The quest for companions to post-common envelope binaries

Beuermann, K.; Dreizler, S.; Hessman, F. V.; Deller, Jakob

doi:10.1051/0004-6361/201219391

Cited by 80 publications

(99 citation statements)

References 39 publications

(63 reference statements)

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“…(1) Beuermann et al (2012b); (2) that the present-day population of PCEBs is simulated with a low value of the CE efficiency, including a fraction of the recombination energy, based on the results of Zorotovic et al (2010). A full parameter study will be presented elsewhere.…”

Section: Binary Population Simulationmentioning

confidence: 99%

Origin of apparent period variations in eclipsing post-common-envelope binaries

Zorotovic

Schreiber

2013

A&A

118

159

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Context. Apparent period variations detected in several eclipsing, close-compact binaries are frequently interpreted as being caused by circumbinary giant planets. This interpretation raises the question of the origin of the potential planets that must have either formed in the primordial circumbinary disk, together with the host binary star, and survived its evolution into a close-compact binary or formed in a post-common-envelope circumbinary disk that remained bound to the post-common-envelope binary (PCEB). Aims. Here we combine current knowledge of planet formation and the statistics of giant planets around primordial and evolved binary stars with the theory of close-compact binary star evolution aiming to derive new constraints on possible formation scenarios. Methods. We compiled a comprehensive list of observed eclipsing PCEBs, estimated the fraction of systems showing apparent period variations, reconstructed the evolutionary history of the PCEBs, and performed binary population models of PCEBs to characterize their main sequence binary progenitors. We reviewed the currently available constraints on the fraction of PCEB progenitors that host circumbinary giant planets. Results. We find that the progenitors of PCEBs are very unlikely to be frequent hosts of giant planets ( < ∼ 10 per cent), while the frequency of PCEBs with observed apparent period variations is very high (∼90 per cent). Conclusions. The variations in eclipse timings measured in eclipsing PCEBs are probably not caused by first-generation planets that survived common-envelope evolution. The remaining options for explaining the observed period variations are second-generation planet formation or perhaps variations in the shape of a magnetically active secondary star. We suggest observational tests for both options.

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Section: Binary Population Simulationmentioning

confidence: 99%

Origin of apparent period variations in eclipsing post-common-envelope binaries

Zorotovic

Schreiber

2013

A&A

118

159

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“…Following Beuermann et al (2012b), we include their eclipse timings in Fig. 4 along with others having a quoted error ≤0.0001 d (Wood et al 1993;Lee et al 2009;Brát et al 2011 's fit, curving upwards rather than following the proposed quadratic decline.…”

Section: Hw Virmentioning

confidence: 99%

Period and amplitude variations in post-common-envelope eclipsing binaries observed with SuperWASP

Lohr

Norton

Anderson

et al. 2014

A&A

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Period or amplitude variations in eclipsing binaries may reveal the presence of additional massive bodies in the system, such as circumbinary planets. Here, we have studied twelve previously-known eclipsing post-common-envelope binaries for evidence of such light curve variations, on the basis of multi-year observations in the SuperWASP archive. The results for HW Vir provided strong evidence for period changes consistent with those measured by previous studies, and help support a two-planet model for the system. ASAS J102322−3737.0 exhibited plausible evidence for a period increase not previously suggested; while NY Vir, QS Vir and NSVS 14256825 afforded less significant support for period change, providing some confirmation to earlier claims. In other cases, period change was not convincingly observed; for AA Dor and NSVS 07826147, previous findings of constant period were confirmed. This study allows us to present hundreds of new primary eclipse timings for these systems, and further demonstrates the value of wide-field high-cadence surveys like SuperWASP for the investigation of variable stars.

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“…Several evolutionary channels have been proposed: (1) commonenvelope ejection channels, leading to sdBs in binaries with orbital periods below ∼10 d and a white dwarf or low-mass main sequence companion; (2) a stable Roche lobe overflow channel resulting in binary systems with orbital periods between ∼10 d and ∼100 d and much thicker hydrogen envelopes; and (3) a double helium white dwarf merger channel that gives rise to single sdB stars with very thin hydrogen envelopes and a wider mass range (Han et al 2002(Han et al , 2003. Recently, sdBs with planetary companions were found (Silvotti et al 2007;Charpinet et al 2011;Beuermann et al 2012), rejuvenating the idea that interactions of a star with a planetary companion might also lead to Appendix A is available in electronic form at http://www.aanda.org the formation of sdBs (Soker & Harpaz 2000). The evolutionary scenarios remain largely untested.…”

Section: Introduction and State Of The Artmentioning

confidence: 99%

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

Bloemen

Aerts

et al. 2014

A&A

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We have computed a new grid of evolutionary subdwarf B star (sdB) models from the start of central He burning, taking into account atomic diffusion due to radiative levitation, gravitational settling, concentration diffusion, and thermal diffusion. We have computed the non-adiabatic pulsation properties of the models and present the predicted p-mode and g-mode instability strips. In previous studies of the sdB instability strips, artificial abundance enhancements of Fe and Ni were introduced in the pulsation driving layers. In our models, the abundance enhancements of Fe and Ni occur naturally, eradicating the need to use artificial enhancements. We find that the abundance increases of Fe and Ni were previously underestimated and show that the instability strip predicted by our simulations solves the so-called blue edge problem of the subdwarf B star g-mode instability strip. The hottest known g-mode pulsator, KIC 10139564, now resides well within the instability strip even when only modes with low spherical degrees (l ≤ 2) are considered.

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The quest for companions to post-common envelope binaries

Cited by 80 publications

References 39 publications

Origin of apparent period variations in eclipsing post-common-envelope binaries

Origin of apparent period variations in eclipsing post-common-envelope binaries

Period and amplitude variations in post-common-envelope eclipsing binaries observed with SuperWASP

The blue-edge problem of the V1093 Herculis instability strip revisited using evolutionary models with atomic diffusion

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