2. 2015-5-202 (1) 黑洞的基本物理 (2) 解释 AGN 的连续谱辐射的产生机制 UV － optical IR Lecture 3

3. 2015-5-203 Rees 图 Rees （ 1984 ） 黑洞的形成

4. 2015-5-204 牛顿力学： 黑洞的定义 广义相对论： （ 1 ）球对称（ Schwarzschild ）, 无角动量 c = G = 1 进入视界的粒子在有限的时间内不可避免地落到中心。因此，视界包围的部分不 是恒星那样的实体，而更像一个 “ 洞 ” 。视界包围的部分称为黑洞，更准确地说， 史瓦西黑洞。

5. 2015-5-205 黑洞的定义 （ 2 ）轴对称（ Kerr-Newman ），有电荷，有角动量。 Q ＝ 0  Kerr 解 c = G = 1

6. 2015-5-206

7. As in stars, the rate at which energy is emitted by the nucleus gives us the rate at which energy must be supplied to the nuclear source by accretion: Fuelling Rate 能量平衡

8. Accretion: conversion of gravitational potential energy to radiation. To power a typical AGN requires an accretion rate Most important ! η 的计算， Soltan 假设

9. 有效势能取极小的位置即最内稳定 圆轨道（ Last stable circular orbit ）

12. If we ignore relativistic effects, set r=5Rs (which is about where most of the optical/UV continuum radiation is expected to originate):  0.1, which is an order of magnitude more efficient than fusion of hydrogen to helium (  =0.007). 取  0.1 ， L QSO  10 46 erg s -1

13. If we ignore relativistic effects, set r=5Rs (which is about where most of the optical/UV continuum radiation is expected to originate):  0.1, which is an order of magnitude more efficient than fusion of hydrogen to helium (  =0.007). 取  0.1 ， L QSO  10 46 erg s -1 ASCA (Tanaka et al. 1995)

16. Problem of Angular Momentum The mass accretion rate necessary to sustain the Eddington luminosity. In the simple spherical accretion model, Eddington accretion rate is a maximum possible accretion rate for mass M. This critical rate can easily be exceeded with the models that are not spherically symmetric, such as mass accretion occurs in a disk. （ accrete ionized hydrogen gas ） The major problem with fuelling a quasar by gravitational accretion is not the energy requirement, but angular momentum, since the accretion disk is so small. Infalling gas must lose most of its AM before reaching the AD, where further AM transfer can occur through viscosity.

17. The AM per unit mass is L/m=(GMr) 1/2, where M is the mass interior to r, i.e., M=10 11 M sun and r=10kpc.If this unit mass is moved to within 0.01 pc of a 10 7 M sun central BH, where the viscosity might become important, its AM per unit mass must decrease to (10 7 x 0.01pc/10 11 x10 4 pc)~10 -5 of its initial value. Gravitational interactions with other galaxies are sometimes suspected of playing a major role in fuelling AGNs. Problem of Angular Momentum

18. Tidally-disrupted Star near BH Fuel also could be tidally disrupted stars, which place an upper limit on the central BH mass. A star of mass density  near a massive body of density  BH and radius R can approach no closer than the familiar Roche limit Without being tidally disrupted. To ensure that a star is tidally disrupted before it crosses the event horizon requires r R > R S

19. Tidally-disrupted Star near BH ULMER 1999 Gezari et al. 2006

20. Tidally-disrupted Star near BH ULMER 1999 Disrupt Giant Stars?

21. 2015-5-2021 AGN 的连续谱 归一化 平均谱

22. 2015-5-2022 AGN 的连续谱 SED 弥散很大

23. 2015-5-2023 AGN 的连续谱

24. 2015-5-2024 小篮包

25. 2015-5-2025

26. 2015-5-2026 AGN 的连续谱

27. 2015-5-2027 UV-Optical Continuum

28. 2015-5-2028 A More correct derivation takes into account how the energy is dissipated in the disk through viscosity which is a consequence of work done by viscous torques. If r >> Ri then UV-Optical Continuum

29. 2015-5-2029 UV-Optical Continuum

30. 2015-5-2030 UV-Optical Continuum

32. 2015-5-2032 UV-Optical Continuum

33. 2015-5-2033 UV-Optical Continuum

34. 2015-5-2034 UV-Optical Continuum

35. 2015-5-2035 UV-Optical Continuum(SS)

36. 2015-5-2036 UV-Optical Continuum(ADAF)

37. 2015-5-2037 UV-Optical Continuum

38. 2015-5-2038

39. 2015-5-2039

40. 2015-5-2040 UV-Optical Continuum

41. 2015-5-2041

42. 2015-5-2042 Free － free 发射拟合大蓝包

43. 2015-5-2043 Free － free 发射拟合大蓝包

44. 2015-5-2044 小篮包

45. 2015-5-2045