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Super-Eddington accretion discs with advection and outflows around magnetized neutron stars
Univ Turku, Dept Phys & Astron, Tuorla Observ, Turku 20014, Finland.;Lomonosov Moscow State Univ, Sternberg Astron Inst, Univ Sky Pr 13, Moscow 119992, Russia..
Lomonosov Moscow State Univ, Sternberg Astron Inst, Univ Sky Pr 13, Moscow 119992, Russia..ORCID iD: 0000-0003-4515-8955
Univ Turku, Dept Phys & Astron, Tuorla Observ, Turku 20014, Finland.;Lomonosov Moscow State Univ, Sternberg Astron Inst, Univ Sky Pr 13, Moscow 119992, Russia..
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Univ Turku, Dept Phys & Astron, Tuorla Observ, Turku 20014, Finland.;Russian Acad Sci, Space Res Inst, Profsoyuznaya Str 84-32, Moscow 117997, Russia.;KTH Royal Inst Technol, NORDITA, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden..
2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 626, article id A18Article in journal (Refereed) Published
Abstract [en]

We present a model for a super-Eddington accretion disc around a magnetized neutron star taking into account advection of heat and the mass loss by the wind. The model is semi-analytical and predicts radial profiles of all the basic physical characteristics of the accretion disc. The magnetospheric radius is found as an eigenvalue of the problem. When the inner disc is in radiation-pressure-dominated regime but does not reach its local Eddington limit, advection is mild, and the radius of the magnetosphere depends weakly on the accretion rate. Once it approaches the local Eddington limit the disc becomes advection-dominated, and the scaling for the magnetospheric radius with the mass accretion rate is similar to the classical Alfven relation. Allowing for the mass loss in a wind leads to an increase in the magnetospheric radius. Our model can be applied to a wide variety of magnetized neutron stars accreting close to or above their Eddington limits: ultra-luminous X-ray pulsars, Be/X-ray binaries in outbursts, and other systems. In the context of our model we discuss the observational properties of NGC5907 X-1, the brightest ultra-luminous pulsar currently known, and NGC300 ULX1, which is apparently a Be/X-ray binary experiencing a very bright super-Eddington outburst.

Place, publisher, year, edition, pages
EDP Sciences, 2019. Vol. 626, article id A18
Keywords [en]
accretion, accretion disks, stars: neutron, stars: magnetic field, X-rays: binaries
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-254079DOI: 10.1051/0004-6361/201834414ISI: 000470073000007OAI: oai:DiVA.org:kth-254079DiVA, id: diva2:1330288
Note

QC 20190625

Available from: 2019-06-25 Created: 2019-06-25 Last updated: 2019-06-25Bibliographically approved

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Poutanen, Juri

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