A photometric study of the dwarf nova WZ Sagittae in outburst

Patterson, Joseph; McGraw, J. T.; Coleman, L. A.; Africano, J. L.

doi:10.1086/159236

Cited by 87 publications

(118 citation statements)

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“…WZ Sagittae appears to have shown a similar event about 30 days after the superoutburst began, in all three of its recorded eruptions (in 1913, 1946, and 1978; see Fig. 1 of Patterson et al 1981). A similar bump is evident in a well-observed supermaximum of SU UMa, shown in Fig.…”

Section: Bumps In the Eruption Light Curvesupporting

confidence: 52%

Superhumps in cataclysmic variables: I. T. Leonis

Lemm¹,

Patterson²,

Thomas³

et al. 1993

PASP

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ABSTRACT. We report photometry of the dwarf nova T Leonis during its 1993 supermaximum. The principal outburst lasted approximately 20 days, during which large-amplitude superhumps were consistently seen in the light curve. The mean period was 86.7 ±0.1 min, about 2.4% longer than the orbital period determined from radial-velocity measurements. Analysis of data obtained during the 1987 supermaximum implies that the superhump period decreased slowly, with dP/dt= -6x 10" 5 , or dP/ dm =-0.6 min/mag. These are typical values for SU Ursae Majoris-type dwarf novae. At the end of the outburst, the star suddenly brightened again to magnitude 13, from which it declined on a time scale of about 1 day and without superhumps. It is possible that this event was a normal outburst. This suggests that superoutbursts can trigger normal outbursts, and may explain the "bump" frequently found in the light curves of SU UMa stars very late in a superoutburst.

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Section: Bumps In the Eruption Light Curvesupporting

confidence: 52%

Superhumps in cataclysmic variables: I. T. Leonis

Lemm¹,

Patterson²,

Thomas³

et al. 1993

PASP

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“…The latter type of humps with a period of 0.05726(1) d, 1.0% longer than the orbital period, is "superhumps." Although there had been a suggestion of two types of periodic modulation during the 1978 outburst (Bohusz & Udalski 1979), the evidence was not yet compelling because of the remaining ambiguity in identifying the hump maxima and cycle counts, as already discussed by Patterson et al (1981). Our continuous coverage of the entire outburst first unambiguously established the two periods of 0.056656(2) d and 0.05726(1) d for "early superhumps" and "genuine" superhumps, respectively 2 .…”

Section: Observations and Resultsmentioning

confidence: 99%

First detection of the growing humps at the rapidly rising stage of dwarf novae AL Com and WZ Sge

Ishioka

Uemura

Matsumoto

et al. 2002

A&A

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Abstract. We report on time-series photometric observations in the earliest stages of superoutbursts of the extreme dwarf novae, AL Com and WZ Sge, which started on 2001 May after the 6 years quiescence and on 2001 July after the 23 years quiescence, respectively. We detected the growth of "early superhumps" during the each rising stage. Our observations reject the mass transfer instability for the trigger of the superoutburst of WZ Sge stars, and show the existence of some relations between the "early superhumps" and the spiral structure, which gives a hint of the origin of the "early superhumps."

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“…Of course, it is by no means obvious that combining data from different outbursts is warranted! WZ Sagittae could be significantly more stable than the other stars, although this is difficult to assess because of the simultaneous presence of an orbital hump (Patterson et al 1981). The period excess of this super hump [(.P, h -P orb )/ P orb ] is also notably low at 0.8%, nearly three times smaller than any other star.…”

Section: Understanding the Superhump Period Changes 81 A Period-magnmentioning

confidence: 94%

“…Eruptions to about ninth magnitude in 1907, 1962, and 1973 earned it a classification as a recurrent nova, based on an empirical rule of thumb which associated dwarf novae with eruptions of smaller amplitude (<5 mag) and greater frequency (weeks to months). However, the well-observed 1978 outburst of WZ Sagittae-previously classified as a recurrent nova on the same grounds-made it clear that that star, at least, was a certifiable dwarf nova (Gilliland and Kemper 1980;Patterson et al 1981 ), with the outburst arising from the release of accretion energy in a disk around the white dwarf.…”

Section: Introductionmentioning

confidence: 97%

Superhumps in VY Aquarii

Patterson¹,

Bond²,

Grauer³

et al. 1993

PASP

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For many years VY Aquarii has been regarded as a charter member of the class of recurrent novae, because it erupted several times, with outburst amplitudes of -8 mag, exceeding those normally attributed to dwarf novae. We present observations obtained both in quiescence and eruption that emphasize the great similarity of the star to well-credentialed dwarf novae like WZ Sagittae. Long-term visual and photographic coverage shows two types of eruptions, differing in brightness and time scale by a factor of -5. A transient wave in the quiescent light curve suggests a period in the range 80-120 min, which could be the orbital period of the underlying binary. Photometry during a long eruption in 1986 showed a large-amplitude modulation ("superhump") with a period of 92.7 (or possibly 99.1 ) min, which slowly decreased during the eruption. These are normal signatures of SU Ursae Majoris stars, a subclass of dwarf novae. The superhumps observed in SU UMa stars appear to show a similar degree of period instability, such that P~ -(3-10) X 10~5. Perhaps a more physically significant expression of this is a period-magnitude law: the periods decrease by 0.64±0.10% per magnitude of decline, at least during the early decline. This is a plausible decrease to expect from the precessing-disk model for the origin of superhumps, assuming the disk to be largest near maximum light.

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A photometric study of the dwarf nova WZ Sagittae in outburst

Cited by 87 publications

References 0 publications

Superhumps in cataclysmic variables: I. T. Leonis

Superhumps in cataclysmic variables: I. T. Leonis

First detection of the growing humps at the rapidly rising stage of dwarf novae AL Com and WZ Sge

Superhumps in VY Aquarii

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