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Discovery of orbital eccentricity and evidence for orbital period increase of SS433

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dc.contributor.author Cherepashchuk A.M.
dc.contributor.author Belinski A.A.
dc.contributor.author Dodin A.V.
dc.contributor.author Postnov K.A.
dc.date.accessioned 2022-02-09T20:40:44Z
dc.date.available 2022-02-09T20:40:44Z
dc.date.issued 2021
dc.identifier.issn 1745-3925
dc.identifier.uri https://dspace.kpfu.ru/xmlui/handle/net/169626
dc.description.abstract The examination of long-term (1979-2020) photometric observations of SS433 enabled us to discover a non-zero orbital eccentricity of e = 0.05 ± 0.01. We have also found evidence for a secular increase in the orbital period at a rate of ˙Pb=(1.0± 0.3)× 10-7 s s-1. The binary orbital period increase rate makes it possible to improve the estimate of the binary mass ratio q = MX/MV > 0.8, where MX and MV are the masses of the relativistic object and the optical star, respectively. For an optical star mass of 10 M⊙, the mass of the relativistic object (a black hole) is MX > 8 M⊙. A neutron star in SS433 is reliably excluded because in that case the orbital period should decrease, in contradiction to observations. The derived value of ˙Pb sets a lower limit on the mass-loss rate in the Jeans mode from the binary system 7 × 10-6 M⊙ yr-1. The discovered orbital ellipticity of SS433 is consistent with the model of the slaved accretion disc tracing the precession of the misaligned optical star's rotational axis.
dc.relation.ispartofseries Monthly Notices of the Royal Astronomical Society: Letters
dc.subject binaries: close
dc.subject stars: black holes
dc.subject stars: individual: SS433
dc.title Discovery of orbital eccentricity and evidence for orbital period increase of SS433
dc.type Article
dc.relation.ispartofseries-issue 1
dc.relation.ispartofseries-volume 507
dc.collection Публикации сотрудников КФУ
dc.relation.startpage L19
dc.source.id SCOPUS17453925-2021-507-1-SID85114596366


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