1995
DOI: 10.1086/176496
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The 71 Second Oscillation in the Light Curve of the Old Nova DQ Herculis

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Cited by 44 publications
(65 citation statements)
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“…Using the masses of both components (M 1 = 0.6(±0.07) M and M 2 = 0.4(±0.05) M ) derived by Horne et al (1993), a lower limit of the mass transfer rate,Ṁ 2 = −7.2(±3.2) × 10 −9 M yr −1 is obtained, which is the same order of magnitude as that derived by Zhang et al (1995), and should be considered as a lower limit. Thus, if there are extra mechanisms of mass and angular momentum loss in DQ Herculis, then a considerable mass transfer rate from the red dwarf to the white dwarf is needed to produce the observed orbital period increase.…”
Section: Secular Orbital Period Increasesupporting
confidence: 63%
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“…Using the masses of both components (M 1 = 0.6(±0.07) M and M 2 = 0.4(±0.05) M ) derived by Horne et al (1993), a lower limit of the mass transfer rate,Ṁ 2 = −7.2(±3.2) × 10 −9 M yr −1 is obtained, which is the same order of magnitude as that derived by Zhang et al (1995), and should be considered as a lower limit. Thus, if there are extra mechanisms of mass and angular momentum loss in DQ Herculis, then a considerable mass transfer rate from the red dwarf to the white dwarf is needed to produce the observed orbital period increase.…”
Section: Secular Orbital Period Increasesupporting
confidence: 63%
“…In this case, the average value should be reliable and may be applied. In addition, Zhang et al (1995) and Wood et al (2005) reported their 44 eclipse times in Heliocentric Julian Ephemeris Dates (HJED), which correspond to ephemeris time (ET). Thus, we converted them to Heliocentric Julian Dates (HJD), which correspond to coordinated Universal time (UTC).…”
Section: Observation Of Times Of Light Minimummentioning
confidence: 99%
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“…They all lie in the region of the diagram defined by P spin /P orb < 0.01, but with a large range of orbital periods. They include the very long outburst interval SU UMa star, WZ Sge (Patterson et al 1998) with a proposed spin period of 28 s, the propeller system AE Aqr (Choi, Dotani & Agrawal 1999) with a 33 s spin period, the 'DQ Her systems' V533 Her (Thorstensen & Taylor 2000) and DQ Her (Zhang et al 1995), and also XY Ari (Hellier, Mukai & Beardmore 1997) and the long orbital period old nova GK Per (Morales-Rueda, Still & Roche 1996).…”
Section: Rapid Rotatorsmentioning
confidence: 99%
“…This edge-on (i % 89 ; Petterson 1980) system displays a sinusoidal 71 s photometric periodicity with an amplitude near 1% and is the prototype for the DQ Her class, reviewed most recently by Patterson (1994;see also Warner 1995, pp. 412-440;Zhang et al 1995). The magnetic white dwarf primary of DQ Her is hidden from view by the edge-on accretion disk, but we receive pulsed, reprocessed radiation from the disk as the sweeping beam of soft X-rays emitted from the accretion columns at the magnetic poles of the white dwarf as the star rotates once every 71 s. Variations in the phase of the 71 s signal outside eclipse result from self-eclipses of the disk and from variations in the opening angle of the disk as a function of azimuthal angle about the white dwarf primary (e.g., Chester 1979;O'Donoghue 1985).…”
Section: Introductionmentioning
confidence: 99%