The quest for companions to post-common envelope binaries

Beuermann, K.; Breitenstein, P.; Dębski, B.; Diese, J.; Dubovský, Pavol A.; Dreizler, S.; Hessman, F. V.; Hornoch, K.; Husser, T. O.; Pojmański, G.; Wolf, M.; Woźniak, P. R.; Zasche, P.; Denk, B.; Langer, Matej; Wagner, C. A.; Wahrenberg, D.; Bollmann, T.; Habermann, F. N.; Haustovich, N.; Lauser, M.; Liebing, F.; Niederstadt, F.

doi:10.1051/0004-6361/201118105

Cited by 48 publications

(58 citation statements)

References 24 publications

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“…Whilst Niarchos et al (2003) and Çamurdan et al (2012) provided confirmatory light curve parameters, most investigators (Qian et al 2009(Qian et al , 2013Çamurdan et al 2012;Beuermann et al 2012;Pulley et al 2015) have focused on an apparent quasi-periodic variation in the eclipsing binary period. Although not proven, and following the rejection of other possible mechanisms, e.g.…”

Section: Recent Data and Ephemerismentioning

confidence: 99%

The quest for stable circumbinary companions to post-common envelope sdB eclipsing binaries

Pulley

Faillace

Smith

et al. 2018

A&A

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Context. Period variations have been detected in a number of eclipsing close compact binary subdwarf B stars (sdBs) and these have often been interpreted as caused by circumbinary massive planets or brown dwarfs. According to canonical binary models, the majority of sdB systems are produced from low mass stars with degenerate cores where helium is ignited in flashes. Various evolutionary scenarios have been proposed for these stars, but a definite mechanism remains to be established. Equally puzzling is the formation of these putative circumbinary objects which must have formed either from the remaining post common envelope circumbinary disk or survived its evolution. Aims. In this paper we review the eclipse time variations (ETVs) exhibited by seven such systems (EC10246-2707, HS0705+6700, HS2231+2441, J08205+0008, NSVS 07826147, NSVS 14256825 and NY Vir) and explore if there is conclusive evidence that the ETVs observed over the last two decades can reliably predict the presence of one or more circumbinary bodies. Methods. We report 246 new observations of the seven sdB systems made between 2013 September and 2017 July using a worldwide network of telescopes. We combined our new data with previously published measurements to analyse the ETVs of these systems. Results. Our data shows that period variations cannot be modelled simply on the basis of circumbinary objects. This implies that more complex processes may be taking place in these systems. These difficulties are compounded by the secondary star not being spectroscopically visible. From eclipse time variations, it has historically been suggested that five of the seven binary systems reported herein had circumbinary objects. Based on our recent observations and analysis only three systems remain serious contenders. We find agreement with other observers that at least a decade of observations is required to establish reliable ephemeris. With longer observational baselines it is quite conceivable that the data will support the circumbinary object hypothesis of these binary systems. Also we generally agree with other observers that larger values of (O-C) residuals are found with secondary companions of spectral type M5/6 or earlier possibly as a result of an Applegate type mechanism

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Section: Recent Data and Ephemerismentioning

confidence: 99%

The quest for stable circumbinary companions to post-common envelope sdB eclipsing binaries

Pulley

Faillace

Smith

et al. 2018

A&A

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“…On the basis of very similar O−C variations, Beuermann et al (2012a) argue for a single circumbinary low-mass companion in an elliptical orbit, while Almeida et al (2013) prefer a twoplanet model. Hinse et al (2014), however, find that the data are insufficient to constrain any particular one-planet model, and provide no convincing evidence for a second circumbinary companion.…”

Section: Nsvs 14256825mentioning

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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“…Apsidal motion can be excluded if the expected shift of the secondary eclipse is found to be absent (e.g. Beuermann et al 2010Beuermann et al , 2012. The high frequency of exoplanets around normal stars has resulted in a re-consideration of the third-body hypothesis, starting with a series of papers by the group of Qian et al (2009Qian et al ( , 2010, and references therein).…”

Section: Discussionmentioning

confidence: 99%

“…So far only a handful of post-common envelope binaries (PCEBs) with circum-binary planets have been found (e.g. Lee et al 2009;Qian et al 2009Qian et al , 2010Beuermann et al 2010Beuermann et al , 2011Beuermann et al , 2012, but other PCEBs display similar orbital period variations (e.g. Parsons et al 2010;Qian et al 2011), giving the impression that there might be an intimate connection between the evolution of close binaries, the ejection of the CE, and the presence of planets.…”

Section: Introductionmentioning

confidence: 99%

The quest for companions to post-common envelope binaries

Backhaus

Bauer²,

Beuermann

et al. 2012

A&A

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As part of an ongoing collaboration between student groups at high schools and professional astronomers, we have searched for the presence of circum-binary planets in a bona-fide unbiased sample of twelve post-common envelope binaries (PCEBs) from the Catalina Sky Survey (CSS) and the Sloan Digital Sky Survey (SDSS). Although the present ephemerides are significantly more accurate than previous ones, we find no clear evidence for orbital period variations between 2005 and 2011 or during the 2011 observing season. The sparse long-term coverage still permits O-C variations with a period of years and an amplitude of tens of seconds, as found in other systems. Our observations provide the basis for future inferences about the frequency with which planetsized or brown-dwarf companions have either formed in these evolved systems or survived the common envelope (CE) phase.

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The quest for companions to post-common envelope binaries

Cited by 48 publications

References 24 publications

The quest for stable circumbinary companions to post-common envelope sdB eclipsing binaries

The quest for stable circumbinary companions to post-common envelope sdB eclipsing binaries

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

The quest for companions to post-common envelope binaries

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