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2008

Masses, Beaming and Eddington Ratios in Ultraluminous X-ray Sources

King, A. R.

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I suggest that the beaming factor in bright ULXs varies as $b \propto \dot m^{-2}$, where $\dot m$ is the Eddington ratio for accretion.

This is required by the observed universal $L_{\rm soft} \propto T^{-4}$ relation between soft--excess luminosity and temperature, and is reasonable on general physical grounds.
The beam scaling means that all observable properties of bright ULXs depend essentially only on the Eddington ratio $\dot m$, and that these systems vary mainly because the beaming is sensitive to the Eddington ratio.
This suggests that bright ULXs are stellar--mass systems accreting at Eddington ratios of order 10 -- 30, with beaming factors $b \ga 0.1$.

Masses, Beaming and Eddington Ratios in Ultraluminous X-ray Sources · Around

Built on

Shakura N. I., Sunyaev R. A., 1973, A&A, 24, 337
1973
Earlier work this paper cites.
King A. R., Begelman M. C., 1999, ApJ, 519, L169
1999
Earlier work this paper cites.
King A. R., Davies M. B., Ward M. J., Fabbiano G., Elvis M., 2001, ApJ, 552, L109
2001
Earlier work this paper cites.
King A. R., 2002, MNRAS, 335, L13
2002
Earlier work this paper cites.
King A. R., Puchnarewicz E. M., 2002, MNRAS, 336, 445
2002
Earlier work this paper cites.

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Then

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Later among the works it cites.
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Original
2008
Closest in time.
King A. R., 2008, MNRAS, 385, L113
2008
Closest in time.

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