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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20090702T000000
DTEND;TZID=Atlantic/Canary:20090702T010000
UID:iactalks-137
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/137
CREATED:2009-07-02T00:00:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:The role of massive black hole recoil in galaxy evolution
DESCRIPTION:The role of massive black hole recoil in galaxy evolution\nMiss
  Javiera Guedes\n\nThe coalescence of a massive black hole (MBH) binary le
 ads to the gravitational-wave recoil of the system and its ejection from t
 he galaxy core. We have carried out N-body simulations of the motion of a 
 M=3.7 M⊙ MBH remnant in the “Via Lactea I” Milky Way-sized halo.
  The hole receives a kick velocity of Vkick = 80, 120, 200, 300, and 400 k
 m/s at redshift 1.5, and its orbit is followed for over 1 Gyr within a “
 live” host halo, subject only to gravity and dynamical friction against 
 the dark matter background. We show that, owing to asphericities in the da
 rk matter potential, the orbit of the MBH is highly non-radial, resulting 
 in a significantly increased decay timescale compared to a spherical halo.
  The simulations are used to construct a semi-analytic model of the motion
  of the MBH in a time-varying triaxial Navarro-Frenk-White dark matter hal
 o plus a spherical stellar bulge, where the dynamical friction force is ca
 lculated directly from the velocity dispersion tensor. Such a model should
  offer a realistic picture of the dynamics of kicked MBHs in situations wh
 ere gas drag, friction by disk stars, and the flattening of the central cu
 sp by the returning hole are all negligible effects. We find that, in a Mi
 lky Way-sized galaxy, a recoiling hole carrying a gaseous disk of initial 
 mass ~2 MBH may shine as a quasar for a substantial fraction of its “wan
 dering” phase. The long decay timescales of recoiling MBHs predicted by 
 this study may thus be favorable to the detection of off-nuclear quasar ac
 tivity.\n\n
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