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</div> <div class="control"> <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/2403.14313">arXiv:2403.14313</a> <span> [<a href="https://arxiv.org/pdf/2403.14313">pdf</a>, <a href="https://arxiv.org/format/2403.14313">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.20240017">10.1002/ASNA.20240017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia23ckh: Symbiotic outburst of the assumed Mira variable V390 Sco </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merc%2C+J">Jaroslav Merc</a>, <a href="/search/astro-ph?searchtype=author&query=Velez%2C+P">Peter Velez</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">St茅phane Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">Olivier Garde</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BB%2C+P+L">Pascal Le D没</a>, <a href="/search/astro-ph?searchtype=author&query=Mulato%2C+L">Lionel Mulato</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+T">Thomas Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</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="2403.14313v1-abstract-short" style="display: inline;"> The poorly studied variable star V390 Sco, previously classified as a Mira pulsator, was detected in a brightening event by the ESA Gaia satellite in September 2023. This work presents an analysis of available archival multifrequency photometric data of this target, along with our spectroscopic observations. Our findings lead to the conclusion that V390 Sco is a new symbiotic star identified by Ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14313v1-abstract-full').style.display = 'inline'; document.getElementById('2403.14313v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14313v1-abstract-full" style="display: none;"> The poorly studied variable star V390 Sco, previously classified as a Mira pulsator, was detected in a brightening event by the ESA Gaia satellite in September 2023. This work presents an analysis of available archival multifrequency photometric data of this target, along with our spectroscopic observations. Our findings lead to the conclusion that V390 Sco is a new symbiotic star identified by Gaia, currently undergoing a classical symbiotic outburst. Additionally, we uncovered three prior outbursts of this system through archival photometry. The outbursts recur approximately every 2330 - 2400 days, and we hypothesize the periastron passage in an eccentric orbit may trigger them, similarly to the case of BX Mon, DD Mic, or MWC 560. A detailed investigation into the nature of the donor star suggested that V390 Sco is an S-type symbiotic star, likely hosting a less evolved, semiregularly pulsating giant donor, but not a Mira variable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14313v1-abstract-full').style.display = 'none'; document.getElementById('2403.14313v1-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> 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </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">9 pages, 9 figures, 1 table; accepted in Astronomische Nachrichten</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.08360">arXiv:2310.08360</a> <span> [<a href="https://arxiv.org/pdf/2310.08360">pdf</a>, <a href="https://arxiv.org/format/2310.08360">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> </div> </div> <p class="title is-5 mathjax"> A planetary collision afterglow and transit of the resultant debris cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M">Matthew Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Lock%2C+S">Simon Lock</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+G">Grant Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=van+Capelleveen%2C+R">Richelle van Capelleveen</a>, <a href="/search/astro-ph?searchtype=author&query=Mamajek%2C+E">Eric Mamajek</a>, <a href="/search/astro-ph?searchtype=author&query=Carone%2C+L">Ludmila Carone</a>, <a href="/search/astro-ph?searchtype=author&query=Hambsch%2C+F">Franz-Josef Hambsch</a>, <a href="/search/astro-ph?searchtype=author&query=Masiero%2C+J">Joseph Masiero</a>, <a href="/search/astro-ph?searchtype=author&query=Mainzer%2C+A">Amy Mainzer</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+J+D">J. Davy Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez%2C+E">Edward Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Leinhardt%2C+Z">Zo毛 Leinhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Dou%2C+J">Jingyao Dou</a>, <a href="/search/astro-ph?searchtype=author&query=Tanna%2C+P">Pavan Tanna</a>, <a href="/search/astro-ph?searchtype=author&query=Sainio%2C+A">Arttu Sainio</a>, <a href="/search/astro-ph?searchtype=author&query=Barker%2C+H">Hamish Barker</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">St茅phane Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">Olivier Garde</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BB%2C+P+L">Pascal Le D没</a>, <a href="/search/astro-ph?searchtype=author&query=Mulato%2C+L">Lionel Mulato</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+T">Thomas Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+R">Michael Rizzo Smith</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="2310.08360v1-abstract-short" style="display: inline;"> Planets grow in rotating disks of dust and gas around forming stars, some of which can subsequently collide in giant impacts after the gas component is removed from the disk. Monitoring programs with the warm Spitzer mission have recorded significant and rapid changes in mid-infrared output for several stars, interpreted as variations in the surface area of warm dusty material ejected by planetary… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08360v1-abstract-full').style.display = 'inline'; document.getElementById('2310.08360v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.08360v1-abstract-full" style="display: none;"> Planets grow in rotating disks of dust and gas around forming stars, some of which can subsequently collide in giant impacts after the gas component is removed from the disk. Monitoring programs with the warm Spitzer mission have recorded significant and rapid changes in mid-infrared output for several stars, interpreted as variations in the surface area of warm dusty material ejected by planetary-scale collisions and heated by the central star: e.g., NGC 2354-ID8, HD 166191 and V844 Persei. Here we report combined observations of the young (about 300 Myr), solar-like star ASASSN-21qj: an infrared brightening consistent with a blackbody temperature of 1000 K and a luminosity of 4 percent of that of the star lasting for about 1000 days, partially overlapping in time with a complex and deep wavelength-dependent optical eclipse that lasted for about 500 days. The optical eclipse started 2.5 years after the infrared brightening, implying an orbital period of at least that duration. These observations are consistent with a collision between two exoplanets of several to tens of Earth masses at 2 to 16 au from the central star. Such an impact produces a hot, highly-extended post-impact remnant with sufficient luminosity to explain the infrared observations. Transit of the impact debris, sheared by orbital motion into a long cloud, causes the subsequent complex eclipse of the host star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08360v1-abstract-full').style.display = 'none'; document.getElementById('2310.08360v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </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">28 pages, 9 figures, 2 tables, author's Accepted Manuscript version, reproducible workflow built with showyourwork; open-source code can be found at https://github.com/mkenworthy/ASASSN-21qj-collision/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023, Nature, 622, 251-254. Published 2023 October 11 at https://www.nature.com/articles/s41586-023-06573-9 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.03537">arXiv:2305.03537</a> <span> [<a href="https://arxiv.org/pdf/2305.03537">pdf</a>, <a href="https://arxiv.org/format/2305.03537">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/10.1093/mnras/stad1434">10.1093/mnras/stad1434 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> V618 Sgr: Galactic eclipsing symbiotic nova detected in repeated outbursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merc%2C+J">J. Merc</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lis%2C+R">R. G谩lis</a>, <a href="/search/astro-ph?searchtype=author&query=Velez%2C+P">P. Velez</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">S. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">O. Garde</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BB%2C+P+L">P. Le D没</a>, <a href="/search/astro-ph?searchtype=author&query=Mulato%2C+L">L. Mulato</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+T">T. Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlsen%2C+T">T. Bohlsen</a>, <a href="/search/astro-ph?searchtype=author&query=Curry%2C+S">S. Curry</a>, <a href="/search/astro-ph?searchtype=author&query=Love%2C+T">T. Love</a>, <a href="/search/astro-ph?searchtype=author&query=Barker%2C+H">H. Barker</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="2305.03537v1-abstract-short" style="display: inline;"> V618 Sgr was previously classified as an R CrB-type variable and later as a possible symbiotic star. Our study aims to analyse the nature of this target, which is currently undergoing significant brightening in properties similar to those of known symbiotic novae. We analyse literature information, photometric observations, and 35 new optical spectra. Our findings strongly suggest that V618 Sgr is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03537v1-abstract-full').style.display = 'inline'; document.getElementById('2305.03537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.03537v1-abstract-full" style="display: none;"> V618 Sgr was previously classified as an R CrB-type variable and later as a possible symbiotic star. Our study aims to analyse the nature of this target, which is currently undergoing significant brightening in properties similar to those of known symbiotic novae. We analyse literature information, photometric observations, and 35 new optical spectra. Our findings strongly suggest that V618 Sgr is an eclipsing symbiotic nova currently in outburst. Additionally, since the star has demonstrated at least two similar brightenings in the past, we propose that V618 Sgr could be the first known galactic symbiotic nova observed in repeated outbursts of this type and may host a relatively massive white dwarf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03537v1-abstract-full').style.display = 'none'; document.getElementById('2305.03537v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </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">6 pages, 6 figures, 1 table; accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.07554">arXiv:2210.07554</a> <span> [<a href="https://arxiv.org/pdf/2210.07554">pdf</a>, <a href="https://arxiv.org/format/2210.07554">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="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/stac3008">10.1093/mnras/stac3008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WHTZ 1: A high excitation Planetary Nebula not a gaseous cocoon from runaway star HD 185806 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Parker%2C+Q+A">Quentin A. Parker</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BB%2C+P+L">Pascal Le D没</a>, <a href="/search/astro-ph?searchtype=author&query=Ritter%2C+A">Andreas Ritter</a>, <a href="/search/astro-ph?searchtype=author&query=Goodhew%2C+P">Peter Goodhew</a>, <a href="/search/astro-ph?searchtype=author&query=Rasool%2C+S">Sakib Rasool</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">Stephane Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">Olivier Garde</a>, <a href="/search/astro-ph?searchtype=author&query=Mulato%2C+L">Lionel Mulato</a>, <a href="/search/astro-ph?searchtype=author&query=Petit%2C+T">Thomas Petit</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="2210.07554v1-abstract-short" style="display: inline;"> We present evidence that the nebular cocoon and bow-shock emission nebula putatively and recently reported as deriving from the 9th magnitude "runaway" star HD 185806 is the previously discovered but obscure planetary nebula WHTZ 1 (Ra 7). It has a Gaia DR3 G~16 blue ionizing star at its geometric centre. We present imagery, spectroscopy, other data and arguments to support that this emission sour… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07554v1-abstract-full').style.display = 'inline'; document.getElementById('2210.07554v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.07554v1-abstract-full" style="display: none;"> We present evidence that the nebular cocoon and bow-shock emission nebula putatively and recently reported as deriving from the 9th magnitude "runaway" star HD 185806 is the previously discovered but obscure planetary nebula WHTZ 1 (Ra 7). It has a Gaia DR3 G~16 blue ionizing star at its geometric centre. We present imagery, spectroscopy, other data and arguments to support that this emission source is a high excitation Planetary Nebula not a stellar wind bow shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07554v1-abstract-full').style.display = 'none'; document.getElementById('2210.07554v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </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">8 pages, 6 figure, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.14629">arXiv:2209.14629</a> <span> [<a href="https://arxiv.org/pdf/2209.14629">pdf</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/10.1016/j.newast.2022.101943">10.1016/j.newast.2022.101943 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> DeGaPe 35: Amateur discovery of a new southern symbiotic star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Petit%2C+T">Thomas Petit</a>, <a href="/search/astro-ph?searchtype=author&query=Merc%2C+J">Jaroslav Merc</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A1lis%2C+R">Rudolf G谩lis</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">St茅phane Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Demange%2C+T">Thierry Demange</a>, <a href="/search/astro-ph?searchtype=author&query=Galli%2C+R">Richard Galli</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">Olivier Garde</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BB%2C+P+L">Pascal Le D没</a>, <a href="/search/astro-ph?searchtype=author&query=Mulato%2C+L">Lionel Mulato</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="2209.14629v1-abstract-short" style="display: inline;"> In this work, we present the discovery and characterization of a new southern S-type symbiotic star, DeGaPe 35. We have obtained the low-resolution spectroscopic observations and supplemented them with photometry from Gaia DR3 and other surveys. The optical spectra of this target show prominent emission lines, including highly ionized [Fe VII] and O VI lines. The cool component of this symbiotic b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.14629v1-abstract-full').style.display = 'inline'; document.getElementById('2209.14629v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.14629v1-abstract-full" style="display: none;"> In this work, we present the discovery and characterization of a new southern S-type symbiotic star, DeGaPe 35. We have obtained the low-resolution spectroscopic observations and supplemented them with photometry from Gaia DR3 and other surveys. The optical spectra of this target show prominent emission lines, including highly ionized [Fe VII] and O VI lines. The cool component of this symbiotic binary is an M4-5 giant with effective temperature ~ 3 380 - 3 470 K and luminosity ~ 3 000 L$_\odot$ (for the adopted distance of 3 kpc). The hot component is a shell-burning white dwarf. The photometric observations of the Gaia satellite, published recently in the Gaia DR3 suggested the variability with the period of about 700 - 800 days that we tentatively attributed to the orbital motion of the binary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.14629v1-abstract-full').style.display = 'none'; document.getElementById('2209.14629v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </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 for publication in New Astronomy; 7 pages, 5 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.11026">arXiv:2109.11026</a> <span> [<a href="https://arxiv.org/pdf/2109.11026">pdf</a>, <a href="https://arxiv.org/ps/2109.11026">ps</a>, <a href="https://arxiv.org/format/2109.11026">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/10.1093/mnras/stab2759">10.1093/mnras/stab2759 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Outbursts and stellar properties of the classical Be star HD 6226 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+N+D">Noel D. Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Thizy%2C+O">Olivier Thizy</a>, <a href="/search/astro-ph?searchtype=author&query=Bjorkman%2C+J+E">Jon E. Bjorkman</a>, <a href="/search/astro-ph?searchtype=author&query=Carciofi%2C+A">Alex Carciofi</a>, <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+A+C">Amanda C. Rubio</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J+D">Joshua D. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Bjorkman%2C+K+S">Karen S. Bjorkman</a>, <a href="/search/astro-ph?searchtype=author&query=Labadie-Bartz%2C+J">Jonathan Labadie-Bartz</a>, <a href="/search/astro-ph?searchtype=author&query=Genaro%2C+M">Matheus Genaro</a>, <a href="/search/astro-ph?searchtype=author&query=Wisniewski%2C+J+P">John P. Wisniewski</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">Luqian Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Gies%2C+D+R">Douglas R. Gies</a>, <a href="/search/astro-ph?searchtype=author&query=Chojnowski%2C+S+D">S. Drew Chojnowski</a>, <a href="/search/astro-ph?searchtype=author&query=Daly%2C+A">Andrea Daly</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+T">Thompson Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Fowler%2C+C">Carlie Fowler</a>, <a href="/search/astro-ph?searchtype=author&query=Gullingsrud%2C+A+D">Allison D. Gullingsrud</a>, <a href="/search/astro-ph?searchtype=author&query=Habel%2C+N">Nolan Habel</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+D+J">David J. James</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+E">Emily Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kuchta%2C+H">Heidi Kuchta</a>, <a href="/search/astro-ph?searchtype=author&query=Lane%2C+A">Alexis Lane</a>, <a href="/search/astro-ph?searchtype=author&query=Miroshnichenko%2C+A">Anatoly Miroshnichenko</a>, <a href="/search/astro-ph?searchtype=author&query=Mishra%2C+A">Ashish Mishra</a>, <a href="/search/astro-ph?searchtype=author&query=Pablo%2C+H">Herbert Pablo</a> , et al. (36 additional authors not shown) </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="2109.11026v1-abstract-short" style="display: inline;"> The bright and understudied classical Be star HD 6226 has exhibited multiple outbursts in the last several years during which the star grew a viscous decretion disk. We analyze 659 optical spectra of the system collected from 2017-2020, along with a UV spectrum from the Hubble Space Telescope and high cadence photometry from both TESS and the KELT survey. We find that the star has a spectral type… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11026v1-abstract-full').style.display = 'inline'; document.getElementById('2109.11026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.11026v1-abstract-full" style="display: none;"> The bright and understudied classical Be star HD 6226 has exhibited multiple outbursts in the last several years during which the star grew a viscous decretion disk. We analyze 659 optical spectra of the system collected from 2017-2020, along with a UV spectrum from the Hubble Space Telescope and high cadence photometry from both TESS and the KELT survey. We find that the star has a spectral type of B2.5IIIe, with a rotation rate of 74% of critical. The star is nearly pole-on with an inclination of $13.4$ degree. We confirm the spectroscopic pulsational properties previously reported, and report on three photometric oscillations from KELT photometry. The outbursting behavior is studied with equivalent width measurements of H$伪$ and H$尾$, and the variations in both of these can be quantitatively explained with two frequencies through a Fourier analysis. One of the frequencies for the emission outbursts is equal to the difference between two photometric oscillations, linking these pulsation modes to the mass ejection mechanism for some outbursts. During the TESS observation time period of 2019 October 7 to 2019 November 2, the star was building a disk. With a large dataset of H$伪$ and H$尾$ spectroscopy, we are able to determine the timescales of dissipation in both of these lines, similar to past work on Be stars that has been done with optical photometry. HD 6226 is an ideal target with which to study the Be disk-evolution given its apparent periodic nature, allowing for targeted observations with other facilities in the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11026v1-abstract-full').style.display = 'none'; document.getElementById('2109.11026v1-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> 22 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </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">48 pages including appendices, accepted to MNRAS. MNRAS online version has a 3D printed dynamical spectrum in the appendix. Contact for this section (due to size limitations)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.13049">arXiv:1911.13049</a> <span> [<a href="https://arxiv.org/pdf/1911.13049">pdf</a>, <a href="https://arxiv.org/format/1911.13049">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> </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/10.1051/0004-6361/201936639">10.1051/0004-6361/201936639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> (704) Interamnia: A transitional object between a dwarf planet and a typical irregular-shaped minor body </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=Vernazza%2C+P">P. Vernazza</a>, <a href="/search/astro-ph?searchtype=author&query=Viikinkoski%2C+M">M. Viikinkoski</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrais%2C+M">M. Ferrais</a>, <a href="/search/astro-ph?searchtype=author&query=Rambaux%2C+N">N. Rambaux</a>, <a href="/search/astro-ph?searchtype=author&query=Podlewska-Gaca%2C+E">E. Podlewska-Gaca</a>, <a href="/search/astro-ph?searchtype=author&query=Drouard%2C+A">A. Drouard</a>, <a href="/search/astro-ph?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/astro-ph?searchtype=author&query=Jehin%2C+E">E. Jehin</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Marsset%2C+M">M. Marsset</a>, <a href="/search/astro-ph?searchtype=author&query=Marchis%2C+F">F. Marchis</a>, <a href="/search/astro-ph?searchtype=author&query=Warner%2C+B">B. Warner</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">R. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Asenjo%2C+V">V. Asenjo</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bronikowska%2C+M">M. Bronikowska</a>, <a href="/search/astro-ph?searchtype=author&query=Brothers%2C+T">T. Brothers</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">S. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Colazo%2C+C">C. Colazo</a>, <a href="/search/astro-ph?searchtype=author&query=Coliac%2C+J">J-F. Coliac</a>, <a href="/search/astro-ph?searchtype=author&query=Duffard%2C+R">R. Duffard</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+A">A. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">A. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Marciniak%2C+A">A. Marciniak</a> , et al. (34 additional authors not shown) </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="1911.13049v2-abstract-short" style="display: inline;"> With an estimated diameter in the 320 to 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with $D$ > 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with $D$ $\lesssim$ 200 km. However, despite its large size, little is known about the shape and spin state of Interamn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.13049v2-abstract-full').style.display = 'inline'; document.getElementById('1911.13049v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.13049v2-abstract-full" style="display: none;"> With an estimated diameter in the 320 to 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with $D$ > 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with $D$ $\lesssim$ 200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller ($D$ $\lesssim$ 200 km) bodies. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling (ADAM) algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Interamnia's volume-equivalent diameter of 332 $\pm$ 6 km implies a bulk density of $蟻$=1.98 $\pm$ 0.68 gcm$^{-3}$ , which suggests that Interamnia - like Ceres and Hygiea - contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2 $蟽$ level. The rather regular shape of Interamnia implies that the size and mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller ($D$ $\lesssim$ 300km) less massive ($m$ $\lesssim$ 3x10$^{19}$ kg) bodies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.13049v2-abstract-full').style.display = 'none'; document.getElementById('1911.13049v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </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 for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 633, A65 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.03637">arXiv:1707.03637</a> <span> [<a href="https://arxiv.org/pdf/1707.03637">pdf</a>, <a href="https://arxiv.org/format/1707.03637">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/10.1016/j.icarus.2017.07.005">10.1016/j.icarus.2017.07.005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Shape models of asteroids based on lightcurve observations with BlueEye600 robotic observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Durech%2C+J">Josef Durech</a>, <a href="/search/astro-ph?searchtype=author&query=Hanus%2C+J">Josef Hanus</a>, <a href="/search/astro-ph?searchtype=author&query=Broz%2C+M">Miroslav Broz</a>, <a href="/search/astro-ph?searchtype=author&query=Lehky%2C+M">Martin Lehky</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">Raoul Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Antonini%2C+P">Pierre Antonini</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">Stephane Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Crippa%2C+R">Roberto Crippa</a>, <a href="/search/astro-ph?searchtype=author&query=Dubreuil%2C+P">Pierre Dubreuil</a>, <a href="/search/astro-ph?searchtype=author&query=Farroni%2C+G">Gino Farroni</a>, <a href="/search/astro-ph?searchtype=author&query=Kober%2C+G">Gilles Kober</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+A">Alain Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Manzini%2C+F">Federico Manzini</a>, <a href="/search/astro-ph?searchtype=author&query=Oey%2C+J">Julian Oey</a>, <a href="/search/astro-ph?searchtype=author&query=Poncy%2C+R">Raymond Poncy</a>, <a href="/search/astro-ph?searchtype=author&query=Rinner%2C+C">Claudine Rinner</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+R">Rene Roy</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="1707.03637v1-abstract-short" style="display: inline;"> We present physical models, i.e. convex shapes, directions of the rotation axis, and sidereal rotation periods, of 18 asteroids out of which 10 are new models and 8 are refined models based on much larger data sets than in previous work. The models were reconstructed by the lightcurve inversion method from archived publicly available lightcurves and our new observations with BlueEye600 robotic obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.03637v1-abstract-full').style.display = 'inline'; document.getElementById('1707.03637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.03637v1-abstract-full" style="display: none;"> We present physical models, i.e. convex shapes, directions of the rotation axis, and sidereal rotation periods, of 18 asteroids out of which 10 are new models and 8 are refined models based on much larger data sets than in previous work. The models were reconstructed by the lightcurve inversion method from archived publicly available lightcurves and our new observations with BlueEye600 robotic observatory. One of the new results is the shape model of asteroid (1663)~van~den~Bos with the rotation period of 749\,hr, which makes it the slowest rotator with known shape. We describe our strategy for target selection that aims at fast production of new models using the enormous potential of already available photometry stored in public databases. We also briefly describe the control software and scheduler of the robotic observatory and we discuss the importance of building a database of asteroid models for studying asteroid physical properties in collisional families. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.03637v1-abstract-full').style.display = 'none'; document.getElementById('1707.03637v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.07422">arXiv:1510.07422</a> <span> [<a href="https://arxiv.org/pdf/1510.07422">pdf</a>, <a href="https://arxiv.org/ps/1510.07422">ps</a>, <a href="https://arxiv.org/format/1510.07422">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> </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/10.1051/0004-6361/201527441">10.1051/0004-6361/201527441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New and updated convex shape models of asteroids based on optical data from a large collaboration network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Eurech%2C+J">J. 膸urech</a>, <a href="/search/astro-ph?searchtype=author&query=Oszkiewicz%2C+D+A">D. A. Oszkiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">R. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Delbo%27%2C+M">M. Delbo'</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+O">O. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Afonina%2C+V">V. Afonina</a>, <a href="/search/astro-ph?searchtype=author&query=Anquetin%2C+R">R. Anquetin</a>, <a href="/search/astro-ph?searchtype=author&query=Antonini%2C+P">P. Antonini</a>, <a href="/search/astro-ph?searchtype=author&query=Arnold%2C+L">L. Arnold</a>, <a href="/search/astro-ph?searchtype=author&query=Audejean%2C+M">M. Audejean</a>, <a href="/search/astro-ph?searchtype=author&query=Aurard%2C+P">P. Aurard</a>, <a href="/search/astro-ph?searchtype=author&query=Bachschmidt%2C+M">M. Bachschmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Badue%2C+B">B. Badue</a>, <a href="/search/astro-ph?searchtype=author&query=Barbotin%2C+E">E. Barbotin</a>, <a href="/search/astro-ph?searchtype=author&query=Barroy%2C+P">P. Barroy</a>, <a href="/search/astro-ph?searchtype=author&query=Baudouin%2C+P">P. Baudouin</a>, <a href="/search/astro-ph?searchtype=author&query=Berard%2C+L">L. Berard</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bernasconi%2C+L">L. Bernasconi</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch%2C+J">J-G. Bosch</a>, <a href="/search/astro-ph?searchtype=author&query=Bouley%2C+S">S. Bouley</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhinova%2C+I">I. Bozhinova</a>, <a href="/search/astro-ph?searchtype=author&query=Brinsfield%2C+J">J. Brinsfield</a> , et al. (144 additional authors not shown) </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="1510.07422v1-abstract-short" style="display: inline;"> Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. This amount already provided a deep insight into physical properties of main-belt asteroids or large collisional families. We aim to increase the number of asteroid shape models and rotation states. Such results are an important input for various further stu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07422v1-abstract-full').style.display = 'inline'; document.getElementById('1510.07422v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.07422v1-abstract-full" style="display: none;"> Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. This amount already provided a deep insight into physical properties of main-belt asteroids or large collisional families. We aim to increase the number of asteroid shape models and rotation states. Such results are an important input for various further studies such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides, in combination with known masses, bulk density estimates, but constrains also theoretical collisional and evolutional models of the Solar System. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as an input for the convex inversion method, and derive 3D shape models of asteroids, together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that one hundred observers who submit their optical data to publicly available databases. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature or their masses will be most likely determined from their gravitational influence on smaller bodies, which orbital deflection will be observed by the ESA Gaia astrometric mission. This was achieved by using additional optical data from recent apparitions for the shape optimization. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and 3 near-Earth asteroids. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07422v1-abstract-full').style.display = 'none'; document.getElementById('1510.07422v1-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> 26 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 586, A108 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.8212">arXiv:1407.8212</a> <span> [<a href="https://arxiv.org/pdf/1407.8212">pdf</a>, <a href="https://arxiv.org/ps/1407.8212">ps</a>, <a href="https://arxiv.org/format/1407.8212">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/10.1051/0004-6361/201424284">10.1051/0004-6361/201424284 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early evolution of the extraordinary Nova Del 2013 (V339 Del) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Skopal%2C+A">A. Skopal</a>, <a href="/search/astro-ph?searchtype=author&query=Drechsel%2C+H">H. Drechsel</a>, <a href="/search/astro-ph?searchtype=author&query=Tarasova%2C+T+N">T. N. Tarasova</a>, <a href="/search/astro-ph?searchtype=author&query=Kato%2C+T">T. Kato</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+M">M. Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Teyssier%2C+F">F. Teyssier</a>, <a href="/search/astro-ph?searchtype=author&query=Garde%2C+O">O. Garde</a>, <a href="/search/astro-ph?searchtype=author&query=Guarro%2C+J">J. Guarro</a>, <a href="/search/astro-ph?searchtype=author&query=Edlin%2C+J">J. Edlin</a>, <a href="/search/astro-ph?searchtype=author&query=Buil%2C+C">C. Buil</a>, <a href="/search/astro-ph?searchtype=author&query=Antao%2C+D">D. Antao</a>, <a href="/search/astro-ph?searchtype=author&query=Terry%2C+J+N">J. N. Terry</a>, <a href="/search/astro-ph?searchtype=author&query=Lemoult%2C+T">T. Lemoult</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">S. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Bohlsen%2C+T">T. Bohlsen</a>, <a href="/search/astro-ph?searchtype=author&query=Favaro%2C+A">A. Favaro</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+K">K. Graham</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="1407.8212v1-abstract-short" style="display: inline;"> We determine the temporal evolution of the luminosity L(WD), radius R(WD) and effective temperature Teff of the white dwarf (WD) pseudophotosphere of V339 Del from its discovery to around day 40. Another main objective was studying the ionization structure of the ejecta. These aims were achieved by modelling the optical/near-IR spectral energy distribution (SED) using low-resolution spectroscopy (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.8212v1-abstract-full').style.display = 'inline'; document.getElementById('1407.8212v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.8212v1-abstract-full" style="display: none;"> We determine the temporal evolution of the luminosity L(WD), radius R(WD) and effective temperature Teff of the white dwarf (WD) pseudophotosphere of V339 Del from its discovery to around day 40. Another main objective was studying the ionization structure of the ejecta. These aims were achieved by modelling the optical/near-IR spectral energy distribution (SED) using low-resolution spectroscopy (3500 - 9200 A), UBVRcIc and JHKLM photometry. During the fireball stage (Aug. 14.8 - 19.9, 2013), Teff was in the range of 6000 - 12000 K, R(WD) was expanding non-uniformly in time from around 66 to around 300 (d/3 kpc) R(Sun), and L(WD) was super-Eddington, but not constant. After the fireball stage, a large emission measure of 1.0-2.0E+62 (d/3 kpc)**2 cm**(-3) constrained the lower limit of L(WD) to be well above the super-Eddington value. The evolution of the H-alpha line and mainly the transient emergence of the Raman-scattered O VI 1032 A line suggested a biconical ionization structure of the ejecta with a disk-like H I region persisting around the WD until its total ionization, around day 40. It is evident that the nova was not evolving according to the current theoretical prediction. The unusual non-spherically symmetric ejecta of nova V339 Del and its extreme physical conditions and evolution during and after the fireball stage represent interesting new challenges for the theoretical modelling of the nova phenomenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.8212v1-abstract-full').style.display = 'none'; document.getElementById('1407.8212v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">14 pages, 9 figures, 3 tables, accepted for Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 569, A112 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1305.1393">arXiv:1305.1393</a> <span> [<a href="https://arxiv.org/pdf/1305.1393">pdf</a>, <a href="https://arxiv.org/ps/1305.1393">ps</a>, <a href="https://arxiv.org/format/1305.1393">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> <p class="title is-5 mathjax"> Spectroscopy of the mysterious Be system FF Cam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garrel%2C+T">T. Garrel</a>, <a href="/search/astro-ph?searchtype=author&query=Miroshnichenko%2C+A+S">A. S. Miroshnichenko</a>, <a href="/search/astro-ph?searchtype=author&query=Danford%2C+S">S. Danford</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">S. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Houpert%2C+F">F. Houpert</a>, <a href="/search/astro-ph?searchtype=author&query=Grankin%2C+K+N">K. N. Grankin</a>, <a href="/search/astro-ph?searchtype=author&query=Kusakin%2C+A+V">A. V. Kusakin</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="1305.1393v1-abstract-short" style="display: inline;"> FF Cam is a variable star near the North celestial pole with hydrogen lines in emission. Its optical variability of ~0.3 mag was discovered by HIPPARCOS. The spectral type assigned to the star in SIMBAD is B9, but its position coincides with a ROSAT X-ray source. This suggests the presence of a high-temperature region in the system that could originate at or near a companion object. We undertook a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.1393v1-abstract-full').style.display = 'inline'; document.getElementById('1305.1393v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1305.1393v1-abstract-full" style="display: none;"> FF Cam is a variable star near the North celestial pole with hydrogen lines in emission. Its optical variability of ~0.3 mag was discovered by HIPPARCOS. The spectral type assigned to the star in SIMBAD is B9, but its position coincides with a ROSAT X-ray source. This suggests the presence of a high-temperature region in the system that could originate at or near a companion object. We undertook a spectroscopic monitoring of FF Cam since the beginning of 2012 and found an extremely variable H-alpha line profile as well as periodically variable radial velocities of numerous absorption lines. The main conclusion from our study is that FF Cam is a binary system with an orbital period of 7.785 days, a B-type primary and a K-type secondary component. We discuss the spectral features, their variations, and the nature of FF Cam. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.1393v1-abstract-full').style.display = 'none'; document.getElementById('1305.1393v1-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> 6 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2013. </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">4 pages, 4 figures, Proceedings of the XI-th Hvar Astrophysical Colloquium "The Most Mysterious Binaries: Significance for 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/1301.6943">arXiv:1301.6943</a> <span> [<a href="https://arxiv.org/pdf/1301.6943">pdf</a>, <a href="https://arxiv.org/ps/1301.6943">ps</a>, <a href="https://arxiv.org/format/1301.6943">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> </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/10.1051/0004-6361/201220701">10.1051/0004-6361/201220701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hanu%C5%A1%2C+J">J. Hanu拧</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Eurech%2C+J">J. 膸urech</a>, <a href="/search/astro-ph?searchtype=author&query=Bro%C5%BE%2C+M">M. Bro啪</a>, <a href="/search/astro-ph?searchtype=author&query=Marciniak%2C+A">A. Marciniak</a>, <a href="/search/astro-ph?searchtype=author&query=Warner%2C+B+D">B. D. Warner</a>, <a href="/search/astro-ph?searchtype=author&query=Pilcher%2C+F">F. Pilcher</a>, <a href="/search/astro-ph?searchtype=author&query=Stephens%2C+R">R. Stephens</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+R">R. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">B. Carry</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Capek%2C+D">D. 膶apek</a>, <a href="/search/astro-ph?searchtype=author&query=Antonini%2C+P">P. Antonini</a>, <a href="/search/astro-ph?searchtype=author&query=Audejean%2C+M">M. Audejean</a>, <a href="/search/astro-ph?searchtype=author&query=Augustesen%2C+K">K. Augustesen</a>, <a href="/search/astro-ph?searchtype=author&query=Barbotin%2C+E">E. Barbotin</a>, <a href="/search/astro-ph?searchtype=author&query=Baudouin%2C+P">P. Baudouin</a>, <a href="/search/astro-ph?searchtype=author&query=Bayol%2C+A">A. Bayol</a>, <a href="/search/astro-ph?searchtype=author&query=Bernasconi%2C+L">L. Bernasconi</a>, <a href="/search/astro-ph?searchtype=author&query=Borczyk%2C+W">W. Borczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch%2C+J+-">J. -G. Bosch</a>, <a href="/search/astro-ph?searchtype=author&query=Brochard%2C+E">E. Brochard</a>, <a href="/search/astro-ph?searchtype=author&query=Brunetto%2C+L">L. Brunetto</a>, <a href="/search/astro-ph?searchtype=author&query=Casulli%2C+S">S. Casulli</a>, <a href="/search/astro-ph?searchtype=author&query=Cazenave%2C+A">A. Cazenave</a>, <a href="/search/astro-ph?searchtype=author&query=Charbonnel%2C+S">S. Charbonnel</a>, <a href="/search/astro-ph?searchtype=author&query=Christophe%2C+B">B. Christophe</a> , et al. (95 additional authors not shown) </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="1301.6943v1-abstract-short" style="display: inline;"> The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.6943v1-abstract-full').style.display = 'inline'; document.getElementById('1301.6943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.6943v1-abstract-full" style="display: none;"> The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.6943v1-abstract-full').style.display = 'none'; document.getElementById('1301.6943v1-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 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </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 for publication in A&A, January 15, 2013</span> </p> </li> </ol> 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