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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.15768">arXiv:2407.15768</a> <span> [<a href="https://arxiv.org/pdf/2407.15768">pdf</a>, <a href="https://arxiv.org/format/2407.15768">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Early-Time Observations of SN 2023wrk: A Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+J">Jialian Liu</a>, <a href="/search/?searchtype=author&query=Wang%2C+X">Xiaofeng Wang</a>, <a href="/search/?searchtype=author&query=Andrade%2C+C">Cristina Andrade</a>, <a href="/search/?searchtype=author&query=Duverne%2C+P">Pierre-Alexandre Duverne</a>, <a href="/search/?searchtype=author&query=Zhang%2C+J">Jujia Zhang</a>, <a href="/search/?searchtype=author&query=Li%2C+L">Liping Li</a>, <a href="/search/?searchtype=author&query=Wang%2C+Z">Zhenyu Wang</a>, <a href="/search/?searchtype=author&query=Navarete%2C+F">Felipe Navarete</a>, <a href="/search/?searchtype=author&query=Reguitti%2C+A">Andrea Reguitti</a>, <a href="/search/?searchtype=author&query=Schuldt%2C+S">Stefan Schuldt</a>, <a href="/search/?searchtype=author&query=Cai%2C+Y">Yongzhi Cai</a>, <a href="/search/?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/?searchtype=author&query=Yang%2C+Y">Yi Yang</a>, <a href="/search/?searchtype=author&query=Brink%2C+T+G">Thomas G. Brink</a>, <a href="/search/?searchtype=author&query=Zheng%2C+W">WeiKang Zheng</a>, <a href="/search/?searchtype=author&query=Esamdin%2C+A">Ali Esamdin</a>, <a href="/search/?searchtype=author&query=Iskandar%2C+A">Abdusamatjan Iskandar</a>, <a href="/search/?searchtype=author&query=Bai%2C+C">Chunhai Bai</a>, <a href="/search/?searchtype=author&query=Liu%2C+J">Jinzhong Liu</a>, <a href="/search/?searchtype=author&query=Li%2C+X">Xin Li</a>, <a href="/search/?searchtype=author&query=Hu%2C+M">Maokai Hu</a>, <a href="/search/?searchtype=author&query=Li%2C+G">Gaici Li</a>, <a href="/search/?searchtype=author&query=Li%2C+W">Wenxiong Li</a>, <a href="/search/?searchtype=author&query=Ma%2C+X">Xiaoran Ma</a>, <a href="/search/?searchtype=author&query=Yan%2C+S">Shengyu Yan</a> , et al. (22 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="2407.15768v1-abstract-short" style="display: inline;"> We present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days the light curve shows a bump feature, while the B - V color is blue and remains nearly constant. The overall spectral evolution is similar to tha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15768v1-abstract-full').style.display = 'inline'; document.getElementById('2407.15768v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.15768v1-abstract-full" style="display: none;"> We present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days the light curve shows a bump feature, while the B - V color is blue and remains nearly constant. The overall spectral evolution is similar to that of an SN 1991T/SN 1999aa-like SN Ia, while the C II $\lambda6580$ absorption line appears to be unusually strong in the first spectrum taken at $t \approx -$15.4 days after the maximum light. This carbon feature disappears quickly in subsequent evolution but it reappears at around the time of peak brightness. The complex evolution of the carbon line and the possible detection of Ni III absorption around 4700 脜 and 5300 脜 in the earliest spectra indicate macroscopic mixing of fuel and ash. The strong carbon lines is likely related to collision of SN ejecta with unbound carbon, consistent with the predictions of pulsational delayed-detonation or carbon-rich circumstellar-matter interaction models. Among those carbon-rich SNe Ia with strong C II $\lambda6580$ absorption at very early times, the line-strength ratio of C II to Si II and the B-V color evolution are found to exhibit large diversity, which may be attributed to different properties of unbound carbon and outward-mixing $^{56}$Ni. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15768v1-abstract-full').style.display = 'none'; document.getElementById('2407.15768v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted for publication in the Astrophysical Journal (27 pages, 14 figures, 7 tables)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17287">arXiv:2310.17287</a> <span> [<a href="https://arxiv.org/pdf/2310.17287">pdf</a>, <a href="https://arxiv.org/format/2310.17287">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Ready for O4 II: GRANDMA Observations of Swift GRBs during eight-weeks of Spring 2022 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Melo%2C+I+T+e">I. Tosta e Melo</a>, <a href="/search/?searchtype=author&query=Ducoin%2C+J+-">J. -G. Ducoin</a>, <a href="/search/?searchtype=author&query=Vidadi%2C+Z">Z. Vidadi</a>, <a href="/search/?searchtype=author&query=Andrade%2C+C">C. Andrade</a>, <a href="/search/?searchtype=author&query=Rupchandani%2C+V">V. Rupchandani</a>, <a href="/search/?searchtype=author&query=Agayeva%2C+S">S. Agayeva</a>, <a href="/search/?searchtype=author&query=Abdelhadi%2C+J">J. Abdelhadi</a>, <a href="/search/?searchtype=author&query=Abe%2C+L">L. Abe</a>, <a href="/search/?searchtype=author&query=Aguerre-Chariol%2C+O">O. Aguerre-Chariol</a>, <a href="/search/?searchtype=author&query=Aivazyan%2C+V">V. Aivazyan</a>, <a href="/search/?searchtype=author&query=Alishov%2C+S">S. Alishov</a>, <a href="/search/?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/?searchtype=author&query=Bai%2C+J+-">J. -M. Bai</a>, <a href="/search/?searchtype=author&query=Baransky%2C+A">A. Baransky</a>, <a href="/search/?searchtype=author&query=Bednarz%2C+S">S. Bednarz</a>, <a href="/search/?searchtype=author&query=Bendjoya%2C+P">Ph. Bendjoya</a>, <a href="/search/?searchtype=author&query=Benkhaldoun%2C+Z">Z. Benkhaldoun</a>, <a href="/search/?searchtype=author&query=Beradze%2C+S">S. Beradze</a>, <a href="/search/?searchtype=author&query=Bizouard%2C+M+A">M. A. Bizouard</a>, <a href="/search/?searchtype=author&query=Bhardwaj%2C+U">U. Bhardwaj</a>, <a href="/search/?searchtype=author&query=Blazek%2C+M">M. Blazek</a>, <a href="/search/?searchtype=author&query=Bo%C3%ABr%2C+M">M. Bo毛r</a>, <a href="/search/?searchtype=author&query=Broens%2C+E">E. Broens</a>, <a href="/search/?searchtype=author&query=Burkhonov%2C+O">O. Burkhonov</a>, <a href="/search/?searchtype=author&query=Christensen%2C+N">N. Christensen</a> , et al. (84 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="2310.17287v1-abstract-short" style="display: inline;"> We present a campaign designed to train the GRANDMA network and its infrastructure to follow up on transient alerts and detect their early afterglows. In preparation for O4 II campaign, we focused on GRB alerts as they are expected to be an electromagnetic counterpart of gravitational-wave events. Our goal was to improve our response to the alerts and start prompt observations as soon as possible… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17287v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17287v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17287v1-abstract-full" style="display: none;"> We present a campaign designed to train the GRANDMA network and its infrastructure to follow up on transient alerts and detect their early afterglows. In preparation for O4 II campaign, we focused on GRB alerts as they are expected to be an electromagnetic counterpart of gravitational-wave events. Our goal was to improve our response to the alerts and start prompt observations as soon as possible to better prepare the GRANDMA network for the fourth observational run of LIGO-Virgo-Kagra (which started at the end of May 2023), and future missions such as SM. To receive, manage and send out observational plans to our partner telescopes we set up dedicated infrastructure and a rota of follow-up adcates were organized to guarantee round-the-clock assistance to our telescope teams. To ensure a great number of observations, we focused on Swift GRBs whose localization errors were generally smaller than the GRANDMA telescopes' field of view. This allowed us to bypass the transient identification process and focus on the reaction time and efficiency of the network. During 'Ready for O4 II', 11 Swift/INTEGRAL GRB triggers were selected, nine fields had been observed, and three afterglows were detected (GRB 220403B, GRB 220427A, GRB 220514A), with 17 GRANDMA telescopes and 17 amateur astronomers from the citizen science project Kilonova-Catcher. Here we highlight the GRB 220427A analysis where our long-term follow-up of the host galaxy allowed us to obtain a photometric redshift of $z=0.82\pm0.09$, its lightcurve elution, fit the decay slope of the afterglows, and study the properties of the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17287v1-abstract-full').style.display = 'none'; document.getElementById('2310.17287v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.06225">arXiv:2302.06225</a> <span> [<a href="https://arxiv.org/pdf/2302.06225">pdf</a>, <a href="https://arxiv.org/format/2302.06225">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.3847/2041-8213/acc8d0">10.3847/2041-8213/acc8d0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRANDMA and HXMT Observations of GRB 221009A -- the Standard-Luminosity Afterglow of a Hyper-Luminous Gamma-Ray Burst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kann%2C+D+A">D. A. Kann</a>, <a href="/search/?searchtype=author&query=Agayeva%2C+S">S. Agayeva</a>, <a href="/search/?searchtype=author&query=Aivazyan%2C+V">V. Aivazyan</a>, <a href="/search/?searchtype=author&query=Alishov%2C+S">S. Alishov</a>, <a href="/search/?searchtype=author&query=Andrade%2C+C+M">C. M. Andrade</a>, <a href="/search/?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/?searchtype=author&query=Baransky%2C+A">A. Baransky</a>, <a href="/search/?searchtype=author&query=Bendjoya%2C+P">P. Bendjoya</a>, <a href="/search/?searchtype=author&query=Benkhaldoun%2C+Z">Z. Benkhaldoun</a>, <a href="/search/?searchtype=author&query=Beradze%2C+S">S. Beradze</a>, <a href="/search/?searchtype=author&query=Berezin%2C+D">D. Berezin</a>, <a href="/search/?searchtype=author&query=Bo%C3%ABr%2C+M">M. Bo毛r</a>, <a href="/search/?searchtype=author&query=Broens%2C+E">E. Broens</a>, <a href="/search/?searchtype=author&query=Brunier%2C+S">S. Brunier</a>, <a href="/search/?searchtype=author&query=Bulla%2C+M">M. Bulla</a>, <a href="/search/?searchtype=author&query=Burkhonov%2C+O">O. Burkhonov</a>, <a href="/search/?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/?searchtype=author&query=Chen%2C+Y">Y. Chen</a>, <a href="/search/?searchtype=author&query=Chen%2C+Y+P">Y. P. Chen</a>, <a href="/search/?searchtype=author&query=Conti%2C+M">M. Conti</a>, <a href="/search/?searchtype=author&query=Coughlin%2C+M+W">M. W. Coughlin</a>, <a href="/search/?searchtype=author&query=Cui%2C+W+W">W. W. Cui</a>, <a href="/search/?searchtype=author&query=Daigne%2C+F">F. Daigne</a>, <a href="/search/?searchtype=author&query=Delaveau%2C+B">B. Delaveau</a>, <a href="/search/?searchtype=author&query=Devillepoix%2C+H+A+R">H. A. R. Devillepoix</a> , et al. (91 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="2302.06225v2-abstract-short" style="display: inline;"> GRB 221009A is the brightest Gamma-Ray Burst (GRB) detected in more than 50 years of study. In this paper, we present observations in the X-ray and optical domains after the GRB obtained by the GRANDMA Collaboration (which includes observations from more than 30 professional and amateur telescopes) and the Insight-HXMT Collaboration. We study the optical afterglow with empirical fitting from GRAND… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06225v2-abstract-full').style.display = 'inline'; document.getElementById('2302.06225v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.06225v2-abstract-full" style="display: none;"> GRB 221009A is the brightest Gamma-Ray Burst (GRB) detected in more than 50 years of study. In this paper, we present observations in the X-ray and optical domains after the GRB obtained by the GRANDMA Collaboration (which includes observations from more than 30 professional and amateur telescopes) and the Insight-HXMT Collaboration. We study the optical afterglow with empirical fitting from GRANDMA+HXMT data, augmented with data from the literature up to 60 days. We then model numerically, using a Bayesian approach, the GRANDMA and HXMT-LE afterglow observations, that we augment with Swift-XRT and additional optical/NIR observations reported in the literature. We find that the GRB afterglow, extinguished by a large dust column, is most likely behind a combination of a large Milky-Way dust column combined with moderate low-metallicity dust in the host galaxy. Using the GRANDMA+HXMT-LE+XRT dataset, we find that the simplest model, where the observed afterglow is produced by synchrotron radiation at the forward external shock during the deceleration of a top-hat relativistic jet by a uniform medium, fits the multi-wavelength observations only moderately well, with a tension between the observed temporal and spectral evolution. This tension is confirmed when using the extended dataset. We find that the consideration of a jet structure (Gaussian or power-law), the inclusion of synchrotron self-Compton emission, or the presence of an underlying supernova do not improve the predictions, showing that the modelling of GRB22109A will require going beyond the most standard GRB afterglow model. Placed in the global context of GRB optical afterglows, we find the afterglow of GRB 221009A is luminous but not extraordinarily so, highlighting that some aspects of this GRB do not deviate from the global known sample despite its extreme energetics and the peculiar afterglow evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06225v2-abstract-full').style.display = 'none'; document.getElementById('2302.06225v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Accepted to ApJL for the special issue, 37 pages, 23 pages main text, 6 tables, 13 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/2202.09766">arXiv:2202.09766</a> <span> [<a href="https://arxiv.org/pdf/2202.09766">pdf</a>, <a href="https://arxiv.org/format/2202.09766">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/stac2054">10.1093/mnras/stac2054 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRANDMA Observations of ZTF/Fink Transients during Summer 2021 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aivazyan%2C+V">V. Aivazyan</a>, <a href="/search/?searchtype=author&query=Almualla%2C+M">M. Almualla</a>, <a href="/search/?searchtype=author&query=Antier%2C+S">S. Antier</a>, <a href="/search/?searchtype=author&query=Baransky%2C+A">A. Baransky</a>, <a href="/search/?searchtype=author&query=Barynova%2C+K">K. Barynova</a>, <a href="/search/?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/?searchtype=author&query=Bayard%2C+F">F. Bayard</a>, <a href="/search/?searchtype=author&query=Beradze%2C+S">S. Beradze</a>, <a href="/search/?searchtype=author&query=Berezin%2C+D">D. Berezin</a>, <a href="/search/?searchtype=author&query=Blazek%2C+M">M. Blazek</a>, <a href="/search/?searchtype=author&query=Boutigny%2C+D">D. Boutigny</a>, <a href="/search/?searchtype=author&query=Boust%2C+D">D. Boust</a>, <a href="/search/?searchtype=author&query=Broens%2C+E">E. Broens</a>, <a href="/search/?searchtype=author&query=Burkhonov%2C+O">O. Burkhonov</a>, <a href="/search/?searchtype=author&query=Cailleau%2C+A">A. Cailleau</a>, <a href="/search/?searchtype=author&query=Christensen%2C+N">N. Christensen</a>, <a href="/search/?searchtype=author&query=Cejudo%2C+D">D. Cejudo</a>, <a href="/search/?searchtype=author&query=Coleiro%2C+A">A. Coleiro</a>, <a href="/search/?searchtype=author&query=Coughlin%2C+M+W">M. W. Coughlin</a>, <a href="/search/?searchtype=author&query=Datashvili%2C+D">D. Datashvili</a>, <a href="/search/?searchtype=author&query=Dietrich%2C+T">T. Dietrich</a>, <a href="/search/?searchtype=author&query=Dolon%2C+F">F. Dolon</a>, <a href="/search/?searchtype=author&query=Ducoin%2C+J+-">J. -G. Ducoin</a>, <a href="/search/?searchtype=author&query=Duverne%2C+P+-">P. -A. Duverne</a>, <a href="/search/?searchtype=author&query=Marchal-Duval%2C+G">G. Marchal-Duval</a> , et al. (58 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="2202.09766v2-abstract-short" style="display: inline;"> We present our follow-up observations with GRANDMA of transient sources revealed by the Zwicky Transient Facility (ZTF). Over a period of six months, all ZTF triggers were examined in real time by a dedicated science module implemented in the Fink broker, which will be used for the data processing of the Vera C. Rubin Observatory. In this article, we present three selection methods to identify kil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09766v2-abstract-full').style.display = 'inline'; document.getElementById('2202.09766v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09766v2-abstract-full" style="display: none;"> We present our follow-up observations with GRANDMA of transient sources revealed by the Zwicky Transient Facility (ZTF). Over a period of six months, all ZTF triggers were examined in real time by a dedicated science module implemented in the Fink broker, which will be used for the data processing of the Vera C. Rubin Observatory. In this article, we present three selection methods to identify kilonova candidates. Out of more than 35 million candidates, a hundred sources have passed our selection criteria. Six were then followed-up by GRANDMA (by both professional and amateur astronomers). The majority were finally classified either as asteroids or as supernovae events. We mobilized 37 telescopes, bringing together a large sample of images, taken under various conditions and quality. To complement the orphan kilonova candidates (those without associated gamma-ray bursts, which were all), we included three additional supernovae alerts to conduct further observations of during summer 2021. We demonstrate the importance of the amateur astronomer community that contributed images for scientific analyzes of new sources discovered in a magnitude range r'=17-19 mag. We based our rapid kilonova classification on the decay rate of the optical source that should exceed 0.3 mag/day. GRANDMA's follow-up determined the fading rate within 1.5+/-1.2 days post-discovery, without waiting for further observations from ZTF. No confirmed kilonovae were discovered during our observing campaign. This work will be continued in the coming months in the view of preparing for kilonova searches in the next gravitational-wave observing run O4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09766v2-abstract-full').style.display = 'none'; document.getElementById('2202.09766v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">22 pages, 9 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/2012.12152">arXiv:2012.12152</a> <span> [<a href="https://arxiv.org/pdf/2012.12152">pdf</a>, <a href="https://arxiv.org/format/2012.12152">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/staa3968">10.1093/mnras/staa3968 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photometric analysis of three totally eclipsing W UMa stars with increasing periods: TYC 3700-1384-1, V1511 Her and V1179 Her </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Broens%2C+E">Eric Broens</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="2012.12152v1-abstract-short" style="display: inline;"> The first multi-colour light curve models and period studies for the totally eclipsing W UMa stars TYC 3700-1384-1, V1511 Her and V1179 Her are presented. All three stars are A-subtype W UMa stars of spectral type F. The light curve solutions show that TYC 3700-1384-1 has a moderately low mass ratio of q = 0.182 +/- 0.001 and a degree of overcontact of f = 49%. For V1179 Her a mass ratio q = 0.153… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12152v1-abstract-full').style.display = 'inline'; document.getElementById('2012.12152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12152v1-abstract-full" style="display: none;"> The first multi-colour light curve models and period studies for the totally eclipsing W UMa stars TYC 3700-1384-1, V1511 Her and V1179 Her are presented. All three stars are A-subtype W UMa stars of spectral type F. The light curve solutions show that TYC 3700-1384-1 has a moderately low mass ratio of q = 0.182 +/- 0.001 and a degree of overcontact of f = 49%. For V1179 Her a mass ratio q = 0.153 +/- 0.001 and a degree of overcontact of f = 48% is derived. The solution for V1511 Her is inconclusive, however the mass ratio is expected to be between 0.13 < q < 0.15. The evolutionary status is compared with zero-age main sequence stars taking into account energy transfer from the primary to the secondary component. The primary component of TYC 3700-1384-1 fits well in the main-sequence, while V1179 Her is more evolved. The period study reveals for all three stars a continuously increasing period at a rate of dP/dt = 6.1x10-7 d/yr, dP/dt = 5.0x10-7 d/yr and dP/dt = 9.6x10-7 d/yr for TYC 3700-1384-1, V1511 Her and V1179 Her respectively. The estimated mass transfer rates derived from these period changes are 1.6x10-7 solMass/yr for TYC 3700-1384-1 and 1.9x10-7 solMass/yr for V1179 Her. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12152v1-abstract-full').style.display = 'none'; document.getElementById('2012.12152v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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, 15 figures. This is a pre-copyedited, author-produced PDF of an article accepted for publication in MNRAS following peer review</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.5021">arXiv:1301.5021</a> <span> [<a href="https://arxiv.org/pdf/1301.5021">pdf</a>, <a href="https://arxiv.org/ps/1301.5021">ps</a>, <a href="https://arxiv.org/format/1301.5021">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/stt113">10.1093/mnras/stt113 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Light curve analysis and orbital period change of the extreme mass-ratio overcontact binary AW CrB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Broens%2C+E">Eric Broens</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="1301.5021v1-abstract-short" style="display: inline;"> Extreme mass-ratio contact binaries with a high degree of overcontact may be in the late evolutionary stages of the contact phase. Detailed photometric analyses and orbital period studies of those systems can provide invaluable information for the coalescence scenario of close binary systems, as recently observed in V1309 Sco. In this paper the first light curve analysis and period study for the t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.5021v1-abstract-full').style.display = 'inline'; document.getElementById('1301.5021v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.5021v1-abstract-full" style="display: none;"> Extreme mass-ratio contact binaries with a high degree of overcontact may be in the late evolutionary stages of the contact phase. Detailed photometric analyses and orbital period studies of those systems can provide invaluable information for the coalescence scenario of close binary systems, as recently observed in V1309 Sco. In this paper the first light curve analysis and period study for the totally eclipsing contact binary AW CrB is presented. The VRcIc CCD photometric light curves are analysed by means of the WD code. The asymmetry of the light curves is modelled by a cool star spot on the primary component. It is shown that AW CrB has a high degree of overcontact f=75% and an extreme mass-ratio of q=0.10, placing it among the few contact binaries with the lowest known mass-ratios. The mean density of the primary component suggest that it has evolved away from the ZAMS. Eighty-four times of minimum light are reported, derived from observations available in public archives, the literature, and the observations presented in this paper. The orbital period study shows a continuously increasing period, at a rate of dP/dt=3.58x10^-7 d yr^-1, suggesting a mass transfer from the secondary component to the primary one, implying a further decreasing mass-ratio. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.5021v1-abstract-full').style.display = 'none'; document.getElementById('1301.5021v1-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 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 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/0804.0105">arXiv:0804.0105</a> <span> [<a href="https://arxiv.org/pdf/0804.0105">pdf</a>, <a href="https://arxiv.org/ps/0804.0105">ps</a>, <a href="https://arxiv.org/format/0804.0105">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/10.1111/j.1365-2966.2008.13269.x">10.1111/j.1365-2966.2008.13269.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Unique Frequency Spectrum of the Blazhko RRc Star LS Her </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Wils%2C+P">Patrick Wils</a>, <a href="/search/?searchtype=author&query=Kleidis%2C+S">Stelios Kleidis</a>, <a href="/search/?searchtype=author&query=Broens%2C+E">Eric Broens</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="0804.0105v1-abstract-short" style="display: inline;"> The Blazhko effect in RR Lyrae stars is still poorly understood theoretically. Stars with multiple Blazhko periods or in which the Blazhko effect itself varies are particularly challenging. This study investigates the Blazhko effect in the RRc star LS Her. Detailed VRI CCD photometry has been performed on 63 nights during six months. LS Her is confirmed to have a Blazhko period of 12.75+/-0.02 d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.0105v1-abstract-full').style.display = 'inline'; document.getElementById('0804.0105v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0804.0105v1-abstract-full" style="display: none;"> The Blazhko effect in RR Lyrae stars is still poorly understood theoretically. Stars with multiple Blazhko periods or in which the Blazhko effect itself varies are particularly challenging. This study investigates the Blazhko effect in the RRc star LS Her. Detailed VRI CCD photometry has been performed on 63 nights during six months. LS Her is confirmed to have a Blazhko period of 12.75+/-0.02 days. However, where normally the side frequencies of the Blazhko triplet are expected, an equidistant group of three frequencies is found on both sides of the main pulsation frequency. As a consequence the period and amplitude of the Blazhko effect itself vary in a cycle of 109+/-4 days. LS Her is a unique object turning out to be very important in the verification of the theories for the Blazhko effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.0105v1-abstract-full').style.display = 'none'; document.getElementById('0804.0105v1-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> 1 April, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2008. </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 MNRAS</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 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