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Magnetohydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries

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dc.contributor Aalto-yliopisto fi
dc.contributor Aalto University en
dc.contributor.author Navarrete, Felipe H.
dc.contributor.author Schleicher, Dominik R. G.
dc.contributor.author Kaepylae, Petri J.
dc.contributor.author Schober, Jennifer
dc.contributor.author Voelschow, Marcel
dc.contributor.author Mennickent, Ronald E.
dc.date.accessioned 2020-02-28T09:31:12Z
dc.date.available 2020-02-28T09:31:12Z
dc.date.issued 2020-01
dc.identifier.citation Navarrete , F H , Schleicher , D R G , Kaepylae , P J , Schober , J , Voelschow , M & Mennickent , R E 2020 , ' Magnetohydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries ' , Monthly Notices of the Royal Astronomical Society , vol. 491 , no. 1 , pp. 1043-1056 . https://doi.org/10.1093/mnras/stz3065 en
dc.identifier.issn 0035-8711
dc.identifier.issn 1365-2966
dc.identifier.other PURE UUID: f95743fe-b2f5-4f7a-a44e-b15302325bcd
dc.identifier.other PURE ITEMURL: https://research.aalto.fi/en/publications/magnetohydrodynamical-origin-of-eclipsing-time-variations-in-postcommonenvelope-binaries-for-solar-mass-secondaries(f95743fe-b2f5-4f7a-a44e-b15302325bcd).html
dc.identifier.other PURE FILEURL: https://research.aalto.fi/files/41216118/Navarrete_Magnetohydrodynamical.stz3065.pdf
dc.identifier.uri https://aaltodoc.aalto.fi/handle/123456789/43272
dc.description | openaire: EC/H2020/665667/EU//EPFL Fellows
dc.description.abstract Eclipsing time variations have been observed for a wide range of binary systems, including post-common-envelope binaries. A frequently proposed explanation, apart from the possibility of having a third body, is the effect of magnetic activity, which may alter the internal structure of the secondary star, particularly its quadrupole moment, and thereby cause quasi-periodic oscillations. Here, we present two compressible non-ideal magnetohydrodynamical simulations of the magnetic dynamo in a solar mass star, one of them with three times the solar rotation rate ('slow rotator'), and the other one with 20 times the solar rotation rate ('rapid rotator'), to account for the high rotational velocities in close binary systems. For the slow rotator, we find that both the magnetic field and the stellar quadrupole moment change in a quasi-periodic manner, leading to O-C (observed minus corrected times of the eclipse) variations of similar to 0.025 s. For the rapid rotator, the behaviour of the magnetic field as well as the quadrupole moment changes becomes considerably more complex, due to the less coherent dynamo solution. The resulting O-C variations are of the order of 0.13 s. The observed system V471 Tau shows two modes of eclipsing time variations, with amplitudes of 151 and 20 s, respectively. However, the current simulations may not capture all relevant effects due to the neglect of the centrifugal force and self-gravity. Considering the model limitations and that the rotation of V471 Tau is still a factor of 2.5 faster than our rapid rotator, it may be conceivable to reach the observed magnitudes. en
dc.format.extent 14
dc.format.extent 1043-1056
dc.format.mimetype application/pdf
dc.language.iso en en
dc.relation info:eu-repo/grantAgreement/EC/H2020/665667/EU//EPFL Fellows
dc.relation.ispartofseries Monthly Notices of the Royal Astronomical Society en
dc.relation.ispartofseries Volume 491, issue 1 en
dc.rights openAccess en
dc.subject.other 113 Computer and information sciences en
dc.title Magnetohydrodynamical origin of eclipsing time variations in post-common-envelope binaries for solar mass secondaries en
dc.type A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä fi
dc.description.version Peer reviewed en
dc.contributor.department Universidad de Concepción
dc.contributor.department Centre of Excellence Research on Solar Long-Term Variability and Effects, ReSoLVE
dc.contributor.department Observatoire de Sauverny
dc.contributor.department University of Hamburg
dc.contributor.department Department of Computer Science en
dc.subject.keyword dynamo
dc.subject.keyword MHD
dc.subject.keyword methods: numerical
dc.subject.keyword binaries: eclipsing
dc.subject.keyword stars: rotation
dc.subject.keyword WHITE-DWARF
dc.subject.keyword ACTIVITY CYCLES
dc.subject.keyword EVOLUTION
dc.subject.keyword CONVECTION
dc.subject.keyword MECHANISM
dc.subject.keyword MODELS
dc.subject.keyword STAR
dc.subject.keyword 113 Computer and information sciences
dc.identifier.urn URN:NBN:fi:aalto-202002282321
dc.identifier.doi 10.1093/mnras/stz3065
dc.type.version publishedVersion

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