Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00574936" target="_blank" >RIV/67985815:_____/23:00574936 - isvavai.cz</a>
Result on the web
<a href="https://hdl.handle.net/11104/0345567" target="_blank" >https://hdl.handle.net/11104/0345567</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/ace25e" target="_blank" >10.3847/1538-4357/ace25e</a>
Alternative languages
Result language
angličtina
Original language name
Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Original language description
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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
—
OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA22-34467S" target="_blank" >GA22-34467S: Binary interaction on the red giant branch: Hot subdwarfs as a test case.</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
1538-4357
Volume of the periodical
953
Issue of the periodical within the volume
2
Country of publishing house
GB - UNITED KINGDOM
Number of pages
16
Pages from-to
122
UT code for WoS article
001046038300001
EID of the result in the Scopus database
2-s2.0-85167894997