Results 1 to 10 of about 694 (118)
The population of hot subdwarf stars studied with Gaia: I. the catalog of known hot subdwarf stars [PDF]
Astronomy & Astrophysics, 2017 In preparation for the upcoming all-sky data releases of the Gaia mission we compiled a catalogue of known hot subdwarf stars and candidates drawn from the literature and yet unpublished databases. The catalogue contains 5613 unique sources and provides multi-band photometry from the ultraviolet to the far infrared, ground based proper motions ...
S. Geier +7 more
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The Formation of Subdwarf A-type Stars [PDF]
The Astrophysical Journal, 2019 Abstract Subdwarf A-type stars (sdAs) are objects that have hydrogen-rich spectra with surface gravity similar to that of hot subdwarf stars but effective temperature below the zero-age horizontal branch. They are considered to be metal-poor main-sequence (MS) stars or extremely low-mass white dwarfs (ELM WDs).
Jinlong Yu +8 more
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The Formation of Subdwarf B Stars [PDF]
International Astronomical Union Colloquium, 2002 AbstractWe performed full binary evolution calculations and carried out binary population synthesis studies in order to investigate the formation of subdwarf B (sdB) stars via the channels of stable Roche lobe overflow (RLOF), common envelope ejection and helium white dwarf mergers. Our model is successful in the explanation of observational properties
Han, Z +4 more
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Kinematics of nearby subdwarf stars [PDF]
Astronomy & Astrophysics, 2005 We present an analysis of the space motions of 742 subdwarf stars based on the sample of Carney et al. (1994, CLLA). Hipparcos parallaxes, TYC2+HIP proper motions and Tycho2 proper motions were combined with radial velocities and metallicities from CLLA. The kinematical behavior is discussed in particular in relation to their metallicities.
Arifyanto, M. I. +3 more
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Hot subdwarf stars in close-up view [PDF]
Astronomy & Astrophysics, 2013 Context: Hot subdwarf B stars (sdBs) are considered to be core helium-burning stars with very thin hydrogen envelopes situated on or near the extreme horizontal branch (EHB). The formation of sdBs is still unclear as well as the chemical composition of their atmospheres. The observed helium depletion is attributed to atmospheric diffusion.
Geier, S. +7 more
openaire +6 more sources
The EC14026 Stars — Pulsating Hot Subdwarfs [PDF]
Symposium - International Astronomical Union, 1998 The Edinburgh-Cape Blue Object Survey (Stobie et al. 1997a) is a southern hemisphere survey to discover hot, blue stellar objects brighter than B=18 at galactic latitudes more than 30° from the galactic plane. The main categories of object detected are hot subdwarfs, white dwarfs, blue horizontal branch stars, apparently normal B stars, cataclysmic ...
C. Koen +3 more
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The origin of subdwarf B stars
Bulletin de la Société Royale des Sciences de Liège, 2023 The origin of subdwarf B stars (sdBs) is unclear. Different formation channels are proposed including: close-binary evolution, helium-mixing on the red giant branch and the hot flasher scenario. Circumstantial evidence exists that sdBs can result from single star evolution in high metallicity populations.
Ralf Napiwotzki, Callum Aubrey
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New Subdwarf B Star Periods [PDF]
, 2003 4 pages, 2 figures. Uses CRCKAPB.sty. To appear in the Proceedings of the XIII European Workshop on White Dwarfs. NATO Science Series II, Kluwer Academic Publishers.
Morales-Rueda, L. +3 more
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Substellar Companions and the Formation of Hot Subdwarf Stars [PDF]
AIP Conference Proceedings, 2011 6 pages, Part of PlanetsbeyondMS/2010 proceedings, http://arxiv.org/html/1011.6606v1, Report number ...
Geier, Stephan +14 more
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Hot subdwarf B stars with neutron star components [PDF]
Astronomy & Astrophysics, 2020 Context. Subdwarf B stars (sdBs) play a crucial role in stellar evolution, asteroseismology, and far-UV radiation of early-type galaxies, and have been intensively studied with observation and theory. It has theoretically been predicted that sdBs with neutron star (NS) companions exist in the Galaxy, but none have been discovered yet.
You Wu +4 more
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