New Insights into the Dynamics of Planets in P-Type Motion Around Binaries

Funk, B.; Eggl, Siegfried; Gyergyovits, M.; Schwarz, Richard P.; Pilat-Lohinger, Elke

doi:10.1017/s1743921311028018

Cited by 2 publications

(2 citation statements)

References 3 publications

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“…The dynamical stability of the first fitted planetary configurations (Beuermann et al 2010) were investigated with detailed N-body simulations by Funk et al (2011) andHorner et al (2012b) who found that some were unstable, whereas others were dynamically feasible. In the first fit, the outer planet's eccentricity was set to zero.…”

Section: Introductionmentioning

confidence: 99%

Second generation planet formation in NN Serpentis?

Völschow

Banerjee

Hessman

2014

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In this paper, we study the general impact of stellar mass-ejection events in planetary orbits in post-common envelope binaries with circumbinary planets like those around NN Serpentis. We discuss a set of simple equations that determine upper and lower limits for orbital expansion and investigate the effect of initial eccentricity. We deduce the range of possible semi-major axes and initial eccentricity values of the planets prior to the common-envelope event. In addition to spherically-symmetric mass-ejection events, we consider planetary dynamics under the influence of an expanding disk. In order to have survived, we suggest that the present planets in NN Ser must have had semi-major axes > ∼ 10 AU and high eccentricity values which is in conflict with current observations. Consequently, we argue that these planets were not formed together with their hosting stellar system, but rather originated from the fraction of matter of the envelope that remained bound to the binary. According to the cooling age of the white dwarf primary of 10 6 yr, the planets around NN Ser might be the youngest known so far and open up a wide range of further study of second generation planet formation.

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Section: Introductionmentioning

confidence: 99%

Second generation planet formation in NN Serpentis?

Völschow

Banerjee

Hessman

2014

A&A

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“…The proposed companions around HU Aqr have been studied in detail, and a series of studies have revealed them to be dynamically unfeasible (Horner et al 2011;Hinse et al 2012a;Wittenmyer et al 2012a;Funk et al 2011Funk et al , 2012Goździewski et al 2012). The same is true of HW Vir ) and NSVS 14256825 Hinse et al 2014).…”

Section: Introductionmentioning

confidence: 99%

On the RZ Draconis substellar circumbinary companions

Hinse

Horner

Lee

et al. 2014

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Context. Recently, using the light-travel time effect, planets and substellar companions have been proposed to orbit around binary star systems (also known as circumbinary companions) as a result of variations in timing of the observed eclipses. For the majority of these systems the proposed orbital architecture features a crossing of the orbital configurations as a result of high eccentricities for one or both of the companions. For such systems, strong mutual gravitational interactions are expected, resulting in catastrophic orbital instabilities, or collisions between the proposed components, on very short timescales. Aims. We re-examine the primary and secondary eclipse timings of the short-period and semi-detached binary RZ Draconis (RZ Dra). The proposed companions were reported to have masses of around 0.07 and 0.18 M with the inner companion on an orbit with moderate eccentricity (0.46), whose apocenter distance crosses the orbit of the outer companion. We show that the companions proposed previously follow highly unstable orbits. In an attempt to find a stable system we searched the underlying χ 2 parameter space for a best-fit model and carried out an orbit-stability study to test possible best-fit models. If the binary period changes are truly due to additional massive companions in a hierarchical configuration, they must follow stable orbits. Methods. For numerical orbital stability calculations we used well established orbit integration routines. Computations were carried out using a large-scale multi-CPU computing environment. Our data analysis of times of primary and secondary eclipse is based on the Levenberg-Marquardt least-squares minimization algorithm using the two-body Keplerian light-travel time effect model. Results. Despite the wide variety of potential models tested for the RZ Dra system in this work, we found very few models that were stable for even one million years, with the vast majority of systems tested falling apart on timescales of just hundreds of years. It seems therefore likely that the observed timing variations are not solely the result of massive, unseen companions.

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New Insights into the Dynamics of Planets in P-Type Motion Around Binaries

Cited by 2 publications

References 3 publications

Second generation planet formation in NN Serpentis?

Second generation planet formation in NN Serpentis?

On the RZ Draconis substellar circumbinary companions

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