Y Gem, a symbiotic star outshone by its asymptotic giant branch primary component
I tiakina i:
| I whakaputaina i: | arXiv.org (Dec 18, 2024), p. n/a |
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| Kaituhi matua: | |
| Ētahi atu kaituhi: | , , , |
| I whakaputaina: |
Cornell University Library, arXiv.org
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| Ngā marau: | |
| Urunga tuihono: | Citation/Abstract Full text outside of ProQuest |
| Ngā Tūtohu: |
Kāore He Tūtohu, Me noho koe te mea tuatahi ki te tūtohu i tēnei pūkete!
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| Whakarāpopotonga: | 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. |
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| ISSN: | 2331-8422 |
| Puna: | Engineering Database |