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Accretion Onto the Neutron Star in Be/X-ray Binaries

Published online by Cambridge University Press:  19 July 2016

Kimitake Hayasaki  and
Atsuo T. Okazaki
Kimitake Hayasaki
Affiliation:
Devision of Physics, Graduate School of Science, Hokkaido University, Kitaku, Sapporo 060-0810, Japan
Atsuo T. Okazaki
Affiliation:
Faculty of Engineering, Hokkai-Gakuen University, Toyohira-ku, Sapporo 062-8605, Japan

Abstract

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We study accretion onto the neutron star in Be/X-ray binaries, using a 3D SPH code and the data imported from a high resolution simulation by Okazaki et al. (2002) for a coplanar system with a short period (Porb = 24.3 d) and moderate eccentricity (e = 0.34). We find that a time-dependent accretion disk is formed around the neutron star in Be/X-ray binaries. The disk shrinks after the periastron passage of the Be star and restores its radius afterwards. Our simulations show that the truncated Be disk model for Be/X-ray binaries is consistent with the observed X-ray behavior.

Type
Part 11: Accreting Pulsars
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 449 - 450
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Bate, M. R., Bonnell, I. A., & Price, N. M. 1995, MNRAS, 277, 362.CrossRefGoogle Scholar
Okazaki, A. T., Bate, M. R., Ogilvie, G. I., & Pringle, J. E. 2002, MNRAS, 337, 967.CrossRefGoogle Scholar