Y Gem: A White Dwarf Symbiotic Star?

Yu, Zhuo-li; Xu, Xiaojie; Shao, Yong; Wang, Q. Daniel; Li, Xiang-Dong

doi:10.3847/1538-4357/ac6ba0

Cited by 4 publications

(3 citation statements)

References 61 publications

(103 reference statements)

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“…keV with a reduced chi-square value of 0.96/39. This temperature is consistent with what would be expected from a 0.8M e accreting nonmagnetic WD (Yu et al 2018) and is way higher than what is expected for accretion onto a mainsequence companion (∼1 keV; see Yu et al 2022).…”

Section: -+supporting

confidence: 87%

“…Assuming the UV emission originated from the WD accretion, and taking the typical luminosity ratio L UV /L X ∼ 10 (Luna et al 2013), we can estimate a typical accretion rate of ∼10 −12 -10 −11 M e yr −1 for a 0.8M e WD. Such low mass accretion rates may occur in wideorbit (P orb > 10 4 days) SySts (e.g., Yu et al 2022), whose existence have been predicted by population synthesis works but were rarely confirmed observationally (Mikołajewska 2012). These SySts would be natural laboratories to investigate the stellar evolution and accretion theories, e.g., the wind mass-loss rate, the disk thermal-viscous instability (Hameury 2020), and the emission mechanism of lowaccretion-rate WDs.…”

Section: Number Of Systs In 500 Pcmentioning

confidence: 99%

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The Missing Symbiotic Stars: A Joint Analysis with Gaia, GALEX, and XMM-Newton Data

Xu,

Shao,

2024

ApJ

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The existence of a population of low-accretion-rate symbiotic stars (SySts), consisting of a giant star and a compact companion (usually a white dwarf), has been proposed recently. However, their population has not been fully understood. In this work, we present an investigation on SySts candidates consisting of asymptotic giant branch stars (AGBs) by cross-correlating the Gaia DR3, the Galaxy Evolution Explorer All-Sky Imaging Survey, and the 4XMM DR13 catalogs. We first build a sample of AGBs within 500 pc based on their locations in the Gaia color–absolute magnitude diagram. We then explore the UV and X-ray properties of the sampled AGBs and compare them to known SySts and candidates. We find 10 SySts candidates based on the far-ultraviolet excess. The typical UV luminosity of the candidates is 1031 erg s−1, which corresponds to a typical accretion rate of 10−12–10−11 M ⊙ yr−1, which is more than 1 order of magnitude lower than known SySts. Based on these findings, the total number of SySts within 500 pc is estimated to be 18. The number of AGBs with X-ray flux above 10−14 erg s−1 cm−2 within 500 pc is estimated to be 37. Our finding implies that a large number of low-accretion-rate SySts are yet to be detected, which provides a base for a complete understanding of their population.

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Section: -+supporting

confidence: 87%

Section: Number Of Systs In 500 Pcmentioning

confidence: 99%

The Missing Symbiotic Stars: A Joint Analysis with Gaia, GALEX, and XMM-Newton Data

Xu,

Shao,

2024

ApJ

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confidence: 99%

2022 Index IEEE Transactions on Magnetics Vol. 58

2022

IEEE Trans. Magn.

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This index covers all technical items-papers, correspondence, reviews, etc.-that appeared in this periodical during 2022, and items from previous years that were commented upon or corrected in 2022. Departments and other items may also be covered if they have been judged to have archival value.The Author Index contains the primary entry for each item, listed under the first author's name. The primary entry includes the coauthors' names, the title of the paper or other item, and its location, specified by the publication abbreviation, year, month, and article number. Article numbers are based on specified topic areas and corresponding codes associated with the publication. The Subject Index contains entries describing the item under all appropriate subject headings, plus the first author's name, the publication abbreviation, month, and year, and associated article number. Note that the item title is found only under the primary entry in the Author Index.

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Reflection physics in X-ray-emitting symbiotic stars

Toalá

2024

Monthly Notices of the Royal Astronomical Society

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X-ray-emitting symbiotic stars exhibit a variety of spectral shapes classified as α, β, γ, δ and β/δ types, which have been attributed to different phenomena such as thermonuclear burning on the surface of the white dwarf (WD) component, shocks between winds and jets with the red giant companion’s extended atmosphere, the presence of heavily extinguished hot plasma from the inner region from an accretion disk and/or a combination of these. However, there is observational evidence that this classification scheme is not definite and, for example, some sources change from one type to another within months or years. In this work, it is proposed that a simple disk-like model can be used to explain the X-ray properties observed from reflection dominated symbiotic stars. For this purpose we use the Stellar Kinematics Including Radiative Transfer (skirt) code, which has been recently upgraded to include radiative transfer from X-ray photons. It is found that thee properties of the accretion disk (geometry and density) in combination with the viewing angle can be invoke to explain the spectral properties of β, δ and β/δ X-ray-emitting symbiotic stars. Spectral variations and type swaps observed for some X-ray-emitting sources can also be explained by variations in the disk properties.

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Y Gem: A White Dwarf Symbiotic Star?

Cited by 4 publications

References 61 publications

The Missing Symbiotic Stars: A Joint Analysis with Gaia, GALEX, and XMM-Newton Data

The Missing Symbiotic Stars: A Joint Analysis with Gaia, GALEX, and XMM-Newton Data

2022 Index IEEE Transactions on Magnetics Vol. 58

Reflection physics in X-ray-emitting symbiotic stars

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