How much electric surcharge fits on … a “white 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.

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Jupiter-sized planet found orbiting tiny white dwarf star

Physics World ◽

10.1088/2058-7058/33/11/08 ◽

2021 ◽

Vol 33 (11) ◽

pp. 7i-7i

Author(s):

Hamish Johnston

Keyword(s):

White Dwarf ◽

Dwarf Star

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

The Astrophysical Journal ◽

10.3847/1538-4357/aaa89b ◽

2018 ◽

Vol 854 (1) ◽

pp. 40 ◽

Cited By ~ 26

Author(s):

E. Dennihy ◽

J. C. Clemens ◽

B. H. Dunlap ◽

S. M. Fanale ◽

J. T. Fuchs ◽

...

Keyword(s):

White Dwarf ◽

Rapid Evolution ◽

Dwarf Star

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

The Astronomical Journal ◽

10.1086/115084 ◽

1989 ◽

Vol 97 ◽

pp. 1440 ◽

Cited By ~ 9

Author(s):

James Liebert ◽

F. Wesemael ◽

D. Husfeld ◽

R. Wehrse ◽

S. G. Starrfield ◽

...

Keyword(s):

High Resolution ◽

White Dwarf ◽

High Resolution Spectrum ◽

Dwarf Star

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

The Astrophysical Journal ◽

10.1086/163193 ◽

1985 ◽

Vol 292 ◽

pp. 606 ◽

Cited By ~ 80

Author(s):

D. E. Winget ◽

E. L. Robinson ◽

R. E. Nather ◽

S. O. Kepler ◽

D. Odonoghue

Keyword(s):

White Dwarf ◽

Dwarf Star ◽

Secular Evolution

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The Dwarf Nova EX Hydrae

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000013862 ◽

1974 ◽

Vol 2 (5) ◽

pp. 271-274 ◽

Cited By ~ 1

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.

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

International Astronomical Union Colloquium ◽

10.1017/s0252921100099929 ◽

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).

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

Science ◽

10.1126/science.aat5330 ◽

2019 ◽

Vol 364 (6435) ◽

pp. 66-69 ◽

Cited By ~ 53

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.

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