectroscopic observations centered in the spectral lines most widely used as optical indicators of chromospheric activity (H{alpha}, H{beta}, Ca II H & K, and He I D{3}) in a sample of F, G, K and M chromospherically inactive stars. The spectra have been obtained with the aim of providing a library of high and mid-resolution spectra to be used in the application of the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9609203v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9609203v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9609203v1-abstract-full" style="display: none;"> In this work we present spectroscopic observations centered in the spectral lines most widely used as optical indicators of chromospheric activity (H{alpha}, H{beta}, Ca II H & K, and He I D{3}) in a sample of F, G, K and M chromospherically inactive stars. The spectra have been obtained with the aim of providing a library of high and mid-resolution spectra to be used in the application of the spectral subtraction technique to obtain the active-chromosphere contribution to these lines in chromospherically active single and binary stars. This library can also be used for spectral classification purposes. A digital version with all the spectra is available via ftp and the World Wide Web (WWW) in both ASCII and FITS formats <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9609203v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9609203v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 1996; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1996. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, latex file using psfig.sty and A&AS laa-s.sty, 7 PostScript figures. Full postscript (text and figures) and the spectra in both FITS and ASCII formats available at http://www.ucm.es/OTROS/Astrof/fgkmsl/fgkmsl.html Accepted for publication in 'Astronomy and Astrophysics Suppl. Ser.'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9511125">arXiv:astro-ph/9511125</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9511125">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9511125">ps</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> The behaviour of the excess CaII H & K and H_epsilon emissions in chromospherically active binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9511125v1-abstract-short" style="display: inline;"> In this work we analyze the behaviour of the excess Ca~{\sc ii} H \& K and H$蔚$ emissions in a sample of 73 chromospherically active binary systems (RS$~$CVn and BY$~$Dra classes), of different activity levels and luminosity classes. This sample includes the 53 stars analyzed by Fern谩ndez-Figueroa et al. (1994) and the observations of 28 systems described by Montes et al. (1995c). By using the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9511125v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9511125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9511125v1-abstract-full" style="display: none;"> In this work we analyze the behaviour of the excess Ca~{\sc ii} H \& K and H$蔚$ emissions in a sample of 73 chromospherically active binary systems (RS$~$CVn and BY$~$Dra classes), of different activity levels and luminosity classes. This sample includes the 53 stars analyzed by Fern谩ndez-Figueroa et al. (1994) and the observations of 28 systems described by Montes et al. (1995c). By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of spectral type and luminosity class similar to those of the binary star components) we obtain the active-chromosphere contribution to the Ca~{\sc ii} H \& K lines in these 73 systems. We have determined the excess Ca~{\sc ii} H \& K emission equivalent widths and converted them into surface fluxes. The emissions arising from each component were obtained when it was possible to deblend both contributions. We have found that the components of active binaries are generally stronger emitters than single active stars for a given effective temperature and rotation rate. A slight decline of the excess Ca~{\sc ii} H \& K emissions towards longer rotation periods, P$_{\rm rot}$, and larger Rossby numbers, R$_{0}$, is found. When we use R$_{0}$ instead of P$_{\rm rot}$ the scatter is reduced and a saturation at R$_{0}$ $\approx$~0.3 is observed. A good correlation between the excess Ca~{\sc ii}~K and H$蔚$ chromospheric emission fluxes has been found. The correlations obtained between the excess Ca~{\sc ii}~K emission and other activity indicators, (C~{\sc iv} in the transition region, and X-rays in the corona) indicate that the exponents of the power-law relations increase with the formation temperature of the spectral features. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9511125v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9511125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 1995; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 1995. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages in uuencoded compressed postscript file including text, tables, and figures. The paper is also available through http://www.ucm.es/OTROS/Astrof/dpto_preprints.html Request hard copy of preprint to dmg@ucmast.fis.ucm.es. Accepted for publication in 'Astronomy and Astrophysics'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9506025">arXiv:astro-ph/9506025</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9506025">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9506025">ps</a>, <a href="https://arxiv.org/format/astro-ph/9506025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> </div> <p class="title is-5 mathjax"> Application of the spectral subtraction technique to the CaII H & K and H$蔚$ lines in a sample of chromospherically active binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Montes%2C+D">D. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=De+Castro%2C+E">E. De Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez-Figueroa%2C+M+J">M. J. Fernandez-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Cornide%2C+M">M. Cornide</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9506025v1-abstract-short" style="display: inline;"> We present new spectroscopic observations in the Ca~{\sc ii} H \& K line region for a sample of 28 chromospherically active binary systems (RS$~$CVn and BY$~$Dra classes), with different activity levels. By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of similar spectral type and luminosity class) we obtain the active-ch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9506025v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9506025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9506025v1-abstract-full" style="display: none;"> We present new spectroscopic observations in the Ca~{\sc ii} H \& K line region for a sample of 28 chromospherically active binary systems (RS$~$CVn and BY$~$Dra classes), with different activity levels. By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of similar spectral type and luminosity class) we obtain the active-chromosphere contribution to the Ca~{\sc ii} H \& K lines and to the H$蔚$ line when it is present. We have compared the emission equivalent widths obtained with this technique with those obtained by reconstruction of the absorption line profile below the emission peak(s). The emissions arising from each individual star were obtained when it was possible to deblend the contribution of both components. The Ca~{\sc ii} line profiles corresponding to different seasons and orbital phases are analysed in order to determine the contribution of each component and to study the chromospheric activity variations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9506025v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9506025v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 1995; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1995. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages LaTex format, no figures. Postscript file including tex and figures available at http://www.ucm.es/OTROS/Astrof/dpto_preprints.html, request hard copy of preprint to dmg@ucmast.fis.ucm.es. Accepted for publication in 'Astronomy and Astrophysics Supplements'</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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