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Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
- 1.0574936 - ASÚ 2024 RIV GB eng J - Journal Article
Lei, Z. - He, R. - Németh, Péter - Zou, X. - Xiao, H. - Yang, Y. - Zhao, J.
Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST.
Astrophysical Journal. Roč. 953, č. 2 (2023), č. článku 122. ISSN 0004-637X. E-ISSN 1538-4357
R&D Projects: GA ČR(CZ) GA22-34467S
Institutional support: RVO:67985815
Keywords : B subdwarf stars * stellar masses * spectral energy distribution
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 4.9, year: 2022
Method of publishing: Open access
Masses for 664 single-lined hot subdwarf stars identified in LAMOST were calculated by comparing synthetic fluxes from spectral energy distribution with observed fluxes from a Virtual Observatory service. Three groups of hot subdwarf stars were selected from the whole sample according to their parallax precision to study the mass distributions. We found.that He-poor sdB/sdOB stars present a wide mass distribution from 0.1 to 1.0 M-circle dot with a sharp mass peak at around 0.46 M-circle dot, which is consistent with canonical binary model prediction. He-rich sdB/sdOB/sdO stars present a much flatter mass distribution than He-poor sdB/sdOB stars and with a mass peak at around 0.42 M-circle dot. By comparing the observed mass distributions to the predictions of different formation scenarios, we concluded that the binary merger channel, including two helium white dwarfs (He-WDs) and He-WD + mainsequence mergers, cannot be the only main formation channel for He-rich hot subdwarfs, and other formation channels, such as the surviving companions from Type Ia supernovae, could also make impacts on producing this special population, especially for He-rich hot subdwarfs with masses less than 0.44 M-circle dot. He-poor sdO stars also present a flatter mass distribution with an inconspicuous peak mass at 0.18 M-circle dot. The similar mass-Delta RVmax distribution between He-poor sdB/sdOB and sdO stars supports the scenario that He-poor sdO stars could be the subsequent evolution stage of He-poor sdB/sdOB stars.
Permanent Link: https://hdl.handle.net/11104/0345567
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