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(200) N no\ 10)$ ῌaQpq) rst) uvtpq VwxyaQ+@"7K) rstzuv. ῎῍ῑῌ 1) Tamazawa S., Toyama K., Kaneko N., Ono Y., 1975, ApSpSci 32, 403 2) Kato S., Fukue J., Mineshige S., 1998, Black-Hole Accretion Disks (Kyoto University Press) 3) Fukue J., 2005a, PASJ 57, 841 4) Fukue J., 2005b, PASJ 57, 1023 5) Fukue J., 2006a, PASJ 58, 187 6) Turolla R., Nobili L., 1988, MNRAS 235, 1273 7) Turolla R., Zampieri L., Nobili L., 1995, MNRAS 272, 625 8) Dullemnod C. P., 1999, A&A 343, 1030 9) Fukue J., 2006b, PASJ 58, 461 10) Akizuki C., Fukue J., 2006, in preparation. t+@9 {) BK|}~+F#
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(202) J) 234lmM+?9 -N $ -X) /; =!- * +S ῌBK;. Jun FUKUE Astronomical Institute, Osaka Kyoiku University, Asahigaoka 4῍698῍1, Kashiwara, Osaka 582῍ 8582, Japan. QR. I,QR{) BK; QR -8 ? $ "¡¢£¤56 FLD (fluxlimited di#usion) {¥-8 ? $ ¦§ ? ) #) ¨"gXI -) \"£K?$. º 99 ». Velocity-Dependent Eddington Factor in Relativistic Radiation Hydrodynamics. º9¼. Abstract : We here introduce a “velocitydependent Eddington factor,” which may be useful for moment formalisms in relativistic radiation hydrodynamics. Such a field of AAA class in theoretical astronomy is important for the recent trend in astrophysics, such as black hole accretion flow, relativistic jets, gamma-ray bursts, neutrino tranfer, dynamical phenomena in the early universe.. 513.
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