Y Gem, a symbiotic star outshone by its asymptotic giant branch primary component
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| Udgivet i: | arXiv.org (Dec 18, 2024), p. n/a |
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Cornell University Library, arXiv.org
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| Online adgang: | Citation/Abstract Full text outside of ProQuest |
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| LEADER | 00000nab a2200000uu 4500 | ||
|---|---|---|---|
| 001 | 3131953326 | ||
| 003 | UK-CbPIL | ||
| 022 | |a 2331-8422 | ||
| 035 | |a 3131953326 | ||
| 045 | 0 | |b d20241218 | |
| 100 | 1 | |a Guerrero, M A | |
| 245 | 1 | |a Y Gem, a symbiotic star outshone by its asymptotic giant branch primary component | |
| 260 | |b Cornell University Library, arXiv.org |c Dec 18, 2024 | ||
| 513 | |a Working Paper | ||
| 520 | 3 | |a A considerable number of asymptotic giant branch (AGB) stars exhibit UV excess and/or X-ray emission that indicates a binary companion. AGB stars are so bright that they easily outshine their companions. This almost prevents their identification. Y Gem has been known for some decades to be an AGB star that is bright in the far-UV and X-rays, but it is unclear whether its companion is a main-sequence star or a white dwarf (WD) in a symbiotic system (SySt). Our goal is to uncover the true nature of Y Gem, which will help us to study the possible misidentified population of SySts. Multiwavelength IR, optical, UV, and X-ray observations were analyzed to investigate the properties of the stellar components and the accretion process in Y Gem. In particular, an optical spectrum of Y Gem is presented here for the first time, while X-ray data are interpreted by means of reflection models produced by an accretion disk and material in its vicinity. The optical spectrum exhibits the typical sawtooth-shaped features of molecular absorptions in addition to narrow recombination and forbidden emission lines. The emission lines and the analysis of the extinction-corrected UV spectrum suggest a hot component with \(T_\mathrm{eff}\approx\)60,000 K, \(L\)=140 L\(_{\odot}\), and \(R\)=0.11 R\(_{\odot}\) that very likely is an accreting WD. The late component is found to be an 1.1 M\(_\odot\) AGB star with \(T_\mathrm{eff}\)=3350 K and \(R\)=240 R\(_\odot\). Using IR, optical, UV, and X-ray data, we found that Y Gem is an S-type SySt whose compact component is accreting at an estimated mass-accretion rate of \(\dot{M}_\mathrm{acc}=2.3\times10^{-7}\) M\(_\odot\) yr\(^{-1}\). At this accretion rate, the accreting WD has reached the stable and steady burning phase in which no recurrent events are expected. | |
| 653 | |a Binary stars | ||
| 653 | |a Ultraviolet spectra | ||
| 653 | |a Asymptotic giant branch stars | ||
| 653 | |a Astronomical models | ||
| 653 | |a Accretion disks | ||
| 653 | |a Emission analysis | ||
| 653 | |a X ray reflection | ||
| 653 | |a Main sequence stars | ||
| 653 | |a Asymptotic properties | ||
| 653 | |a Optical data processing | ||
| 653 | |a White dwarf stars | ||
| 653 | |a Companion stars | ||
| 653 | |a Symbiotic stars | ||
| 653 | |a Burning rate | ||
| 653 | |a Optical properties | ||
| 700 | 1 | |a Vasquez-Torres, D A | |
| 700 | 1 | |a Rodríguez-González, J B | |
| 700 | 1 | |a Toalá, J A | |
| 700 | 1 | |a Ortiz, R | |
| 773 | 0 | |t arXiv.org |g (Dec 18, 2024), p. n/a | |
| 786 | 0 | |d ProQuest |t Engineering Database | |
| 856 | 4 | 1 | |3 Citation/Abstract |u https://www.proquest.com/docview/3131953326/abstract/embedded/6A8EOT78XXH2IG52?source=fedsrch |
| 856 | 4 | 0 | |3 Full text outside of ProQuest |u http://arxiv.org/abs/2411.14270 |