吸積盤的蒸發(fā)與冕(編輯修改稿)
2025-10-22 23:21 本頁面
【文章內容簡介】 pendence on the accretion rate 臨界吸積率 Two basic spectral states Schematic view of accretion in hard and soft state Transition of spectrum ? Xray transients ? Outburst: MdotMdotcrit, soft state ? quiescence: MdotMdotcrit, hard state ? Persistant Xray binaries ( X1) Mdot varying up and down hard/soft spectral transition Change occurs at L~1037ergs/s (Mdot~1017g/s) Change from outer thin disk to inner corona/ADAF What causes the change of accretion mode and how to determine rtr? Narayan et al (1998) Done et al. 2022 What causes the change of accretion mode? 基本思想：盤內區(qū)的強蒸發(fā)耗空內盤，從而使吸積由外區(qū)薄盤主導過渡到內區(qū) ADAF主導，轉換半徑由黑洞質量與吸積率決定。 ADAF+Disk+Corona 黑洞 冷盤 熱冕 ADAF Log r Log m . Accretion flows around BH ? ADAF/CDAF: Very lowmdot system . Quiescent BHCs ? Inner ADAF+Outer disk+corona:Low mdot ? Standard disk+corona: Medium/high mdot ? Slim disk (+corona？ ): Very highmdot system Hysteresis in Xray binariesAdditional support to the disk evaporation model Schematic light curve of an Xray nova outburst Model explanation Different irradiation in hard and soft state leads to different evaporation rate and transition rate Compton cooling AGN 中的吸積 Observational features in AGN ? SED: powerlaw ? Radio: synchrotron ? IR: warm dust grain ? BBB: disk ? Soft xray excess+ hard Xray tail: disk+ptonization+Bremsstrahlung ? fluorescent iron lines: reflection of hard Xrays ? SED indicates hot plasma + cold gas, which is monly thought to be corona+thin disk Theoretical disk+corona model in AGNs ? 盤與冕特征： AGN盤輻
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