Evolution of intermediate-mass X-ray binaries driven by magnetic braking of Ap-Bp stars: I. Ultracompact X-ray binariesReportar como inadecuado




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Reference: Chen, W-C and Podsiadlowski, Philipp, (2016). Evolution of intermediate-mass X-ray binaries driven by magnetic braking of Ap/Bp stars: I. Ultracompact X-ray binaries. The Astrophysical Journal, 830 (2), 131.Citable link to this page:

 

Evolution of intermediate-mass X-ray binaries driven by magnetic braking of Ap/Bp stars: I. Ultracompact X-ray binaries

Abstract: It is generally believed that ultracompact X-ray binaries (UCXBs) evolved from binaries consisting of a neutron star accreting from a low-mass white dwarf(WD) or helium star where mass transfer is driven by gravitational radiation. However, the standard WD evolutionary channel cannot produce the relatively long-period (40–60 minutes) UCXBs with ahigh time-averaged mass-transfer rate. In this work, we explore an alternative evolutionary route toward UCXBs, where the companions evolve from intermediate-mass Ap/Bp stars with an anomalously strong magnetic field (100–10,000 G). Including the magnetic braking caused by the coupling between the magneticfield and an irradiation-driven wind induced by the X-rayflux from the accreting component, we show that intermediate-mass X-ray binaries(IMXBs)can evolve into UCXBs. Using theMESAcode, we have calculated evolutionary sequences for a large number of IMXBs. The simulated results indicate that, for a small wind-driving efficiency f=10^−5, the anomalous magnetic braking can drive IMXBs to an ultra-short period of 11 minutes. Comparing our simulated results with the observed parameters of 15identified UCXBs, the anomalous magnetic braking evolutionary channel can account for the formation of seven and eight sources with f = 10^-3, and 10^−5, respectively. In particular, a relatively large value of f canfit three of the long-period, persistent sources with ahigh mass-transfer rate. Though the proportion of Ap/Bp stars in intermediate-mass stars is only 5%, the lifetime of the UCXB phase is 2 Gyr, producing a relatively high number of observable systems, making this an alternative evolutionary channel for the formation of UCXBs.

Publication status:PublishedPeer Review status:Peer reviewedVersion:Publisher's versionDate of acceptance:2016-08-08 Funder: University of Henan Province   Funder: China Scholarship Council   Funder: National Science Foundation of China   Notes:© 2016. The American Astronomical Society. All rights reserved.

Bibliographic Details

Publisher: Institute of Physics

Publisher Website: http://www.iop.org/

Journal: The Astrophysical Journalsee more from them

Publication Website: http://iopscience.iop.org/journal/0004-637X

Volume: 830

Issue: 2

Extent: 131

Issue Date: 2016-10

pages:131Identifiers

Doi: https://doi.org/10.3847/0004-637X/830/2/131

Issn: 1538-4357

Uuid: uuid:4a876a0a-3421-49c8-8d99-6632316158d2

Urn: uri:4a876a0a-3421-49c8-8d99-6632316158d2

Pubs-id: pubs:638436 Item Description

Type: journal-article;

Version: Publisher's versionKeywords: binaries: general stars: evolution stars: mass-loss X-rays: binaries

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Autor: Chen, W-C - Oxford, MPLS, Physics, Astrophysics - - - Podsiadlowski, Philipp - Oxford, MPLS, Physics, Astrophysics St Edmund Hall

Fuente: https://ora.ox.ac.uk/objects/uuid:4a876a0a-3421-49c8-8d99-6632316158d2



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