CRUISE NEWS IN BIO
CRUISE NEWS IN BIO Uni Stu 4
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This 18 page Class Notes was uploaded by Danielle Moore on Saturday September 12, 2015. The Class Notes belongs to Uni Stu 4 at University of California - Irvine taught by Staff in Fall. Since its upload, it has received 47 views. For similar materials see /class/201929/uni-stu-4-university-of-california-irvine in University Studies at University of California - Irvine.
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Date Created: 09/12/15
in circumnuclear disks Massimo Dotti Collaborators Marta Volonteri Unlversrty of Mrchrgan Mateusz Ruszkowski Monica Colpi Francesco Haardt Lucio Mayer Luca Paredi Albino Perego Irvine 422009 MBHs evolution in a stellar background Begelman Blanford amp Rees 1980 o Dynamical friction tidal stripping DF efficient only for major mergers Kazantzidis et a1 2005 Callegan39 et a1 2009 0 Three body interactions loss cone depletion non spherical background massive perturbers Milosavljevic amp Merritt 2001 Berczik Merritt amp Spurzem 2005 Perets amp Alexander 2008 O Gravitational wave emission I 14 amv 00014pc h F l4 tel t 26 Gyr t 30 Gyr l 43 Gyr 6 kpc scale 5322 G55 39 60 kpc scale39 Mayer et al 2007 Face0n 5 160 pc scale MBHs evolution in gaseous backgrounds FAQ Do the MBHS reach the final coalescence Are the MBHs observable during their dynamical evolution Initial conditions Central MBH of 4 x 106 Mo Equal mass merger Gaseous disk Mestel second MBH of4 x 106 Mo and e z 07 20 R0 00 or counter rotating R MDisc 108 RDisc Pure adiabatic evolution y53 75 Spaans amp Silk 2000 Stellar bulge Plummet EDiskR Z Q J1 une 9039 4 B91 1 4W uquot MBulge 7 X 108 a 55 pc Accretion Each set of initial conditions has been used for two different runs MBHs can accrete gas particles MBHs can not accrete gas particles gas particles are accreted only if their total energy kineticthermalpotential in the reference frame of the MBHs is less than a fixed fraction 8 of the negative gravitational energy 8 gt05 accretion possible only resolving the BHL radius of the MBHs No feedback Dynamics 3 O MD et a1 2009 MD et a1 2009 S W gt 0 quot 1 r 4 E 0 0 0 Q 40 N 1 VBH V Env 0 Orbital angular momentum ip MD et al in prep corotating m o L H E o 5 m L nu a G V counterrotating Accretion events MD et a1 2009 Modulation in the orbiting MBH accretion rate fEdd function of the e ltfEddtlt25Myr gt Z 03 Lb0116X1044 ergs central MBH orbiting MBH ltfEddtgt25 Myr gt Z 045 Lbol Z 24X1044 ergs MD et a1 2009 1BH accretion rate depending on the sign of the angular momentum ltfEddtlt3Myr gt S 01 Lbolz 5X1043 ergs central ltf dd tgt 3Myr gt z orbiting MBH Lbol 24X1044 ergs Spin evolution Spin evolution A MD et a1 2009 MD et a1 2009 accretion rate From the simulations gt L of the accretng ow ycm 4141015 5 10 77 MD et a1 2009 accretion rate From the simulations gt L of the accretng ow 04 06 08 1 t Myr MD et al 2009 Random distribution of spin moduli anti aligned kilns sin orbit in lane isotrov sins Vkick kmS
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