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Bode (1774)
Collaborators: Holger Baumgardt Toshi Ebisuzaki Ortwin Gerhard Alessia Gualandris Piet Hut Jun Makino Steve McMillan
Black Hole Immigrants welcome in the Galactic center
Simon Portegies ZwartUniversity of Amsterdam
M80
Arches
Quintplet
R136
NGC 3603
30 pc
~1 000 000 Msun
Trapezium
Wstrlnd1
MG
G11
5pc
Pleiades
Myr
100Myr
100Myr
Core collapse in a realistic clusterhappens much earlier than in an idealized system. The collapse itself, however, is much shallower.
Portegies Zwart et al 2004Remember: John Fregeau's talk!
supernovae
starlab/kira
6NBODY
High concentration
M82 X1Matsumoto1999
Figer et al 1999Arches clusterQuintuplet
IRS13 (Maillard 2005)
SupermassiveBlack hole
Star cluster
1100pc
Background galaxy
In the tidal field of the Galaxy
N=1128kWo=312RLfilling
Final configurationfor R=8pc N=64k W=3Dissolved at ~4pcBut made IMBH
45.000Msun star cluster sinking from 2pc to the Galactic center.
N=131074
Mbh = 1000Msun
Mbh = 3000Msun
See also Gurkan 2005, Levin 2005, Hansen 2006
Portegies Zwart et al 2005
Baumgardt et al 2006
A total of 7 HVSs (v>700km/s) are found (Brown et al 2005, 2006)
10000Msun
1000Msun
Baumgardt etal (in prep)See also Levin 2005, 2006and Gnedin 2005
Binary breakupHills 1989, Yu&Tremaine 1994
IMBH spiralin
Results and future prospects● About 10.000 star clusters formed within 100pc● 510% of these experience runaway collision● Producing IMBHs of 3003000Msun● At any time there are ~50 IMBHs within the
inner 10pc, and several within the inner mpc● One in 30 IMBHs is still accompanied by a
young (<30Myr) star cluster which is unusually rich in massive (>10Msun) stars, much like IRS13
● The rate at which the IMBHs fall in the SMBH is roughly 1/10Myr