Bulk Comptonization GRB Model and its Relation to the Fermi GRB Spectra
GRBs from rotating black holes - · Bloom et al. 2002 GRB supernova association Reeves et al. 2002...
Transcript of GRBs from rotating black holes - · Bloom et al. 2002 GRB supernova association Reeves et al. 2002...
Maurice H.P.M. van Putten (MIT)
Eve C. Ostriker (Maryland)Amir Levinson (Tel Aviv)
Gerald E. Brown (SUNY Stony Brook)Abhinanda Sarkar (IBM)
David Coward and Ronald R. Burman (UWA)Stephen Eikenberry (Cornell)
Hyun Kyu Lee (Hanyang)
GRBs from rotating black holes
value)(Euclidean 1/2
0.008 0.338 /max
<±=>< VV
25.1≈>< Z
Phenomenology
Clustering-spread in GRB energies and opening angle
Frail et al., 2001
Bloom et al. 2002
GRB supernova association
Reeves et al. 2002
GRB 011121 (z=0.36) GRB 011211 (z=2.41)
HST similar to GRB 1998bw XMM detection of light elements
GRBs: what’s in the black box?
Baryon-poor beamed outflowsCompact and energetic sourceLong-duration (some 20 s, or 10e4 dynamical time-scales)
Method:
Study all energy emissions (in grb, gws, thermal and nu-emissions)Study progenitors and remnants
Rees & Meszaros ‘92,94Rees, this morningPiran, ’98,’99Frail et al. ’01…
2. NS/BH binary coalescence Pacyznski 1991
Core-collapse in rapidly spinning magnetized star in a binary
1. Woosley-Paczynski-Brown hypernovae
Rapid/slow black hole spin from close/wide progenitor binaries
Woosley 1993Pacznski 1998
Brown et al. 2000Woosley, this morning
Lee, Brown & Wijers, 2002
Black hole plus disk or torus systems
Most favored GRB progenitors
Black hole mass 3-15MSolar in SXTs
Some of SXTs may be relics of GRBsBrown et al., 2000
Israelian et al., 1999
Orosz et al., 2001
Kerr black holes
Baryon-free objects Frame-dragging of spacetime Compact energy reservoir in angular momentum
Kerr 1963
Outline
• Bimodal distribution of durations from two accretion modes
• Minor output: BPJ from differential frame-dragging in a dissipative gap
• Major output: gravitational radiation from a torus around a black hole
• Searches for gravitational wave bursts in hypernovae
“A tango between a torus and a black hole”
THPSR Ω−Ω=Ω
dtdJT H /−=+
TPSR Ω=Ω
cpt infinity innerface
-
Equivalence in poloidal topology to pulsars (a)
dtdJT H /−=+=> Causal interactions
Equivalence in poloidal topology to pulsars (b)M
ach’
s pr
inci
ple
cpt infinity
PSR spun-up as infinity wraps around itPSR spun-down by losses to infinity
Long durations from a suspended accretion state
E = ½ Cq2 – µHB
Van Putten, Phys. Rep., 2001H.-K. Lee et al., MNRAS, 2001
Coupling in lowest energy state of black hole
µH = aBJH
Approximately uniform and maximal horizon flux at all spin-rates
Capacitance C=1/rH
Carter (1968) µH = qJH/M ``no fourth hair”
Net charge from symmetries l=1,m=0in a surrounding force-free magnetosphere
0 / /*
>−==
rr BBEEoddevenoddeven
θθ (odd) rB
(odd) θE
(even) θB
0,1 == mlY Cohen et al. 1975 Charge on a sphere from
Suspended accretion state for the life-time of rapid spin
Van Putten & Ostriker 2001
Van Putten (2001)
88s MH10Msun( ) MH /Md
100( ) g2(θ)tspin = δEk/δEB100( )
Black hole-torus coupling at high spin-rate by eHµ
As torus catalyzes spin-energy, the black hole slows downby conservation of total energy and angular momentum
Maxwell stress on the horizon of the black hole Blandford & Znajek (1977)Ruffini & Wilson (1975)
Hyper-accretion onto slowly rotating black holes
Magnetic torque: δτB = Ω sin2θ ( m Af)δAf, µ=cosθInertial balance: δτB = ½ Ω RRδM
.
ω = R/R0 :~ ω(τ;Af)=(1-t/tf)a~
α = ½ in split monopole geometry (SMG)2 In toroidal field geometry (TFG)
0.057s Rd1000km( )
2MH
10Msun( )-1
δEkδEBtfSMG <
0.011s Rd1000km( )
2MH
10Msun( )-1
δEkδEB
g(θ)tfTMG >
δEk /δEB ~ 10-100 produces tf ~ few seconds
Two accretion modes: suspended- and hyperaccretionfor long and short GRBs
Van Putten & Ostriker 2001
Bimodal distribution in durations when Md << MH
Evidence for a suspended accretion state?
Van Putten, Science, 1999
“turbulent shear flow in the torus resulting from the powerful torques acting on it”
Excess heating of inner accretion disk, in broad iron emission lines
XTE J1650-500 MCG-6-30-15
Miller et al., submitted
Wilms et al., 2001 Li-Xin Li 2002
Van Putten, Science 1999Physics Reports 2001
Formation of baryon-poor outflows along open flux-tubes
µH supports open flux tubes
eHµ Tµ
slip/slipno-slip/slip
no-slip/slip
no-slip/no-slip
B- t
opol
ogy
Geometry:flat versus
twisted
``Woman with amirror”(II-III BC)
©Van Putten 2001
Differential frame-draggingaround a Kerr black hole
Equivalence in poloidal topology to pulsars (c)ρ−
topo
logy
+ +
− −
−+
− −Q>0 Q<0
Differential Frame-dragging on an open flux-tube ρ−
topo
logy
+ +
− −
−+
− −Q>0 Q<0
Differential rotation of open flux tube
van Putten, Phys. Rep., 2001
B
HΩ
1
2
ϕAI
+Ω=
ϕAI
H)(
−Ω−Ω=
“Current continuity enforces a dissipative gap”
Lp = ½ ΩT(ΩH − 2ΩT)Af2
Low-sigma outflows from a differential rotation
Van Putten, Phys. Rep., 2001
Van Putten & Levinson, ApJL, 2001
Current continuity over open flux-tube (ΩH − Ω+)Αf = Ω-Αf
Global current closure over outer flux-tube Ω-Αf = ΩTΑf
Output from a differentially rotating gap P = I∆V/2 = I(Ω+ − Ω-)Αf/2
Low-sigma baryon poor jets
)0( =Φ+Φ Ti
Clustering-spread in BPJs
Van Putten & Levinson, ApJL, 2001
cwjj LL /=θ
θH
θj
(a) θH ~ 2 ½ (Erot /Egrb) ¼ (ΩT /ΩH) ¼ ε - ¼ ~ 35o
(b) Ecw ~ (2fb)-½ Egrb ε-1 ~ 1052 erg
θj < 35o
(a) standard (b) variable
Levinson & Eichler, PRL,2000
Lp = ½ ΩT(ΩH − 2ΩT)Af2
Test:Positive correlation true GRB energy ~ M, and durations ~ M^p
(p=1-2)
Energy paradox in long GRBs: true GRB energies 0.01% E-rot
Suspended accretion state converts all E-rot
Unseen emissions in GWsemitted in all directions
Thorne (1996)
LIGO sensitivity curve
Balance in angular momentum and energy transport for atorus around a black hole with a quadrupole mass moment
with the constitutive ansatz for dissipation
by turbulent MHD stresses, into thermal emissions and (conceivably) neutrino emissions
22 )( −+ Ω−Ω≈ rAP
Prad
rad
+Ω+Ω=Ω+=
−−++
−+
ττττττ
Suspended accretion with gravitational radiation
Solutions
%15.0
1)/(2
)1(
2/322
2
2
≈
+≈
++≈
ΩΩ
≈+
≈
Mm
MRfff
OfL
L
T
wH
H
H
T
wH
GW
δ
α
αα
) and 23( 2radGWw Lf τα Ω=−=
True energy budget in emissions from a Kerrblack hole
Van Putten & Levinson, Science, 2002
Minor
Major
jGW EE 100≈
)/( wavesnalgravitatioin 2/
)35( GRBs input to as 21
21
T
22
Hrot
GW
oH
H
rot
j
EE
E
E
ΩΩ=≈
≈
−
−≈
ηη
θθ
ηη
η
A sample of 12 GRBs with measured redshifts and durations
0
0.5
1
1.5
2
2.5
3
3.5
5 10 15 20 25 30 35 40 45 50 55 60 65 70 75 80 85 90
de-redshifted duration [s]
NExpected distribution of durations in LIGO/VIRGO detections
Mean duration ~ 25 sEvent rate ~ 1/yr within 100Mpc
Observational test for Kerr black holes
005.0d20
>∫GWE
GW Efπ
Van Putten, ApJ, 562, L51, 2001;Van Putten & Levinson, Science, 2002
Black hole-torus system Neutron star limit
Image by P.F.A.M. van Putten
• A MAJOR fraction of E-rot of a Kerr black hole is emitted in gravitationalradiation (some 10-20%)
• A MINOR fraction of E-rot of a Kerr black hole is emitted in BPJ as input toGRBs (some 0.1-0.2%)
• These emissions are simultaneous and for the same duration (about 25 s)
• Events 2pi Ef > 0.005 indicate the presence of a Kerr black hole
Strategy: LIGO/VIRGO searches in hypernovae, ~1 per year within D=100Mpc
S/N ~ 2 advanced LIGO (single detector operation) S/N > 2 using dual recycled interferometers
Conclusions
Cutler & Thorne gr-qc/0204090
Harry et al. 2002