Helium White Dwarf-main Sequence Star Mergerand Formation of Pulsating Hot Subdwarf Stars

2020 ◽  
Vol 44 (3) ◽  
pp. 325-333
Author(s):  
MA Xu-dong ◽  
ZHANG Xian-fei
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star

scholarly journals Evolution Models of Helium White Dwarf–Main-sequence Star Merger Remnants

2017 ◽  
Vol 835 (2) ◽  
pp. 242 ◽  
Author(s):  
Xianfei Zhang ◽  
Philip D. Hall ◽  
C. Simon Jeffery ◽  
Shaolan Bi
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star

scholarly journals White dwarf-main sequence star collisions

1977 ◽  
Vol 179 (4) ◽  
pp. 705-718 ◽  
Author(s):  
M. M. Shara ◽  
G. Shaviv
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star

scholarly journals Origin and Radial Distribution of Faint Blue Horizontal-Branch Stars

1988 ◽  
Vol 126 ◽  
pp. 679-680
Author(s):  
Charles D. Bailyn ◽  
Jonathan E. Grindlay ◽  
Haldan Cohn ◽  
Phyllis M. Lugger
Keyword(s):  
Radial Distribution ◽  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star ◽  
Horizontal Branch ◽  
Horizontal Branch Stars

We report the identification of 23 faint blue horizontal branch stars in Omega Centauri similar to those discussed by Buonanno et al. (1985) in M15. We find that these stars are significantly concentrated towards the center of the cluster with respect to other giants. We suggest that they may have formed from the collision of a main sequence star and a white dwarf.

scholarly journals Detached white dwarf main-sequence star binaries

2004 ◽  
Vol 419 (3) ◽  
pp. 1057-1076 ◽  
Author(s):  
B. Willems ◽  
U. Kolb
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star

scholarly journals Revised Stellar Parameters for V471 Tau, A Post-common Envelope Binary in the Hyades

2021 ◽  
Vol 163 (1) ◽  
pp. 34
Author(s):  
Philip S. Muirhead ◽  
Jason Nordhaus ◽  
Maria R. Drout
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Hubble Space Telescope ◽  
Main Sequence Star ◽  
Velocity Measurements ◽  
Single Star ◽  
Orbital Parameters ◽  
Common Envelope ◽  
Star Evolution ◽  
First Time

Abstract V471 Tau is a post-common-envelope binary consisting of an eclipsing DA white dwarf and a K-type main-sequence star in the Hyades star cluster. We analyzed publicly available photometry and spectroscopy of V471 Tau to revise the stellar and orbital parameters of the system. We used archival K2 photometry, archival Hubble Space Telescope spectroscopy, and published radial-velocity measurements of the K-type star. Employing Gaussian processes to fit for rotational modulation of the system flux by the main-sequence star, we recovered the transits of the white dwarf in front of the main-sequence star for the first time. The transits are shallower than would be expected from purely geometric occultations owing to gravitational microlensing during transit, which places an additional constraint on the white-dwarf mass. Our revised mass and radius for the main-sequence star is consistent with single-star evolutionary models given the age and metallicity of the Hyades. However, as noted previously in the literature, the white dwarf is too massive and too hot to be the result of single-star evolution given the age of the Hyades, and may be the product of a merger scenario. We independently estimate the conditions of the system at the time of common envelope that would result in the measured orbital parameters today.

scholarly journals Nova Models and their Problems

1977 ◽  
Vol 42 ◽  
pp. 301-310
Author(s):  
H.-C. Thomas
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Main Sequence Star ◽  
Late Type ◽  
Hydrogen Bomb ◽  
Binary Model ◽  
Photometric Observations

Very detailed spectroscopic and photometric observations of Novae are available today. Unfortunately they do not directly tell us what suddenly makes a star a million times brighter, sometimes even transforming the familiar constellations on the sky. Twenty-five years after its publication, Mestel’s (1952) metaphor of a gigantic hydrogen bomb seems to be most widely accepted, although he at that time applied his model to a Supernova outburst. Later Giannone and Weigert (1967) as well as Rose (1968), Saslaw (1968) and others have computed hydrostatic models of such an event, using Kraft’s (1963) binary model of a late type main sequence star and a white dwarf. Detailed hydrodynamic computations were carried out by Starrfield and his collaborators (for references see Sparks, Starrfield, and Truran, 1977) and recently by Prialnik, Shara, and Shaviv (A & A 62, 339, 1978).

scholarly journals Population Synthesis Studies of White Dwarf Binaries

2004 ◽  
Vol 194 ◽  
pp. 101-103
Author(s):  
U. Kolb ◽  
B. Willems
Keyword(s):  
White Dwarf ◽  
Main Sequence ◽  
Cataclysmic Variables ◽  
Eclipsing Binaries ◽  
Main Sequence Star ◽  
Population Synthesis

AbstractWe present population synthesis studies of white dwarf - main-sequence star binaries, of cataclysmic variables that are driven by circumbinary discs, and of eclipsing binaries in the exoplanet transit search SuperWASP.

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