English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Periodic pulsations have been found in emission from the ultra-luminous X-raysource (ULX) M82 X-2, strongly suggesting that the emitter is a rotatingneutron star rather than a black hole. However, the radiation mechanisms andaccretion mode involved have not yet been clearly established. In this paper,we examine the applicability to this object of standard accretion modes forhigh mass X-ray binaries (HMXBs). We find that spherical wind accretion, whichdrives OB-type HMXBs, cannot apply here but that there is a natural explanationin terms of an extension of the picture for standard Be-type HMXBs. We showthat a neutron star with a moderately strong magnetic field, accreting from adisc-shaped wind emitted by a Be-companion, could be compatible with theobserved relation between spin and orbital period. A Roche lobe overflowpicture is also possible under certain conditions.

Accretion mode of the Ultra-Luminous X-ray source M82 X-2