Hypernovae: GRB-supernovae as LIGO/VIRGO sources of gravitational radiation
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Transcript of Hypernovae: GRB-supernovae as LIGO/VIRGO sources of gravitational radiation
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Hypernovae: GRB-supernovae as Hypernovae: GRB-supernovae as LIGO/VIRGO sources of gravitational LIGO/VIRGO sources of gravitational
radiationradiation
Maurice H.P.M. van Putten (MIT-LIGO)Maurice H.P.M. van Putten (MIT-LIGO)
in collaboration within collaboration with
Amir Levinson (Tel Aviv)Amir Levinson (Tel Aviv) Stephen Eikenberry (U Florida)Stephen Eikenberry (U Florida)Tania Regimbau (MIT-LIGO)Tania Regimbau (MIT-LIGO)
Eve Ostriker (U Maryland)Eve Ostriker (U Maryland)Hyun Kyu Lee (Hanyang U)Hyun Kyu Lee (Hanyang U)David Coward (U of WA)David Coward (U of WA)
Ronald Burman (U of WA)Ronald Burman (U of WA)Paris 2003 LIGO-G030269-00-R
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Star-formation in a molecular cloud
Molecular cloud
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Core-collapse in a rotating massive star in a binary
Molecular cloud
Core-collapse(Woosley-Paczynski-Brown)
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Active stellar nuclei
Molecular cloud
Core-collapse(Woosley-Paczynski-Brown)
Active nucleus inside remnant stellar envelope
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Hypernovae: GRB-supernovae from rotating black holes
Jet through remnant envelope (McFadyen & Woosley’98)
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Hypernovae: GRB-supernovae from rotating black holes
Jet through remnant envelope (McFadyen & Woosley’98)
Torus produces winds & radiation:
Ejection of remnant stellar envelopeExcitation of X-ray line-emissions
van Putten (2003)
wr EE
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GRB-SNe in 011211 and 030329
2002) Ghisellini (G. 104 52rE Stanek, K., et al., 2003 astro-ph/0304173
GRB 011211 (z=2.41) Reeves et al. ‘02
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Outline
1. Quantitative phenomenology of GRB-supernovae
2. A causal spin-connection in active stellar nuclei
3. Durations of tens of seconds of long bursts
4. Calorimetry on radiation energies
5. Observational opportunities for Adv LIGO/VIRGO
6. Conclusions
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GRBs with redshifts (33) and opening angles (16)
GRB redshift angle instrument
GRB970228 0.695 SAX/WFCGRB970508 0.835 0.293 SAX/WFCGRB970828 0.9578 0.072 RXTE/ASMGRB971214 3.42 >0.056 SAX/WFCGRB980425 0.0085 SAX/WFCGRB980613 1.096 >0.127 SAX/WFCGRB980703 0.996 0.135 RXTE/ASMGRB990123 1.6 0.050 SAX/WFCGRB990506 1.3 BAT/PCAGRB990510 1.619 0.053 SAX/WFCGRB990705 0.86 0.054 SAX/WFCGRB990712 0.434 >0.411 SAX/WFCGRB991208 0.706 <0.079 Uly/KO/NEGRB991216 1.02 0.051 BAT/PCAGRB000131 4.5 <0.047 Uly/KO/NEGRB000210 0.846 SAX/WFCGRB000131C 0.42 0.105 ASM/UlyGRB000214 2.03 SAX/WFCGRB000418 1.118 0.198 Uly/KO/NEGRB000911 1.058 Uly/KO/NEGRB000926 2.066 0.051 Uly/KO/NEGRB010222 1.477 SAX/WFCGRB010921 0.45 HE/Uly/SAXGRB011121 0.36 SAX/WFCGRB011211 2.14 SAX/WFCGRB020405 0.69 Uly/MO/SAXGRB020813 1.25 HETEGRB021004 2.3 HETEGRB021211 1.01 HETEGRB030226 1.98 HETEGRB030328 1.52 HETEGRB030329 0.168 HETE
Barthelmy’s IPNhttp://gcn.gsfc.nasa.gov/gcn/Greiner’s cataloguehttp://www.mpe.mpg.de/jcg/grbgeb.htmland Frail et al. (2001)
<- very nearby!
<- most nearby!
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Durations of GRB-SNe True energy in gamma-rays
Frail et al. ‘01
erg103
s 10 few
50
90
E
T
Van Putten ‘02
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The true-but-unseen GRB-event rate
2001) al.et (Frail 500/1
:emissions-GRBin factor beaming lGeometrica
bf
0 1 2 3 4 50.0
0.1
0.2
0.3
0.4
0.5
prob
abili
ty
redshift z
observed simulated: observable simulated: total p
SFR2(z)
year/105.0 rateevent GRB True 6
Van Putten & Regimbau2003, submitted
Unseen event rate = 1/fb or 1/fr times observed event rate
submitted) 2003, Regimbau, &Putten (van 450 1/
:SFR the tolocked sample limited-fluxin rate-lossEvent
rf
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Phenomenology of GRB-SNe from rotating black holes
100MpcDn year withiper event 1
107/
101/
51
4900
rotEE
PT
erg104 :holeblack theofenergy Rotational
ms4 : torus theof periodKeplerian
:holeblack masssolar 7 aFor
54
rotE
P
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Magnetized nucleus in core-collapseMagnetized nucleus in core-collapse
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Goldreich and Julian (1969) (spin-down of pulsars (magnetized neutron stars))
Ruffini & Wilson (1975) (spin-down of black holes, but: weak fields)
Blandford & Znajek (1977) (strong fields, but: causality not addressed, Punsly & Coroniti 1990)…Van Putten (1999) (idem, with causality by topological equivalence to PSRs)…
A causal spin-connection to Kerr black holes
HVan Putten & Levinson, ApJ 2003; Science 2002Van Putten, Phys Rep, 2001; Science 1999
PSR+
PSR-
BH
PSR PSR
H 0
Spin-up Spin-down
Asy
mpto
tic
infinit
y
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Topology of inner and outer torus Topology of inner and outer torus magnetospheres magnetospheres
(vacuum case)(vacuum case)
separatrix
Van Putten & Levinson, ApJ 2003
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New magnetic stability criterion
0 BU
0 BU bR
Tidal dominated
Magnetic dominated
Sum of magnetic and tidal interaction
tilt
y]instabilit bucklingfor 1/15[ 12/1/ kB EE
Van Putten & Levinson, ApJ 2003
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Durations of long bursts
SS
T
H
rotspin M
M
M
RMM
ST
ET
7630
/s40
4
Van Putten & Levinson, ApJ 2003
Most of the spin-energy is dissipated “unseen” in the event horizon of the black hole
spinTT 90
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Long durations
40
13/840
900
10 1 ][
03.0/
1.0/
)03.0/()1.0/(102][
/ parameter Large
observed
MM
theory
PT
HT
HT
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Critical point analysis in baryon-rich torus windCritical point analysis in baryon-rich torus wind
115
3/152
3/12/1
2 1.007.0
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16surface] on torus[
p
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1-30 sg101M
6/1
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2
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MLT
MeV-torus cools by neutrino emission (electron-positron capture on nuclei)
Van Putten & Levinson ApJ 2003
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2MeV
Baryon-poor inner tube
Baryon-richOuter tube
Torus winds create open magnetic flux-tubes
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Van Putten & Levinson, submitted; Science 2002Van Putten, Phys Rep, 2001; Science 1999
PSR+
PSR-BH Magnetic wall
The active stellar nucleus: a black hole in suspended accretion
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Equilibrium charge distribution Equilibrium charge distribution
topolo
gy
Q>0Q>0 Q<0Q<0
Rapidly rotating black hole
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Energy in baryon-poor outflowsEnergy in baryon-poor outflows
)2/(/
surfaces-flux of curvature Poloidal
4/
axisrotation along tube-fluxopen in Outflow
3/2
22
2290
RM
BMA
ATE
HH
HH
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Van Putten & Levinson ApJ 2003
H
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107][
)15.0/(1.0/101][
parameter Small
51
8/341
1
observed
theory
E
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rot
Small GRB-energies
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Durations and GRB-energiesDurations and GRB-energies
0
1
Rotational energy of black hole
Horizon dissipation Black hole output
Torus input Baryon poor outflows
GRBs
tens of seconds
0
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Linearized stability analysis for the torus Linearized stability analysis for the torus
m=2 buckling mode
Free surface waves on inner and outerboundaries mutually interact
(Papaloizou-Pringle 1984)
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Waves in a differentially rotating and incompressible toroidal fluid Waves in a differentially rotating and incompressible toroidal fluid
.0 conditionsboundary enthalpy zero subject to
),(',/,(variable) )2(2 where
)(2)(2
1986) al.et (Goldreichmotion ofequationsEulerLinearized (C)
'frequency corotation and number mode azimuthal of
0,)(
2002)Putten (van onsperturbati alirrotation ible,incompressfor potentialVelocity (B)
]2,23[)(
:criterion) sRayleigh' andKepler (between torusdunperturbean for analysis
stability linearized heconsider t (1984), Pringle-Papaloizou Following (A)
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.0)2()(
1986) al.et (Goldreich 0)(at conditionsBoundary (C)
4/2/,with
),(2
2002)Putten (van in expansion order -Leading (B)
')(
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A free boundary value problem
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Multipole mass-moments in toriMultipole mass-moments in tori
(1986) al.et Goldreich
(1984) Pringle-Papaloizou
0~/ as 3 abqc
Van Putten, 2002
Slenderness ->
]2,23[)(
qr
ar
q
a
US
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Gravitational radiation-reaction force (m=2) Gravitational radiation-reaction force (m=2)
45
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with
)]()/()()/[()/(
so and
becomes EOM in the potential The
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Gravitational radiation-reaction force on quadrupole emissionsGravitational radiation-reaction force on quadrupole emissions
4102
‘
‘
Complex plane of corotation frequency
Increase in imaginary value: backreation promotes instability
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Balance in angular momentum and energy flux
with the constitutive ansatz for dissipation
by turbulent MHD stresses, into thermal emissions and MeV-neutrino emissions
22 )( rAP
Prad
rad
Gravitational radiation in suspended accretion
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~ ~ ~ 42
32rot
diss
rot
w
rot
gw
E
E
E
E
E
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Black hole-beauty: emissions from the torus
Asymptotic results for small slenderness
4e53 erg in gravitational radiation
4e52 erg in torus winds producing SNe
6e52 erg inMeV-neutrinos
torusof radiusmajor -to-minor21
%10/
HT
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Remnants of beautyRemnants of beautyMorphology of GRB-supernova remnant:Morphology of GRB-supernova remnant:
Black hole in a binary with optical companion surrounded by SNRBlack hole in a binary with optical companion surrounded by SNR
Chu, Kim, Points et al., ApJ, 2000
RX J050736-6847.8RX J050736-6847.8
(Candidate GRB-SN remnant)
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Rotational energy of black hole
Horizon dissipation Black hole output
Torus input Baryon poor outflows
Gravitational radiation
Torus winds
Thermal and neutrino emissions
Torus mass loss
GRB3e50erg
SN remnant X-ray emission lines
SN4e51erg
43
2
irradiation of envelope
GWB4e53erg
1e49erg
Calorimetry on active stellar nuclei
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)2( 7
erg1065.3Hz455
2/3
52
mM
MEf Owgw
Observational constraint on gravitational wave-frequency from wind-energy
(scaling value of wind energy corresponds to eta=0.1)
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iaq
coscos)cos(sinsincos
)2sin(cos4
)2cos()cos1(2
00
1
21
t
trh
trh
LT
T
T
0
Phase-modulation of observed radiation by Lense-Thirring precession
Van Putten, Lee, Lee & Kim,2003, in preparation
Line-of-sight
torus
n-torus
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Phase-modulated wave-forms
6/
2/,4/,8/,00
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Stochastic background radiation in gravitational waves
Van Putten, in preparation (2003)
D=100Mpc
h(f)-diagram in matched filtering
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Stochastic background radiation in gravitational waves
Coward, van Putten & Burman 2002Van Putten et al., in preparation (2003)
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Observational opportunities for Adv Observational opportunities for Adv LIGOLIGO
SH
SH
H
D
h
D
h
cs
MM
MM
N
S
BdMSS
N
S
85over averaged 2.1
144over averaged 5.8
Hz104
Hz)500(
Hz104
Hz)500(5.1 4/1
03.011.0
28
57
3/51.0
1
2
1/2-24
2/11
1
1/2-24
2/1
Van Putten (2003), in preparation
12/52/31
1/2-24
2/1
Mpc14071.0Hz104
Hz)500(8
d
M
MS
N
S
Solar
Hh
mf
Matched filtering
Correlating two detectors
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Lower bound on black hole-mass in GRB Lower bound on black hole-mass in GRB 030329030329
Van Putten, Burst Digest (2003), LIGO DCC 030230-00-D
SolarH
Solar
H
mf
h
MM
M
M
N
S
S
25
1)Mpc800/Mpc140(7
201.08
01.0Hz104
Hz)500( :ysensitivit LivingstonCurrent
0.2: torusrotatingrapidly a ofy possibilit theEntertain
2/5
2/3
1
1/2-24
2/1
Spp we use matched filtering and define “no detection”: S/N<1
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ConclusionsConclusionsGRB-SNe from rotating black holes have long durations (gamma0=1e4), small true
GRB-energies (gamma1=1e-4) and an true event rate of 1 per year in D=100Mpc
Durations of tens of seconds correspond to the lifetime of rapid spin of the black hole (gamma0[theory]=gamma0[observation]). Most of black hole spin-energy is dissipated in the event horizon.
GRB-SNe produce 4e53 erg in gravitational radiation via a causal spin-connection between the black hole and a surrounding torus in suspended accretion (gamma2=0.1)
The true GRB-energies represent a small fraction of black hole-spin energy, released through an open tube with finite horizon angle (gamma1[theory]=gamma1[observation])
Matched filtering gives (formally) rise to a current LIGO sensitivity range of 1Mpc, and a (formal) upper bound of 25 Solar masses in GRB 030329
The sensitivity range of Adv LIGO using matched filtering is 100Mpc
Correlation between two detectors may apply to searches for individual events, as well as searches for the contribution of GRB-SNe to the stochastic background radiation in gravitational waves (Omega-B=6e-8)
Opportunity: gravitational radiation from hypernovae: LIGO/VIRGO detections coincident (in position on the sky) with the expected wide-angle optical emissions from an associated supernova and non-coincident with the associated GRB-emissions