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Novikov, I.D.1
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33750283528
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note
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Throughout the paper we use geometrized units G = c=1, where G is the Newtonian gravitational constant, c is the speed of light.
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M. Kishimoto, R. Antonucci, and O. Blaes, astro-ph/0304118
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I.V. Igumenshchev, R. Narayan, and M.A. Abramowicz, astro-ph/0301402.
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Blandford, R.D.1
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O.M. Blaes, astro-ph/0211368
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O.M. Blaes, astro-ph/0211368.
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0000272453
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A large-scale magnetic field in an accretion disk can arise in at least two ways: (1) Inherited from the progenitor of the disk. For example, the merger of a magnetized neutron star with a black hole will naturally lead to the formation of a disk with a large-scale magnetic field. (2) Generated from small-scale magnetic fields through reconnection. See, e.g., C. A. Tout and J. E. Pringle, Mon. Not. R. Astron. Soc. 281, 219 (1996).
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39
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33750307025
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note
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In this paper we use the word "sonic" to refer to "magnetosonic" since we have assumed that the gas pressure is zero.
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41
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0004057466
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The University of Chicago Press, Chicago
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R.M. Wald, General Relativity (The University of Chicago Press, Chicago, 1984).
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General Relativity
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Wald, R.M.1
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42
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85107714081
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note
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n+1 or higher.
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45
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85107714961
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note
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r=0 here so must be located at r=∞ and is not relevant.
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50
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33750292741
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N. Afshordi and B. Paczyński, astro-ph/0202409
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N. Afshordi and B. Paczyński, astro-ph/0202409.
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51
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33750353176
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The contour plot is drawn with MATHEMATICA
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The contour plot is drawn with MATHEMATICA.
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59
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0004148601
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Oxford University Press, New York
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L. Mestel, Stellar Magnetism (Oxford University Press, New York, 1999).
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Stellar Magnetism
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Mestel, L.1
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60
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85107713195
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note
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φ|≪1 at large radii.
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|