Superhump timing in SU Ursae Majoris systems - Implications of the data for the processing disk model

Molnar, Lawrence A.; Kobulnicky, Henry A.

doi:10.1086/171469

Cited by 58 publications

(47 citation statements)

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“…Using the "mean" P SH = 0.08108 d from the entire 2002 superoutburst, we obtain = 4.1%. These fractional superhump excesses are not unusual for an SU UMatype dwarf nova with this P orb (Molnar & Kobulnicky 1992; Patterson 1998), suggesting that V359 Cen should have a normal binary mass ratio q = M 2 /M 1 in spite of its rather unusual outburst characteristics.…”

Section: Superhump Excess and Late Superhumpsmentioning

confidence: 90%

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

Katô

Stubbings²,

Nelson

et al. 2002

A&A

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Abstract. We detected four outbursts of V359 Cen (possible nova discovered in 1939) between 1999 and 2002. Time-resolved CCD photometry during two outbursts (1999 and 2002) revealed that V359 Cen is actually a long-period SU UMa-type dwarf nova with a mean superhump period of 0.08092(1) d. We identified its supercycle length as 307-397 d. This secure identification of the superhump period precludes the previously supposed possibility that V359 Cen could be related to a WZ Sge-type system with a long persistence of late superhumps. The outburst characteristics of V359 Cen are, however, rather unusual in its low occurrence of normal outbursts.

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Section: Superhump Excess and Late Superhumpsmentioning

confidence: 90%

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

Katô

Stubbings²,

Nelson

et al. 2002

A&A

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“…LL And underwent its last known outburst in 1993 December, reaching V \ 13.8 and showing Balmer absorption lines with possible emission cores (Howell & Hurst 1994). Observation of the superhump period (Kato 1993) of 82 minutes combined with the known relationship between superhump and orbital periods (Molnar & Kobulnicky 1992) allowed Howell & Hurst to derive an orbital period of 79 minutes. The faintness of the system resulted in poor S/N spectra from APO, but a good spectrum was obtained with the MMT in 1996 October when LL And was 3 yr into quiescence at V \ 19.9.…”

Section: Wx Cet 2 Months Past Sobmentioning

confidence: 99%

The Effects of Superoutbursts onTOADs

Szkody

Desai

Burdullis

et al. 2000

ApJ

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To explore the amount of secondary irradiation and the long-term e †ects of a superoutburst (SOB) on tremendous outburst amplitude dwarf novae (TOADs), we obtained spectra of EG Cnc for 3È17 months past its SOB, of SW UMa, WX Cet, and USNO 1425.09823278 at 2 months past their SOBs and HV Vir and LL And during their quiescent states at 3 and 5 yr past SOB. The quiescent spectra of EG Cnc, HV Vir, LL And, and USNO 1425 show emission cores surrounded by broad absorption lines from the white dwarf, consistent with very low mass accretion onto low-temperature white dwarfs. SW UMa and WX Cet likely have higher accretion rates and more extensive disks. SW UMa exhibits unusual disk structure, with three zones of emission that persist for 3 days, while EG Cnc and USNO 1425 have a strong orbital modulation of the Balmer lines that may be related to long-lasting irradiation after superoutburst.

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“…Using the well-known empirical correlation between = (P sh − P orb )/P orb and P orb (Molnar & Kobulnicky 1992;Patterson 2001), where P orb and P sh are the orbital and superhump periods respectively, we tried to estimate the value of orbital period. In the vicinity of the period gap, ∼ 0.05.…”

Section: Ccd Light Curve and Data Analysismentioning

confidence: 99%

Discovery and photometric study of the new in-the-gap SU UMa Dwarf Nova Var 73 Dra

Antipin¹,

Павленко²

2002

A&A

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Abstract. We present the discovery and the first investigation of the new dwarf nova Var 73 Dra. We carried out monitoring and time-resolved CCD observations in 2001 August-October and detected several normal outbursts with a recurrence time of about 7-8 days and one slightly brighter superoutburst with a "plateau" phase that lasted 13 days. Our photometry during the superoutburst clearly shows the presence of superhumps with the period 0.0954 (±0.0001) day (although the one-day alias period, 0.1053 d, could not be ruled out). So, the observed features allow us to classify Var 73 Dra as a new SU UMa-type dwarf nova within the well-known gap of orbital period distribution of cataclysmic variables.

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Superhump timing in SU Ursae Majoris systems - Implications of the data for the processing disk model

Cited by 58 publications

References 0 publications

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

The nature of V359 Centauri revealed: New long-period SU UMa-type dwarf nova

The Effects of Superoutbursts onTOADs

Discovery and photometric study of the new in-the-gap SU UMa Dwarf Nova Var 73 Dra

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