the dynamics of black holes in a gaseous...
TRANSCRIPT
The Dynamics of Black Holes in aGaseous Medium
Andres EscalaYale University/Universidad de Chile
November 2002
Advisors: Paolo Coppi, Richard Larson.
Conclusions.
Outline
Scientific Motivation.
Role of Hydrodynamical Friction in theCoalescence of a Binary SMBH.
Evolution After the End of the HydrodynamicalFriction Regime.
SMBH History in the Context ofGalaxy Formation
Current Galaxy Formation Theory is based on Hierarchical Mergers.
What is the fate of the BH's? Will they also Coalesce?
Such Mergers show aVariety of PhysicalConditions. The easiestdistinction is between gasrich and gas poor mergers.
Steinmetz 02'
Hydrodynamical Friction
FHDF = -4π (G ΜΒΗ)2 ρ vBH-2 F(vBH/CS)
Hydrodynamical Friction
FHDF = -4π (G ΜΒΗ)2 ρ vBH-2 F(vBH/CS)
Ostriker '99
Isothermal Sphere
Non Singular Isothermal Spherein Hydrostatic Equilibrium.
Nsph=400,000
One BH (Mbh= 0.01Mgas) initially
in a circular orbit.
Spiral Shock, v=1.1 cS.
X
Y
Evolution of a Single BHinitially in a circular orbit.Hydrostatic gas sphere.Stellar sphere in dynamical
equilibrium.Stronger decay in the gas
sphere (factor of 2).
Isothermal Sphere
Gas
Stars
Adiabatic Sphere
Adiabatic (n=1.5) Sphere inHydrostatic Equilibrium.Single BH (Mbh= 0.01Mgas)
initially in a circular orbit.
Qualitatively same spiral
feature, v=1.1 cS.
X
Y
Hydrostatic gas sphere.Stellar sphere in dynamical
equilibrium.Transonic regime: stronger
decay in the gas sphere.Subsonic regime: comparable.
Adiabatic Sphere
Gas
Stars
Isothermal Sphere
Binary BH initially in acircular orbit.
Spiral shock, v=1.1 cS.
Non-singular isothermalsphere in hydrostaticequilibrium.
X
Y
Isothermal Sphere
0.020.1 0.06
Evolution of the binary'sseparation.Mbinary/Mgas: 0.02,0.06,0.1.
Tsound=1, orbital period=2.
Adiabatic (n=1.5) sphere inhydrostatic equilibrium.Binary BH in a circular
orbit.
Mbinary= 0.02Mgas
Adiabatic Sphere
Adiabatic Sphere
Evolution of the Binary'sSeparation.Mbinary/Mgas: 0.02,0.06,0.1.
Tsound=2, orbital period=4.The total effect is 2-3 times
weaker than isothermal.
0.02
0.06
0.1
Comparison
0.02
0.06
0.1
0.020.1 0.06
t/tsound
[tsound=0.5 torbital]
t/tsound
Isothermal Adiabatic
Efficient Drag Force.
Drag Force (Ostriker 1999) Mach Number
The RadialProfile of the Mach Number (vrot/CS) is Important.
Isothermal
Adiabatic
Strong Drag
Scaling.
Gas Sphere withMgas=1010MO, r=200pc.
Tsound=1.6 106 yr
A Binary SMBH with Mbh=5 108 MO will reduce itsseparation from 200pc to 3pc in 8 106 yr.
Gravitational Radiation Coalescence Timescale (Peters 64'):
tGR = 0.08 c5a4(G3M123)-1 F(e) = 1011 yr > tHo
Non-singular isothermalsphere in hydrostaticequilibrium.
Futher Evolution
Binary BH with Mbinary =Mgas
Roughly equivalent to theevolution of the binary(0.01Mgas) in sphere insider=0.2
X
Y
Non-singular isothermalsphere in hydrostaticequilibrium.
Evolves from spherical toflattened configuration.
Z
X
Futher Evolution (X-Z Plane)
Z
X
Binary BH with Mbinary =Mgas
Evolution of the binary'sseparation.
Mbinary = Mgas
No signature ofcoalescence stalling.
Futher Evolution
.... Still running
Conclusions
With gas, radial Mach number profile is also important(not just density profile).
In the transonic regime the coalescence timescales areshorter (factors of 2) than the stellar (collisionless) case.
Dissipative nature of gas can produce more condencedconfigurations (shorter timescales).
Instead the coalescence is driven by interaction withcircumbinary envelope. No evidence (yet) of stalling.
When binary BH dominates local gravitational potential,the coalescence is no longer hydrodynamical friction.