Cataclysimc variable candidates from the Palomar Green survey

Green, R. F.; Ferguson, Donald H.; Liebert, James; Schmidt, M.

doi:10.1086/131022

Cited by 91 publications

(63 citation statements)

References 7 publications

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“…7, middle curve) is typical for SW Sex stars: strong single peaked Balmer, Heii and Niii/Ciii emission on top of a flat or slightly blue continuum. However, there are a number of marked differences with previous spectroscopic studies of SW Sex (Green et al, 1982;Penning et al, 1984;Williams, 1989 and DMJ97):…”

Section: Average Spectrummentioning

confidence: 71%

SW Sextantis in an excited, low state

Groot

Rutten

Paradijs

2001

A&A

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Abstract. We present low-resolution spectrophotometric optical observations of the eclipsing nova-like cataclysmic variable SW Sex, the prototype of the SW Sex stars. We observed the system when it was in an unusual low state. The spectrum is characterized by the presence of strong Heii and Civ emission lines as well as the normal single peaked Balmer emission lines. The radial temperature profile of the disk follows the expected T∝R −3/4 only in the outer parts and flattens off inside 0.5 times the white dwarf Roche lobe radius. The single peaked emission lines originate in a region above the plane of the disk, at the position of the hot spot.

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Section: Average Spectrummentioning

confidence: 71%

SW Sextantis in an excited, low state

Groot

Rutten

Paradijs

2001

A&A

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“…It was also detected as a cataclysmic variable in the Palomar-Green Survey, and listed as PG 1140+719 (Green et al 1982). They suggested an identification of this object with a previously-registered variable YY Dra.…”

Section: Introductionmentioning

confidence: 90%

Multiple timescales in cataclysmic binaries

Андронов

Chinarova

Han

et al. 2008

A&A

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Aims. We study the variability of the cataclysmic variable DO Dra, on time-scales of between minutes and decades. (15) d . We analyzed the profile of the "composite" (or "mean") outburst. We discovered however, that a variety of different outburst heights and durations had occurred, contrary to theoretical predictions. The analysis of the historical data has shown a correlation between the decay time dt/dm and the outburst maximum brightness with a slope d(dt/dm)/dm = 0.37(9). With increasing maximum brightness, we find that the decay time also increases; this is in contrast to the model predictions, which indicate that outbursts should have a constant shape. This is interpreted as representing the presence of outburst-to-outburst variability of the magnetospheric radius. A presence of a number of missed weak narrow outbursts is predicted from this statistical relationship. We tabulate characteristics of the "quasi-orbital" variations, which indicate that an amplitude maximum occurs between quiescence and the outburst peak. The semi-amplitude of the spin variability does not exceeded 0.02 mag. A new type of variability is detected, during 3 subsequent nights in 2007: periodic (during one nightly run) oscillations with rapidly-decreasing frequency from 86 to 47 cycles/day and a semi-amplitude increasing from 0. m 06 to 0. m 10, during a monotonic brightness increase from 14. m 27 to 14. m 13. This phenomenon was observed only during an unusually prolonged event of ∼1 mag brightening in 2007 (lasting till autumn), during which no (expected) outburst was detected. We refer to this behaviour as to the "transient periodic oscillations" (TPO). We attribute the frequency decrease to "beat"-type of the variability, probably caused by irradiation of a cloud that is spiralling down to the white dwarf. Its frequency would then increase and coverge towards the spin frequency. To study this new and interesting phenomenon, new regular photometric and spectral (in a "target of opportunity" mode) observations are required.

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“…MM Hya was originally selected as a CV by the Palomer-Green survey (Green et al 1982). The SU UMa-type nature was confirmed by Patterson et al (2003).…”

Section: Hydraementioning

confidence: 95%

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

Katô

Hambsch

Monard

et al. 2016

Publications of the Astronomical Society of Japan

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Continuing the project described by Kato et al. (2009), we collected times of superhump maxima for 128 SU UMa-type dwarf novae observed mainly during the 2015-2016 season and characterized these objects. The data have improved the distribution of orbital periods, the relation between the orbital period and the variation of superhumps, the relation between period variations and the rebrightening type in WZ Sge-type objects. Coupled with new measurements of mass ratios using growing stages of superhumps, we now have a clearer and statistically greatly improved evolutionary path near the terminal stage of evolution of cataclysmic variables. Three objects (V452 Cas, KK Tel, ASASSN-15cl) appear to have slowly growing superhumps, which is proposed to reflect the slow growth of the 3:1 resonance near the stability border. ASASSN-15sl, ASASSN-15ux, SDSS J074859.55+312512.6 and CRTS J200331.3−284941 are newly identified eclipsing SU UMa-type (or WZ Sge-type) dwarf novae. ASASSN-15cy has a short (∼0.050 d) superhump period and appears to belong to EI Psc-type objects with compact secondaries having an evolved core. ASASSN-15gn, ASASSN-15hn, ASASSN-15kh and ASASSN-16bu are candidate period bouncers with superhump periods longer than 0.06 d. We have newly obtained superhump periods for 79 objects and 13 orbital periods, including periods from early superhumps. In order that the future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines how to organize observations of various superoutbursts.

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Cataclysimc variable candidates from the Palomar Green survey

Cited by 91 publications

References 7 publications

SW Sextantis in an excited, low state

SW Sextantis in an excited, low state

Multiple timescales in cataclysmic binaries

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

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