Monday, 19 October 2020

homework and exercises - Escape velocity from a rotating black hole


Under Newton, the escape velocity is


vesc=c rs/r


where rs=2 GM/c2. In the nonrotating relativistic case (the Schwarzschild case) the radial escape velocity is the same:


vesc=c rs/r



which is the speed of light, v=c, at the event horizon at r=rs. Since the photon sphere, where an object with v=c would not escape, but be captured into orbit, is at r=3 GM/c2, the transverse escape velocity is


vesc=c rs/r÷1rs/r


and for the observed (shapiro delayed) velocity v the transformation is


v=v 1rs/r ,  v=v (1rs/r)


so the observed angular motion is the same as with Newton, yet locally higher, while the observed radial motion is slowed down because of the radial length contraction and time dilation.


But what about the Kerr case where the rotation is significant and the event horizon is at r=(1+1a2) GM/c2 instead of r=rs?


A testparticle which is locally at rest and therefore corotating with the angular velocity of the frame dragging


Ω=dϕ/dt=2 a r/((a2+r2)2a2(a2+(r2) r)sin2(θ))


should experience the time dilation factor


˙t=dt/dτ=((a2+(r2) r)(a2cos2(θ)+r2))/((a2+r2)2a2(a2+(r2) r)sin2(θ))



relatively to the far away observer, so multiplying Ω with ˙t should give the local frame dragging angular velocity, which, multiplied with the x2+y2 value of the Boyer-Lindquist to cartesian transformation should give the transverse velocity - this is slightly below c for a maximaly rotating black hole (with a=1 - at the edge of the outer equatorial ergosphere where r=1 and R=r2+a2).


But how do I find the radial and total escape velocity, and what are the rules to convert the shapiro-delayed coordinate velocities dr/dt , dϕ/dt ,dθ/dt to the local 3-velocity components v and v of a test particle (local meaning relatively to a frame dragged probe with contant r)? The radial length contraction seems a bit different than in the Schwarzschild-case, where it is the same as the gravitational time dilation factor...



Answer



2 hours left to award the bounty, but no answear so far. At least I found out that the local 3-velocity v=v2r+v2θv2ϕ=v2x+v2yv2z

is related to the coordinate derivatives ˙r, ˙θ, ˙ϕ
by vr1v2=˙r ΣΔ
for the radial component, vθ Σ1v2=˙θ Σ
with the radius of gyration ˉR=(a2+r2)2a2Δsin2θa2cos2θ+r2
for the motion along the latitude and vϕ ˉR1v2=˙ϕ Σ
for the motion along the axis of symmetry, with the terms Σ=r2+a2cos2θ,Δ=r22 r+a2
and x, y, z as the cartesian transformation of the Boyer-Lindquist coordinates.


With the gravitational time dilation


ς=(a2+r2)2a2(a2+(r2)r)sin2(θ)(a2+(r2)r)(a2cos2(θ)+r2)


and


ς=11v2esc


the radial escape velocity should be


vesc=ς21ς



which, in the limit of a0 gives the same result as Schwarzschild.


Example of a testparticle being thrown radially upwards with the local escape velocity by a corotating ZAMO sitting close above the horizon at θ=45°:


enter image description here


(The Spin parameter in the animation is a=Jc/G/M²=0.998)


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