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A Super-Eddington Wind Model for GRO J1655–40

Published online by Cambridge University Press:  12 April 2016

David L. Meier
David L. Meier*
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109

Abstract

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A model for GRO J1655–40 is described in which the hard X/γ-ray behavior, and long delay between the X/γ and radio outbursts, are explained by processes which occur when the accretion rate approaches and exceeds the Eddington limit. The principal feature of the model is a dense, optically thick, super-Eddington wind ejected from the center of the accretion disk. The wind is responsible for determining the luminosity and spectral evolution of the object and for suppressing the formation of a fast, relativistic jet while the accretion rate is above the Eddington limit.

Our model makes use of the “magnetic switch” mechanism we recently discovered with MHD simulations of jet production in magnetized accretion disk coronae. A fast jet can be turned on (or off) by increasing (or decreasing) the Alfvén velocity in the corona relative to a critical value. Examination of models of sub- and super-Eddington disks shows that VA remains below the critical value while the wind is present, but could exceed it when the wind disappears and a hot, optically thin corona forms.

Type
Part 2. Black Hole Transient Sources
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 68 - 72
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Bailyn, C.D. et al. 1995, Nature, 378, 157.CrossRefGoogle Scholar
Begelman, M.C. & Meier, D.L. 1982, ApJ, 253, 873.Google Scholar
Blandford, R.D. & Payne, D.G. 1982, MNRAS, 199, 883.Google Scholar
Campbell-Wilson, D. & Hunstead, R. 1994, IAU Circ. No. 6052 & 6055.Google Scholar
Harmon, B.A. 1995, private communication.Google Scholar
Harmon, B.A., et al. 1995, Nature, 374, 703.Google Scholar
Hawley, J.F. 1991, ApJ, 381, 496.Google Scholar
Hjellming, R.M. & Rupen, M.P. 1995, Nature, 375, 464.Google Scholar
Meier, D.L. 1982, ApJ, 256, 693.Google Scholar
Meier, D.L. 1996, ApJ, 459, 185.Google Scholar
Meier, D.L., Edgington, S.F., Godon, P., Payne, D.G., and Lind, K.R. 1996, in preparation.Google Scholar
Mirabel, I.F. & Rodriguez, L.F. 1994, Nature, 371, 46.Google Scholar
Papaloizou, J.C.B., & Pringle, J.E. 1984, MNRAS, 208, 721.Google Scholar
Shakura, N.I. & Sunyaev, R.A. 1973, A&A, 24, 337.Google Scholar
Tingay, S.J. et al. 1995, Nature, 374, 141.Google Scholar
Wilson, C.A. et al. 1994, IAU Circ. No. 6056.Google Scholar