scholarly journals The mass of the white dwarf in the recurrent nova U Scorpii

2001 ◽  
Vol 327 (4) ◽  
pp. 1323-1333 ◽  
Author(s):  
T. D. Thoroughgood ◽  
V. S. Dhillon ◽  
S. P. Littlefair ◽  
T. R. Marsh ◽  
D. A. Smith
Keyword(s):  
White Dwarf ◽  
Recurrent Nova

scholarly journals The 1987 Outburst of the Recurrent Nova U SCO

1988 ◽  
Vol 103 ◽  
pp. 337-338
Author(s):  
K. Sekiguchi ◽  
M.W. Feast ◽  
P.A. Whitelock ◽  
M.D. Overbeek ◽  
W. Wargau ◽  
...  
Keyword(s):  
White Dwarf ◽  
High Velocity ◽  
Accretion Disc ◽  
Low Mass ◽  
Recurrent Nova ◽  
Thermonuclear Runaway

AbstractSpectral observations obtained soon after the 1987 brightening of U Sco support a thermonuclear runaway model for outbursts of this object. Spectra later in the decline are, however, more characteristic of a hot accretion disc. These observations are reconciled in a model where the low-mass high-velocity shell ejected from the surface of the white dwarf collides with the accretion disc causing it to brighten.

scholarly journals Hubble Space Telescope Far-UV Spectroscopy of the Short Orbital Period Recurrent Nova CI Aql: Implications for White Dwarf Mass Evolution

2019 ◽  
Vol 872 (1) ◽  
pp. 68
Author(s):  
Edward M. Sion ◽  
R. E. Wilson ◽  
Patrick Godon ◽  
Sumner Starrfield ◽  
Robert E. Williams ◽  
...  
Keyword(s):  
Orbital Period ◽  
White Dwarf ◽  
Hubble Space Telescope ◽  
Uv Spectroscopy ◽  
Space Telescope ◽  
Recurrent Nova

scholarly journals Supersoft X-ray phases of recurrent novae as an indicator of their white dwarf masses

2020 ◽  
Vol 72 (5) ◽  
Author(s):  
Mariko Kato ◽  
Izumi Hachisu
Keyword(s):  
Light Curve ◽  
White Dwarf ◽  
Total Duration ◽  
Simple Relation ◽  
Light Curves ◽  
Curve Shape ◽  
Plateau Phase ◽  
Hydrogen Burning ◽  
X Ray ◽  
Recurrent Nova

Abstract We have examined the optical/X-ray light curves of seven well-observed recurrent novae, V745 Sco, M31N 2008-12a, LMC N 1968, U Sco, RS Oph, LMC N 2009a, T Pyx, and one recurrent nova candidate LMC N 2012a. Six novae out of the eight show a simple relation that the duration of supersoft X-ray source (SSS) phase is 0.70 times the total duration of the outburst (= X-ray turnoff time), i.e., tSSS = 0.70 toff, the total duration of which ranges from 10 to 260 d. These six recurrent novae show a broad rectangular X-ray light curve shape, the first half-period of which is highly variable in the X-ray count rate. The SSS phase also corresponds to an optical plateau phase that indicates a large accretion disk irradiated by a hydrogen-burning white dwarf (WD). The two other recurrent novae, T Pyx and V745 Sco, show a narrow triangular-shaped X-ray light curve without an optical plateau phase. Their relations between tSSS and toff are rather different from the above six recurrent novae. We also present theoretical SSS durations for recurrent novae with various WD masses and stellar metallicities (Z = 0.004, 0.01, 0.02, and 0.05) and compare them with the observed durations of these recurrent novae. We show that SSS duration is a good indicator of WD mass in recurrent novae with a broad rectangular X-ray light curve shape.

scholarly journals Multi-Frequency Observations of the 1985 Outburst of RS Ophiuchi

1987 ◽  
Vol 93 ◽  
pp. 243-254
Author(s):  
M.A.J. Snijders
Keyword(s):  
White Dwarf ◽  
X Ray ◽  
Bolometric Luminosity ◽  
Recurrent Nova ◽  
Radio Frequencies

AbstractThe 1985 outburst of the bright, recurrent nova RS Oph was almost simultaneously observed at X-ray, UV, optical, IR and radio frequencies at many epochs. The abundances in the ejected shell and the development of the bolometric luminosity as a function of time suggest that the cause of the outburst is a nuclear runaway on a massive white dwarf.

scholarly journals He3 as the Recurrent Nova Trigger Mechanism

1979 ◽  
Vol 53 ◽  
pp. 526-526
Author(s):  
M.M. Shara
Keyword(s):  
White Dwarf ◽  
Trigger Mechanism ◽  
Recurrent Nova ◽  
Red Giant

Observations of recurrent novae (Warner 1976) imply the presence of a red giant (RG) in most, if not all, cases. Giant secondaries in nova systems are otherwise known or suspected only in the peculiar slow novae RR Tel and RT Ser. Bath and Shaviv (1978) showed quantitatively that only a red giant can transfer enough hydrogen-rich mass (~10-5M⊙) to a white dwarf (WD) companion rapidly enough (in ∽30 years) to yield a recurrent nova.

scholarly journals The massive white dwarf in the recurrent nova T CrB

1997 ◽  
Vol 288 (4) ◽  
pp. 1027-1032 ◽  
Author(s):  
T. Shahbaz ◽  
M. Somers ◽  
B. Yudin ◽  
T. Naylor
Keyword(s):  
White Dwarf ◽  
Recurrent Nova

scholarly journals New Photometric Observations of RS Oph

2011 ◽  
Vol 7 (S281) ◽  
pp. 201-202
Author(s):  
Irina Voloshina ◽  
Vladimir Metlov
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Astronomical Institute ◽  
Long Period ◽  
Photometric Observations ◽  
Sternberg Astronomical Institute ◽  
Recurrent Nova ◽  
Type Giant ◽  
Chandrasekhar Limit

AbstractThe recurrent nova RS Oph is a long period (~455 days) binary system consisting of a hot white dwarf with mass close to the Chandrasekhar limit and an M-type giant secondary. Here we present the results of photometric observations of this nova which were made during recent years with the telescopes of the Sternberg Astronomical Institute in Crimea.

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