摘要By numerically solving the set of basic equations describing black hole accretion flows with low accretion rates, we show that although the dynamical structure of these flows is essentially unaffected by radiative processes in comparison with the case in which the radiation is not considered, the radiative cooling can be more important than the advective cooling in the flow's convection-dominated zone, and this result may have implications to distinguish observationally convection-dominated accretion flows from advection-dominated accretion flows.
Abstract：By numerically solving the set of basic equations describing black hole accretion flows with low accretion rates, we show that although the dynamical structure of these flows is essentially unaffected by radiative processes in comparison with the case in which the radiation is not considered, the radiative cooling can be more important than the advective cooling in the flow's convection-dominated zone, and this result may have implications to distinguish observationally convection-dominated accretion flows from advection-dominated accretion flows.
[1] Narayan R, Mahadevan R and Quataert E 1998 The Theory of BlackHole Accretion Discs ed Abramowicz M A, Bj\"ornsson G and Pringle J E(Cambridge: Cambridge University Press) p 148 [2] Narayan R 2002 Proc. ESO Astrophys. Symp. Lighthouses ofthe Universe ed Gilfanov M, Sunyaev R and Churasov E (Garching 6-10August 2001) p 405 [3] Narayan R and Yi I 1994 Astrophys. J. 428 L13 [4] Narayan R, Igumenshchev I V and Abramowicz M A 2000 Astrophys. J. 539 798 [5] Quataert E and Gruzinov A 2000 Astrophys. J. 539 809 [6] Lu J F, Li S L and Gu W M 2004 Mon. Not. R. Astron. Soc.London 352 147 [7] Abramowicz M A, Igumenshchev I V, Quataert E and Narayan R 2002 Astrophys. J. 565 1101 [8] Lu J F and Gu W M 2002 Nuovo Cimento B 117 733 [9] Igumenshchev I V and Abramowicz M A 2001 AIP Conf. Proc. 586 656 [10] Pen U L, Matzner C D and Wong S 2003 Astrophys. J. 596 L207 [11] Paczyński B and Wiita P J 1980 Astron. Astrophys. 8823 [12] Dullemond C P and Turolla R 1998 Astrophys. J. 503 361 [13] Pan L B, Lu J F and Gu W M 2002 Chin. Astron. Astrophys. 26 7 [14] Lu J F, Lin Y Q and Gu W M 2004 Astrophys. J. 602 L37 [15] Shakura N I and Sunyaev R A 1973 Astron. Astrophys. 24337
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