Stellar wind accretion and accretion disk formation: applications to neutron star high mass X-ray binaries

Abstract

Recent X-ray observations have revealed the complexity and diversity of high-mass X-ray binaries (HMXBs). This diversity challenges a classical understanding of the accretion process onto the compact objects. In this study, we reinforce the conventional concept of the nature of wind-fed accretion onto a neutron star considering the geometrical effect of radiatively accelerated wind, and re-evaluate the transported angular momentum by using a simple wind model. Our results suggest that even in an OB-type HMXB fed by stellar wind, a large amount of angular momentum could be transported to form an accretion disk due to the wind-inhomogeneity, if the binary separation is tight enough and/or stellar wind is slow. We apply our model into actual systems such as LMC X-4 and OAO 1657-415, and discuss the possibility of disk formations in these systems.

12 pages, 12 figures, accepted for publication in PASJ

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Cited by in corpus (9)

• Spectral evidence of an accretion disk in wind-fed X-ray pulsar Vela X-1 during an unusual spin-up period
• A semi-analytical treatment to wind accretion in neutron star supergiant high mass X-ray binaries: I. eccentric orbits
• Spin evolution of neutron stars in wind-fed high mass X-ray binaries
• High-Mass X-Ray Binaries with Be Donors as Ultraluminous X-Ray Sources
• Soft excess in the quiescent Be/X-ray pulsar RX J0812.4-3114
• Possible TeV $\gamma$-ray binary origin of HESS J1828-099
• Torque reversal and orbital profile of X-ray pulsar OAO 1657-415
• Torque reversals and wind variations of X-ray pulsar Vela X-1
• The chemical nature of Orion protostars: Are ORANGES different from PEACHES? ORANGES II