marta volonteri - cscamm · marta volonteri university of michigan. hierarchical evolution of mbhs....
TRANSCRIPT
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Marta Volonteri
University of Michigan
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Hierarchical evolution of MBHs
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What we want to know
‣ How and when BHs accrete mass
‣ How fast BHs spin
‣ How and when BHs merge
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What we want to know
‣ How and when BHs accrete mass
‣ How fast BHs spin
‣ How and when BHs merge
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Mergers and accretion
Katzantidis et al., Mayer et al., di Matteo et al.,
Hopkins et al.
Do MBHs accrete before
or after
merging?
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- “Standard” numerical Bondi-Hoyle accretion
- No feedback
courtesy of S. Callegari
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- turbulent motions
- extrapolation from the refined simulation
courtesy of S. Callegari
High resolution
simulations: M-σ
without feedback
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MBHs in merger remnants Dotti et al. 2009
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Central MBH: MBH = 4 × 106 M
Gaseous disk (Mestel): MDisc = 108 M
RDisc = 100 pc
Stellar bulge (Plummer):
MBulge = 7 ⋅ 108 M
a = 55 pc
Secondary MBH: MBH = 4 × 106 M e ≈ 0.7 co- or counter- rotating
MBHs in circumnuclear disks Dotti et al. 2009
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MBHs in circumnuclear disks Dotti et al. 2009
Adiabatic evolution: ‘COLD’ disk: γ=7/5 ‘HOT’ disk: γ=5/3
Accretion: - accrete only bound particles, within Bondi radius - need to resolve the MBHs Bondi radii (h=0.1 pc)
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Modulation in the accretion rate of the
orbiting MBH
Accretion rate depends on the relative velocity
between MBH and gas
Co-rotating MBH (γ=5/3)
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Accretion rate depends on the relative velocity
between MBH and gas
Accretion rate jumps when the MBH starts co-rotating – angular
momentum flip
Counter-rotating MBH (γ=5/3)
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MBH mass accretion
Accretion depends on the
orbital evolution
Accretion depends on the
thermodynamical properties of the gas
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What we want to know
‣ How and when BHs accrete mass
‣ How fast BHs spin
‣ How and when BHs merge
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The second hair: spins ✔ maximal accretion efficiency
Schwarzschild: spin=0 ε=0.06 maximally rotating: spin=0.998 ε=0.31
✔ growth time
✔ importance of Blandford-Znajek energy extraction
✔ GW parameters estimates
✔ recoil velocities
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Gravitational recoil binary center of mass recoil during coalescence due to
asymmetric emission of GW
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a1 a2 L
L
a1 a2
a1 a2
L
Low kick velocities (~100 km s-1) ~vesc from high-z galaxies
High kick velocities (~1000 km s-1) ~vesc from today’s galaxies
Recoiling MBHs
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500.000 MC realizations for each q=m2/m1: - |a| homogeneously distributed between 0 and 1 - directions isotropically distributed
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Recoiling MBHs
Random distribution of spin moduli
MBH mass ratio directly from the simulations:
q=m2/m1~1 in-plane spins spin-orbit
isotropy
aligned spins
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Spin evolution accretion rate Simulations ang. mom. accreting flow
Dotti,MV et al. 2009
Perego,.., MV 2009
Bardeen-Peterson effect → BH- SS disc alignment
{
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Spin evolution: Bardeen-Peterson effect Perego,.., MV 2009
see also Martin et al 2007;
Lodato & Pringle 2006, 2007
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Spin evolution
a ϑ
Secondary BH
Primary BH
CRE=cold disc,retrograde orbit HPE=hot disc, prograde orbit
Gas rich mergers : spins align to orbital angular momentum
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Recoiling MBHs
Random distribution of spin moduli
aligned spins
spin-orbit isotropy
in plane spins HOT COLD
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Spin evolution: semi-coherent accretion cold disc hot disc
spins tend toward intermediate-large values
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Spin evolution in gas-rich mergers
✔ MBH mergers : spins align to orbital angular momentum
✔ MBH accretion: spins tend to intermediate-large values
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What we want to know
‣ How and when BHs accrete mass
‣ How fast BHs spin
‣ How and when BHs merge
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MBH orbital decay
The orbital evolution depends on the
thermodynamical properties of the gas
The orbital evolution depends on accretion
if MBHs swallow gas, the density decreases
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Hey, where are all these merging MBHS?
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Hunting for sub-parsec binaries SDSS
J092712.65+294344.0 (Bogdanovic et al. 09, Dotti,.., MV et al. 09)
SDSS J153636.22+044127.0
(Boroson & Lauer 09, Chornok et al. 09?)
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Sub-parsec binary QSOs MV, Miller & Dotti 2009
JMM’s challenge: You predict all these tens of mergers per year that LISA will detect. How come there are so few sub-parsec binary QSOs in the SDSS?!?
• MBH merger rate from hierarchical evolving MBH population • select only MBHs with vorb>2000 km/s
• assign luminosity all MBHs are active at some level
quasars are triggered by galaxy mergers
• assign lifetime
(Merloni 2009)
(Haiman et al. 2009)
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All MBHs are active at some level
Merger-driven quasar activity
Most MBH binaries are expected to occur at ‣ higher redshift ‣ lower masses
than sampled by the SDSS quasar catalog MV et al 2003; Sesana, MV & Haardt 2007
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➡ accretion: need to study jointly with dynamics and
thermodynamics
➡ mergers + accretion: determine how fast MBHs
spin at merger, and the magnitude of recoil velocity
➡ orbital decay: need to study jointly with
thermodynamics and accretion
➡ merging MBHs are good at hiding!
Summary