A measurement of secular evolution in the pre-white dwarf star

1985 ◽  
Vol 292 ◽  
pp. 606 ◽  
Author(s):  
D. E. Winget ◽  
E. L. Robinson ◽  
R. E. Nather ◽  
S. O. Kepler ◽  
D. Odonoghue
Keyword(s):  
White Dwarf ◽  
Dwarf Star ◽  
Secular Evolution

Aspects of the Collapse of Compact Objects

1980 ◽  
Vol 4 (1) ◽  
pp. 49-50
Author(s):  
R. A. Gingold ◽  
J. J. Monaghan
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
White Dwarf ◽  
Compact Objects ◽  
Dwarf Star

Misner Thorne and Wheeler (1973), (page 629) suggested that a freshly formed White Dwarf star of several solar masses would, if slowly — rotating, collapse to form a neutron star pancake which would become unstable and eventually produce several, possibly colliding, neutron stars.

Jupiter-sized planet found orbiting tiny white dwarf star

Physics World ◽  
2021 ◽  
Vol 33 (11) ◽  
pp. 7i-7i
Author(s):  
Hamish Johnston
Keyword(s):  
White Dwarf ◽  
Dwarf Star

scholarly journals Classical Novae in the Context of the Evolution of Cataclysmic Binaries

1990 ◽  
Vol 122 ◽  
pp. 313-324
Author(s):  
Hans Ritter
Keyword(s):  
Mass Transfer ◽  
White Dwarf ◽  
White Dwarfs ◽  
Mass Range ◽  
High Mass ◽  
Transfer Rates ◽  
Classical Novae ◽  
Secular Evolution ◽  
Cataclysmic Binaries ◽  
Nova Outbursts

AbstractIn this paper we explore to what extent the TNR model of nova outbursts and our current concepts of the formation and secular evolution of cataclysmic binaries are compatible. Specifically we address the following questions: 1) whether observational selection can explain the high white dwarf masses attributed to novae, 2) whether novae on white dwarfs in the mass range 0.6M⊙ ≲ M ≲ 0.9M⊙ can occur and how much they could contribute to the observed nova frequency, and 3) whether the high mass transfer rates imposed on the white dwarf in systems above the period gap can be accommodated by the TNR model of nova outbursts.

scholarly journals Rapid Evolution of the Gaseous Exoplanetary Debris around the White Dwarf Star HE 1349–2305

2018 ◽  
Vol 854 (1) ◽  
pp. 40 ◽  
Author(s):  
E. Dennihy ◽  
J. C. Clemens ◽  
B. H. Dunlap ◽  
S. M. Fanale ◽  
J. T. Fuchs ◽  
...  
Keyword(s):  
White Dwarf ◽  
Rapid Evolution ◽  
Dwarf Star

The high-resolution spectrum of the pulsating, pre-white dwarf star PG 1159-035 (GW VIR)

1989 ◽  
Vol 97 ◽  
pp. 1440 ◽  
Author(s):  
James Liebert ◽  
F. Wesemael ◽  
D. Husfeld ◽  
R. Wehrse ◽  
S. G. Starrfield ◽  
...  
Keyword(s):  
High Resolution ◽  
White Dwarf ◽  
High Resolution Spectrum ◽  
Dwarf Star

scholarly journals Type IA Supernovae

1992 ◽  
Vol 151 ◽  
pp. 225-234
Author(s):  
J. Craig Wheeler
Keyword(s):  
White Dwarf ◽  
Cataclysmic Variables ◽  
Type Ia Supernovae ◽  
Low Velocity ◽  
Severe Problem ◽  
Transfer Rates ◽  
Secular Evolution ◽  
Thermonuclear Explosion ◽  
Type Ia ◽  
Ia Supernovae

Spectral calculations show that a model based on the thermonuclear explosion of a degenerate carbon/oxygen white dwarf provides excellent agreement with observations of Type Ia supernovae. Identification of suitable evolutionary progenitors remains a severe problem. General problems with estimation of supernova rates are outlined and the origin of Type Ia supernovae from double degenerate systems are discussed in the context of new rates of explosion per H band luminosity, the lack of observed candidates, and the likely presence of H in the vicinity of some SN Ia events. Re-examination of the problems of triggering Type Ia by accretion of hydrogen from a companion shows that there may be an avenue involving cataclysmic variables, especially if extreme hibernation occurs. Novae may channel accreting white dwarfs to a unique locus in accretion rate/mass space. Systems that undergo secular evolution to higher mass transfer rates could lead to just the conditions necessary for a Type Ia explosion. Tests involving fluorescence or absorption in a surrounding circumstellar medium and the detection of hydrogen stripped from a companion, which should appear at low velocity inside the white dwarf ejecta, are suggested. Possible observational confirmation of the former is described.

The Dwarf Nova EX Hydrae

1974 ◽  
Vol 2 (5) ◽  
pp. 271-274 ◽  
Author(s):  
R. D. Watson ◽  
P. T. Rayner
Keyword(s):  
Binary System ◽  
Time Resolution ◽  
White Dwarf ◽  
Roche Lobe ◽  
Dwarf Star ◽  
Dwarf Nova ◽  
Photoelectric Time

The object EX Hya is a dwarf nova with a binary period of 98.3 min (Mumford 1964, 1967). Warner (1972, 1973a) has observed two complete cycles of this star with a photoelectric time resolution of 5 sec. These observations suggested that EX Hya can be understood in terms of the model proposed by Warner and Nather (1971) in their discussion of U Gem. In this model, a white dwarf primary of a semi-detached binary system is surrounded by a disk of gas formed from matter transfered from the secondary, which is a cool dwarf star filling its Roche lobe.

scholarly journals The High Resolution Spectrum of the Pulsating, Pre-White Dwarf Star PG 1159-035 (GW VIR)

1989 ◽  
Vol 114 ◽  
pp. 384-387
Author(s):  
James Liebert ◽  
F. Wesemael ◽  
D. Husfeld ◽  
R. Wehrse ◽  
S. G. Starrfield ◽  
...  
Keyword(s):  
High Resolution ◽  
Effective Temperature ◽  
White Dwarf ◽  
White Dwarfs ◽  
High Resolution Spectrum ◽  
Dwarf Star ◽  
Dwarf Stars ◽  
New Class ◽  
White Dwarf Stars ◽  
Nonradial Pulsation

First reported at the IAU Colloquium No. 53 on White Dwarfs (McGraw et al. 1979), PG 1159-035 (GW Vir) is the prototype of a new class of very hot, pulsating, pre-white dwarf stars. It shows complicated, nonradial pulsation modes which have been studied exhaustively, both observationally and theoretically. The effective temperature has been crudely estimated as 100,000 K with log g ~ 7 (Wesemael, Green and Liebert 1985, hereafter WGL).

scholarly journals A planetesimal orbiting within the debris disc around a white dwarf star

Science ◽  
2019 ◽  
Vol 364 (6435) ◽  
pp. 66-69 ◽  
Author(s):  
Christopher J. Manser ◽  
Boris T. Gänsicke ◽  
Siegfried Eggl ◽  
Mark Hollands ◽  
Paula Izquierdo ◽  
...  
Keyword(s):  
Emission Line ◽  
Solid Body ◽  
White Dwarf ◽  
Periodic Variation ◽  
Emission Lines ◽  
Line Profiles ◽  
Dwarf Star ◽  
Dwarf Stars ◽  
White Dwarf Stars ◽  
Short Period

Many white dwarf stars show signs of having accreted smaller bodies, implying that they may host planetary systems. A small number of these systems contain gaseous debris discs, visible through emission lines. We report a stable 123.4-minute periodic variation in the strength and shape of the Ca ii emission line profiles originating from the debris disc around the white dwarf SDSS J122859.93+104032.9. We interpret this short-period signal as the signature of a solid-body planetesimal held together by its internal strength.

scholarly journals The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

Nature ◽  
2006 ◽  
Vol 443 (7109) ◽  
pp. 308-311 ◽  
Author(s):  
D. Andrew Howell ◽  
Mark Sullivan ◽  
Peter E. Nugent ◽  
Richard S. Ellis ◽  
Alexander J. Conley ◽  
...  
Keyword(s):  
White Dwarf ◽  
Dwarf Star ◽  
Type Ia Supernova ◽  
Type Ia
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