HS 2237+8154: On the onset of mass  transfer or entering the
period gap?

Gänsicke, B. T.; Araujo-Betancor, S.; Hagen, H. J.; Harlaftis, E. T.; Kitsionas, S.; Dreizler, S.; Engels, D.

doi:10.1051/0004-6361:20035591

Cited by 47 publications

(51 citation statements)

References 22 publications

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“…The systems with data that allow an examination of the Hα emission line profile are presented in Table 2. Apart from the six PCEBs with multiple emission components from the present survey and the known objects LTT 560 and QS Vir, we find one other such system (HS 2237+8154; Gänsicke et al 2004). While it is not explicitly mentioned by the authors, the trailed spectrum of the Hα emission line (their Fig.…”

Section: Discussionmentioning

confidence: 57%

Multiple emission line components in detached post-common-envelope binaries

Tappert

Gänsicke

Rebassa‐Mansergas

et al. 2011

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Motivated by the recent discovery of an Hα emission line component originating close to the white dwarf primary in the post-commonenvelope binary (PCEB) LTT 560, we have undertaken a spectroscopic snapshot survey on 11 short-period (P orb < 6 h) PCEBs using FORS2. We have found multi-component Hα emission line profiles in six of our targets, indicating that multiple Hα emission sites are rather common in short-period PCEBs. The underlying physical mechanisms, however, can be fundamentally different. In our sample we find one system where the extracted radial velocities of two identified components indicate that both originate in the late-type secondary star, where one is caused by irradiation from the hot white dwarf primary and the other by stellar activity. Another object presents two components that are located on opposite sides of the centre-of-mass, suggesting a case similar to LTT 560, i.e. that accretion of stellar wind from the secondary star produces Hα emission on, or close to, the white dwarf.

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Section: Discussionmentioning

confidence: 57%

Multiple emission line components in detached post-common-envelope binaries

Tappert

Gänsicke

Rebassa‐Mansergas

et al. 2011

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“…The details of the observations and instruments used are given in Table 2. The data obtained at Wendelstein, Calar Alto, Kryoneri, INT, and OLT were reduced using the pipeline described by Gänsicke et al (2004a), which uses the Sextractor (Bertin & Arnouts 1996) to calculate aperture photometry for all objects in the field of view. The AIP data were reduced entirely within MIDAS.…”

Section: Photometrymentioning

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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“…The 2008 December observations obtained with the NOT were reduced with the pipeline described by Southworth et al (2009a,b), which uses an idl implementation of daophot to perform aperture photometry. The remaining photometric data were reduced using the pipeline described by Gänsicke et al (2004), which performs bias and flat-field corrections within midas 3 and aperture photometry with the SExtractor package (Bertin & Arnouts 1996). Instrumental differential magnitudes were converted into V-band apparent magnitudes, using the SDSS ugriz apparent magnitudes of several comparison stars and the transformation equations given by Lupton 4 .…”

Section: Photometrymentioning

confidence: 99%

Orbital periods of cataclysmic variables identified by the SDSS

Southworth¹,

Hickman²,

Marsh³

et al. 2009

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We present time-resolved spectroscopy and photometry of SDSS J100658.40+233724.4, which we have discovered to be an eclipsing cataclysmic variable with an orbital period of 0.18591324 days (267.71507 min). The observed velocity amplitude of the secondary star is 276 ± 7 km s −1 , which an irradiation correction reduces to 258 ± 12 km s −1 . Doppler tomography of emission lines from the infrared calcium triplet supports this measurement. We have modelled the light curve using the lcurve code and Markov Chain Monte Carlo simulations, finding a mass ratio of 0.51 ± 0.08. From the velocity amplitude and the light curve analysis we find the mass of the white dwarf to be 0.78 ± 0.12 M and the masses and radii of the secondary star to be 0.40 ± 0.10 M and 0.466 ± 0.036 R , respectively. The secondary component is less dense than a normal main sequence star but its properties are in good agreement with the expected values for a CV of this orbital period. By modelling the spectral energy distribution of the system we find a distance of 676 ± 40 pc and estimate a white dwarf effective temperature of 16 500 ± 2000 K.

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HS 2237+8154: On the onset of mass transfer or entering the period gap?

Cited by 47 publications

References 22 publications

Multiple emission line components in detached post-common-envelope binaries

Multiple emission line components in detached post-common-envelope binaries

Dwarf novae in the Hamburg quasar survey: rarer than expected

Orbital periods of cataclysmic variables identified by the SDSS

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