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TwoparametersdescribeBH:MassMandspinaAppearanceofBHalsodependsonaccretionrateAppearanceisaffectedbytheinclination活动星系核（AGN)吸积的基本模式SpectrumfromADAFComparisonoftheSpectraGierlinski&Done2003CompositeSEDforAGN观测光谱指向冷热两相吸积唯像模型：内区热吸积流＋外区冷吸积盘只能解释低光度天体吸积盘＋热冕（ADAF）解释高光度天体理论上。。。Two-phaseaccretionflowsinBHXRBsSpectrafromdiskandcoronaAccretioninAGN吸积模型应用到活动星系核所遇到的困难Spectrumfromdisk+coronainsoftstateHaardt&Maraschi1993两相吸积流中容易被忽略的问题InverseComptonscatteringofdiskemissionPotentialproblemsinmagnetizedaccretionflowAssumptionsinAGNaccretionmodelsAHybridtwo-componentaccretionflowFormassaccretionrateslessthan~0.01condensationdoesnotoccuratanydistance,nothindiskcansteadilyexisttheaccretionflowremainasahotaccretionflow,i.e.ADAF/RIAF.SameasthecaseforBHXRBs,thoughthemasssupplytotheaccretionisdifferentPreliminaryresultsTheSpectrumConclusionremarksAccretionofInterstellarMediuminAGNTwo-phaseaccretionflowsSummary
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