Detection of the white dwarf and the secondary star in the new SU UMa dwarf nova HS 2219+1824

Rodríguez‐Gil, P.; Gänsicke, B. T.; Hagen, H. J.; Marsh, T. R.; Harlaftis, E. T.; Kitsionas, S.; Engels, D.

doi:10.1051/0004-6361:20042026

Cited by 19 publications

(18 citation statements)

References 33 publications

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“…The disc parameters found here are very similar to those found in a number of other studies of quiescent accretion discs in CVs (e.g. Williams 1980; Marsh 1987; Lin, Williams & Stover 1988; Rodriguez‐Gil et al 2005). We refrained from more detailed modelling of the optical data as the spectrum was obtained under non‐photometric conditions, and the flux calibration is subject to some uncertainty.…”

Section: Discussionsupporting

confidence: 88%

GD 552: a cataclysmic variable with a brown dwarf companion?

Unda-Sanzana

Marsh

Gänsicke

et al. 2008

Monthly Notices of the Royal Astronomical Society

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GD 552 is a high proper motion star with the strong, double-peaked emission lines characteristic of the dwarf nova class of cataclysmic variable star, and yet no outburst has been detected during the past 12 years of monitoring. We present spectroscopy taken with the aim of detecting emission from the mass donor in this system. We fail to do so at a level which allows us to rule out the presence of a near-main-sequence star donor. Given GD 552's orbital period of 103 minutes, this suggests that it is either a system that has evolved through the ~80-minute orbital period minimum of cataclysmic variable stars and now has a brown dwarf mass donor, or that has formed with a brown dwarf donor in the first place. This model explains the low observed orbital velocity of the white dwarf and GD 552's low luminosity. It is also consistent with the absence of outbursts from the system

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Section: Discussionsupporting

confidence: 88%

GD 552: a cataclysmic variable with a brown dwarf companion?

Unda-Sanzana

Marsh

Gänsicke

et al. 2008

Monthly Notices of the Royal Astronomical Society

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“…(To a lesser extent, this is also true of the Hα line, too.) In other short-period CVs, the WD is responsible for producing comparable features at these wavelengths (Rodríguez-Gil et al 2005), so we attribute the absorption in CSS 120422 to pressure-broadened absorption from the WD's photosphere. These absorption lines suggest that the WD must contribute much of the system's overall optical flux (e.g.…”

Section: Lbt Spectroscopymentioning

confidence: 94%

A New Sub-Period-Minimum Cataclysmic Variable With Partial Hydrogen Depletion and Evidence of Spiral Disk Structure

Garnavich

Applegate

Magno

et al. 2013

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We present time-resolved spectroscopy and photometry of CSS 120422:111127+571239 (= SBS 1108+574), a recently discovered SU UMatype dwarf nova whose 55-minute orbital period is well below the CV period minimum of ∼78 minutes. In contrast with most other known CVs, its spectrum features He I emission of comparable strength to the Balmer lines, implying a hydrogen abundance less than 0.1 of long period CVs-but still at least 10 times higher than than in AM CVn stars. Together, the short orbital period and remarkable helium-to-hydrogen ratio suggest that mass transfer in CSS 120422 began near the end of the donor star's main-sequence lifetime, meaning that the system is probably an AM CVn progenitor as described by Podsiadlowski, Han, & Rappaport (2003). Moreover, a Doppler tomogram of the Hα line reveals two distinct regions of enhanced emission. While one is the result of the stream-disk impact, the other is probably attributable to spiral disk structure generated when material in the outer disk achieves a 2:1 orbital resonance with respect to the donor.

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“…8.1). References: (1) Araujo-Betancor et al (2005a); (2) Jiang et al (2000); (3) Nogami et al (2000); (4) Rodríguez-Gil et al (2005a); (5) this work; (6) Patterson et al (2003); (7) Thorstensen priv. com., & vsnetcampaign-dn 2681; (8) Kato et al (2002); (9) Tappert & Bianchini (2003); (10) Mennickent et al (2002); (11) Gänsicke et al (2000); (12) Fiedler et al (1997); (13) Billington et al (1996); (14) Shafter & Holland (2003).…”

Section: The Orbital Period Distribution Of Dwarf Novae In the Hqsmentioning

confidence: 93%

“…(b) Double-humped orbital light curves are observed in a large number of short-period dwarf novae, e.g. WX Cet (Rogoziecki & Schwarzenberg-Czerny 2001), WZ Sge (Patterson 1998), RZ Leo, BC UMa, MM Hya, AO Oct, HV Vir (Patterson et al 2003), HS 2331+3905 (Araujo-Betancor et al 2005a), and HS 2219+1824 (Rodríguez-Gil et al 2005a); the origin of those double-humps is not really understood, but most likely associated with the accretion disc/bright spot. In longperiod dwarf novae, double-humped light curves are observed in the red part of the spectrum caused by ellipsoidal modulation of the secondary star, e.g.…”

Section: The Orbital Periodmentioning

confidence: 99%

Dwarf novae in the Hamburg quasar survey: rarer than expected

Aungwerojwit¹,

Gänsicke²,

Rodríguez‐Gil

et al. 2006

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Aims. We report the discovery of five new dwarf novae that were spectroscopically identified in the Hamburg Quasar Survey (HQS), and discuss the properties of the sample of new dwarf novae from the HQS. Methods. Follow-up time-resolved spectroscopy and photometry have been obtained to characterise the new systems. Results. The orbital periods determined from analyses of the radial velocity variations and/or orbital photometric variability are P orb 105.1 min or P orb 109.9 min for HS 0417+7445, P orb = 114.3 ± 2.7 min for HS 1016+3412, P orb = 92.66 ± 0.17 min for HS 1340+1524, P orb = 272.317 ± 0.001 min for HS 1857+7127, and P orb = 258.02 ± 0.56 min for HS 2214+2845. HS 1857+7127 is found to be partially eclipsing. In HS 2214+2845 the secondary star of spectral type M3 ± 1 is clearly detected, and we estimate the distance to the system to be d = 390 ± 40 pc. We recorded one superoutburst of HS 0417+7445, identifying the system as a SU UMatype dwarf nova. HS 1016+3412 and HS 1340+1524 have rare outbursts, and their subtype is yet undetermined. HS 1857+7127 frequently varies in brightness and may be a Z Cam-type dwarf nova. HS 2214+2845 is a U Gem-type dwarf nova with a most likely cycle length of 71 d. Conclusions. To date, 14 new dwarf novae have been identified in the HQS. The ratio of short-period (<3 h) to long-period (>3 h) systems of this sample is 1.3, much smaller compared to the ratio of 2.7 found for all known dwarf novae. The HQS dwarf novae display typically infrequent or low-amplitude outburst activity, underlining the strength of spectroscopic selection in identifying new CVs independently of their variability. The spectroscopic properties of short-period CVs in the HQS, newly identified and previously known, suggest that most, or possibly all of them are still evolving towards the minimum period. Their total number agrees with the predictions of population models within an order of magnitude. However, the bulk of all CVs is predicted to have evolved past the minimum period, and those systems remain unidentified. This suggests that those post-bounce systems have markedly weaker Hβ emission lines compared to the average known short-period CVs, and undergo no or extremely rare outbursts.

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Detection of the white dwarf and the secondary star in the new SU UMa dwarf nova HS 2219+1824

Cited by 19 publications

References 33 publications

GD 552: a cataclysmic variable with a brown dwarf companion?

GD 552: a cataclysmic variable with a brown dwarf companion?

A New Sub-Period-Minimum Cataclysmic Variable With Partial Hydrogen Depletion and Evidence of Spiral Disk Structure

Dwarf novae in the Hamburg quasar survey: rarer than expected

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