Two Planets Orbiting The Recently Formed Post-Common Envelope Binary NN Serpentis

dc.contributor.utaustinauthorWinget, D. E.en_US
dc.contributor.utaustinauthorMiller, G. F.en_US
dc.creatorBeuermann, K.en_US
dc.creatorHessman, F. V.en_US
dc.creatorDreizler, S.en_US
dc.creatorMarsh, T. R.en_US
dc.creatorParsons, S. G.en_US
dc.creatorWinget, D. E.en_US
dc.creatorMiller, G. F.en_US
dc.creatorSchreiber, M. R.en_US
dc.creatorKley, W.en_US
dc.creatorDhillon, V. S.en_US
dc.creatorLittlefair, S. P.en_US
dc.creatorCopperwheat, C. M.en_US
dc.creatorHermes, J. J.en_US
dc.description.abstractPlanets orbiting post-common envelope binaries provide fundamental information on planet formation and evolution. We searched for such planets in NN Ser ab, an eclipsing short-period binary that shows long-term eclipse time variations. Using published, reanalysed, and new mid-eclipse times of NN Ser ab obtained between 1988 and 2010, we find excellent agreement with the light-travel-time effect produced by two additional bodies superposed on the linear ephemeris of the binary. Our multi-parameter fits accompanied by N-body simulations yield a best fit for the objects NN Ser (ab)c and d locked in the 2:1 mean motion resonance, with orbital periods P-c similar or equal to 15.5 yrs and P-d similar or equal to 7.7 yrs, masses M-c sin i(c) similar or equal to 6.9 M-Jup and M-d sin i(d) similar or equal to 2.2 M-Jup, and eccentricities e(c) similar or equal to 0 and e(d) similar or equal to 0.20. A secondary chi(2) minimum corresponds to an alternative solution with a period ratio of 5:2. We estimate that the progenitor binary consisted of an A star with similar or equal to 2 M-circle dot and the present M dwarf secondary at an orbital separation of similar to 1.5 AU. The survival of two planets through the common-envelope phase that created the present white dwarf requires fine tuning between the gravitational force and the drag force experienced by them in the expanding envelope. The alternative is a second-generation origin in a circumbinary disk created at the end of this phase. In that case, the planets would be extremely young with ages not exceeding the cooling age of the white dwarf of 10(6) yrs.en_US
dc.description.sponsorshipAlfried Krupp von Bohlen und Halbach Foundation, Essen 085.D-0541en_US
dc.description.sponsorshipUK's STFCen_US
dc.description.sponsorshipFONDECYT 1061199en_US
dc.description.sponsorshipCentre of Astrophysics Valparaisoen_US
dc.description.sponsorshipNorman Hackerman Advanced Research Program 003658-0255-2007en_US
dc.identifier.citationBeuermann, Klaus, F. V. Hessman, S. Dreizler, T. R. Marsh, S. G. Parsons, Donald Earl Winget, G. F. Miller et al. >Two planets orbiting the recently formed post-common envelope binary NN Serpentis.> Astronomy & Astrophysics, Vol. 521 (Oct., 2010): L60.en_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectbinaries: eclipsingen_US
dc.subjectplanetary systemsen_US
dc.subjectstars: individual: nn seren_US
dc.subjectcataclysmic variablesen_US
dc.subjectplanets and satellites: formationen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleTwo Planets Orbiting The Recently Formed Post-Common Envelope Binary NN Serpentisen_US

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