Cataclysmic Variables: An Empirical Angular Momentum Loss Prescription from Open Cluster Data

Andronov, N.; Pinsonneault, Marc H.; Sills, Alison

doi:10.1086/343030

Cited by 122 publications

(178 citation statements)

References 66 publications

Supporting

Mentioning

165

Contrasting

Order By: Relevance

“…Consequently, in the lifetime of the Galaxy, the vast majority of CVs should have evolved to a period minimum near 80 minutes, and should now have degenerate brown dwarflike secondaries (Howell et al 2001). However, recent models (Andronov et al 2003) suggest (1) much lower angular momentum loss rates, such that it takes 10Y12 Gyr to even reach a 3 hr period, and (2) multiple evolutionary tracks yielding different populations of CVs above and below the 3 hr orbital period.…”

Section: Nova-like Cataclysmic Variablesmentioning

confidence: 99%

Far Ultraviolet Spectroscopic ExplorerSpectroscopy of the Nova‐like Cataclysmic Variable BB Doradus

Godon¹,

Sion²,

Barrett³

et al. 2008

Astrophysical Journal

View full text Add to dashboard Cite

We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE ) spectra of the little-known southern nova-like cataclysmic variable, BB Doradus. The spectrum was obtained as part of our Cycle 8 FUSE survey of highdeclination nova-like stars. The FUSE spectrum of BB Dor, observed in a high state, is modeled with an accretion disk with a very low inclination (possibly lower than 10 ). Assuming an average white dwarf (WD) mass of 0.8 M leads to a mass accretion rate of 10 À9 M yr À1 and a distance on the order of $650 pc, consistent with the extremely low Galactic reddening in the direction of BB Dor. The spectrum presents some broad and deep silicon and sulfur absorption lines, indicating that these elements are overabundant by 3 and 20 times solar, respectively.

show abstract

Section: Nova-like Cataclysmic Variablesmentioning

confidence: 99%

Far Ultraviolet Spectroscopic ExplorerSpectroscopy of the Nova‐like Cataclysmic Variable BB Doradus

Godon¹,

Sion²,

Barrett³

et al. 2008

Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…We use the standard prescription for GR: (Landau & Lifshitz 1951), where G is the gravitational constant, c is the speed of light, a is the orbital separation, M 1 and M 2 are the masses of the two stars, and Q is the orbital angular frequency. Model 2 is GR plus RMB, where the prescription for RMB is given by Andronov et al (2003):…”

Section: Aml Prescriptionsmentioning

confidence: 99%

The Distribution of Secondary Masses in Post-Common-Envelope Binaries: A Potential Test of Disrupted Magnetic Braking

Politano¹,

Weiler²

2006

ApJ

View full text Add to dashboard Cite

The distribution of secondary star masses in present-day post-common-envelope binaries (PCEBs) is calculated using four different models for angular momentum loss (AML) during the post-common-envelope phase: only gravitational radiation (GR), GR plus disrupted magnetic braking (DMB), GR plus reduced MB, and GR plus intermediate MB. For the DMB model, we find that the number of PCEBs decreases abruptly by 38% once MB begins to operate for non-fully convective secondaries. We do not find a similar feature in the distributions calculated using any of the other three AML models in which MB is not disrupted. This percentage decrease in the number of present-day PCEBs predicted using the DMB model is easily large enough that an observed distribution of secondary masses or even spectral types in PCEBs can provide an important test of whether magnetic braking is indeed substantially reduced in secondary stars that are fully convective. We discuss briefly the feasibility of such observations.

show abstract

“…While this may signal a failure of the standard CV evolution theory (e.g. King et al 2002;Barker & Kolb 2003;Andronov et al 2003), it is likely that the known sample of CVs is incomplete and biased. Dwarf novae are predominantly discovered because of their outbursts (Gänsicke 2005), and hence CVs with very long outburst recurrence times or low-amplitude outbursts could be substantially underrepresented in the known CV population.…”

Section: Introductionmentioning

confidence: 99%

Dwarf novae in the Hamburg quasar survey: rarer than expected

Aungwerojwit¹,

Gänsicke²,

Rodríguez‐Gil

et al. 2006

A&A

View full text Add to dashboard Cite

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.

show abstract

Cataclysmic Variables: An Empirical Angular Momentum Loss Prescription from Open Cluster Data

Cited by 122 publications

References 66 publications

Far Ultraviolet Spectroscopic ExplorerSpectroscopy of the Nova‐like Cataclysmic Variable BB Doradus

Far Ultraviolet Spectroscopic ExplorerSpectroscopy of the Nova‐like Cataclysmic Variable BB Doradus

The Distribution of Secondary Masses in Post-Common-Envelope Binaries: A Potential Test of Disrupted Magnetic Braking

Dwarf novae in the Hamburg quasar survey: rarer than expected

Contact Info

Product

Resources

About