scholarly journals Analysis of Pulsating White Dwarf Star Light Curves

2019 ◽  
Author(s):  
Denis J. Sullivan
Keyword(s):  
White Dwarf ◽  
Light Curves ◽  
Dwarf Star

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 Interacting Binary White Dwarf Stars

1992 ◽  
Vol 151 ◽  
pp. 461-464
Author(s):  
J.-E. Solheim
Keyword(s):  
White Dwarf ◽  
Structural Changes ◽  
Light Curves ◽  
Physical Parameters ◽  
Dwarf Stars ◽  
White Dwarf Stars ◽  
Test Models ◽  
Radial Pulsations ◽  
Whole Earth

This group of stars consists of 4 systems, also called helium cataclysmics. Three of them show photometric variations and have been studied by the Whole Earth Telescope (WET), which have revealed multiperiodic light curves showing the signature of g-mode non-radial pulsations on the accreting star. The combination of accretion and g-mode pulsations gives a unique opportunity to test models for the accreator's structural changes in response to accretion. IUE-spectra provide additional physical parameters.

scholarly journals Superoutbursts and Superhumps of SU UMa Stars

1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose
Keyword(s):  
Accretion Disk ◽  
Orbital Period ◽  
White Dwarf ◽  
Binary Systems ◽  
Roche Lobe ◽  
Light Curves ◽  
Close Binary ◽  
Dwarf Novae ◽  
Dwarf Nova ◽  
Close Binary Systems

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.

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

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

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 The Spin-Up Rate of the White Dwarf in GK Per

2004 ◽  
Vol 190 ◽  
pp. 120-123
Author(s):  
Christopher W. Mauche
Keyword(s):  
White Dwarf ◽  
Light Curves ◽  
Optical Measurements ◽  
Pulse Period ◽  
X Ray ◽  
Spin Period

AbstractWe use hard X-ray light curves measured by the Chandra HETG and RXTE PCA during the late rise and plateau phases of the 2002 March–April outburst of the intermediate polar GK Per to determine that its X-ray pulse period P = 351.332 ± 0.002 s. Combined with previous X-ray and optical measurements of the spin period of the white dwarf, we find that its spin-up rate Ṗ = 0.00027 ± 0.00005 s yr−1.

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