Close Binary Progenitors Of Gamma Ray Bursts And GRB...
Transcript of Close Binary Progenitors Of Gamma Ray Bursts And GRB...
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Maxim BarkovABBL RIKEN
Serguei KomissarovUniversity of Leeds, UK
Close Binary Progenitors Of Gamma Ray Bursts
And GRB Extended Emission
1GRB-Workshop, RIKEN9/1/2015
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Plan of this talk
•Models of Central Engines,• Magnetic Unloading,• Realistic initial conditions,• Numerical simulations II: Collapsar model,• Common Envelop and X-Ray flares, • Extended emission of short GRBs,• Conclusions
2GRB-Workshop, RIKEN9/1/2015
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II. Relativistic jet/pancake model of GRBs and afterglows:
jet at birth(we are here) pancake later
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Merge of compact stars – origin of short duration GRBs?
Neutron star + Neutron starNeutron star + Black holeWhite dwarf + Black hole
Black hole + compact disk
Blinnikov (1984),Paczynsky (1986);Goodman (1986);Eichler et al.(1989);
Burst duration: 0.1s – 1.0s
Released binding energy:
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01/09/2015
Fast Rotating Neutron Star as Hypernova engine:
Rotationalenergy:
Wind Power:
Gamma-Ray-Repeaters and Anomalous X-ray pulsars - isolated neutron stars with dipolar(?) magnetic field of 1014- 1015 G (magnetars); (Woods & Thompson, 2004)
Usov(1992), Thompson(1994), Thompson(2005), Bucciantini et al.(2006,2007,2008), Komissarov & Barkov (2007), Barkov & Komissarov (2011)
(i) ultra-relativistic(ii) non-relativistic
01/09/2015 5GRB-Workshop, RIKEN 5
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Collapsars– origin of long duration GRBs?
Woosley (1993)MacFadyen & Woosley (1999)
Iron core collapses into a black hole: “failed supernova”. Rotating envelope
forms hyper-accreting disk
Collapsing envelope
Accretion shock
Accretion disk
The disk is fed by collapsing envelope.
Burst duration > a few seconds6GRB-Workshop, RIKEN9/1/2015
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Mechanisms for tapping the disk energy
BB
Neutrino heating Magnetic braking
fireballMHD wind
Eichler et al.(1989), MacFadyen&Woosley (1999), Aloy et al.(2000) Nagataki et al.(2006), Birkl et al (2007)Zalamea & Beloborodov (2008,2011)
Blandford & Payne (1982)Proga et al. (2003)Fujimoto et al.(2006)Mizuno et al.(2004)
7GRB-Workshop, RIKEN
9/1/2015
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GRB-Workshop, RIKEN 89/1/2015
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Setup
v
B
v
B
v
v
v
(Barkov & Komissarov 2008a,b)(Komissarov & Barkov 2009)black hole
M=3Msuna=0.9
Uniform magnetization R=4500km
Y= 4x1027-4x1028Gcm-2
outer boundary, R= 2.5x104 km
free fallaccretion
(Bethe 1990)
• 2D axisymmetricGRMHD;
• Kerr-Schild metric;• Realistic EOS;• Neutrino cooling;• Starts at 1s from
collapse onset. Lasts for < 1s
Rotation:
rc=6.3x103kml0 = 1017 cm2 s-1
230 1,/minsin crrll
Numerical simulations
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magnetic field lines, and velocity vectors
unit length=4.5kmt=0.24s
Model:AC1=9; Bp=3x1010 G
log10 (g/cm3) log10 P/Pm log10 B/Bp
10GRB-Workshop, RIKEN9/1/2015
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magnetic field lines, and velocity vectors
unit length=4.5kmt=0.31s
Model:AC1=9; Bp=3x1010 G
log10 (g/cm3)
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Model:AC1=9; Bp=3x1010 G
log10 (g/cm3)
magnetic field lines
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)(log10
m
gP
P10log
GB
CsMM SUN
101
1
103.0
315.0
�
9.010 1217
0
ascml
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Jets are powered mainly by the black hole via the Blandford-Znajek mechanism !!
• No explosion if a=0; • Jets originate from
the black hole;• ~90% of total magnetic flux
is accumulated by the black hole;• Energy flux in the ouflow ~
energy flux through the horizon (disk contribution < 10%);
• Theoretical BZ power:
15123
227
50 1048.0106.3 Y sergMafEBZ�
Model: C
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Magnetic Unloading
(???)1/ 2 cMEBZ��
22
227
50106.3 Y MafEBZ�
22
2
11 a
aaf
What is the condition for activation of the BZ-mechanism ?
1) MHD waves must be able to escape from the black hole ergosphereto infinity for the BZ-mechanism to operate, otherwise accretion is expected.
or
2) The torque of magnetic lines from BH should be sufficient to stop accretion (Barkov & Komissarov 2008b)(Komissarov & Barkov 2009)
15GRB-Workshop, RIKEN9/1/2015
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The disk accretion relaxes the explosion conditions. The MF lines’ shape reduces the local accretion rate.
10/1/ 2 cMEBZ��
16GRB-Workshop, RIKEN9/1/2015
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9/1/2015 GRB-Workshop, RIKEN 17
Neutrino heating vs Magnetic jets
Zalamea & Beloborodov (2011)
𝐸𝐵𝑍 = 𝐶(𝑎)𝛽 𝑚𝑐2
Komissarov & BMV (2011)
Magnetically driven jets can last much longer compare to neutrinoheating jets.
22
2
11 a
aaf
𝐶 𝑎 = 2 ∗ 1054𝑓(𝑎) ergs/s
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Discussion
Magnetically-driven stellar explosions require combination of (i) fast rotation of stellar cores and (ii) strong magnetic fields.
Can this be achieved?• Evolutionary models of solitary massive stars show that even much weaker magnetic fields (Taylor-Spruit dynamo) result in rotation being too slow for the collapsar model (Heger et al. 2005)
• Low metallicity may save the collapsar model with neutrino mechanism (Woosley & Heger 2006) but magnetic mechanism needs much strongermagnetic field.
• Solitary magnetic stars (Ap and WD) are slow rotators (solid body rotation).
•We need strongly magnetized star in close binary system!18GRB-Workshop, RIKEN9/1/2015
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BH
starR
)(rl
If l(r)<lcr then matter falling to BH directly
If l(r)>lcr then matter goes to disk and after that to BH
Agreement with model Shibata&Shapiro (2002) on level 1%
Simple model:
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Barkov & Komissarov (2010)
9/1/2015
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Power low density distribution model
3 r
20GRB-Workshop, RIKEN
2s
s
GMcJJ
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Realistic model
M=35 Msun, MWR=13 Msun
Heger at el (2004)
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Realistic model
M=35 Msun, MWR=13 MsunM=20 Msun, MWR=7 Msun
neutrino limit
BZ limit
Realistic model Heger at el (2004)
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Uniform magnetization R=150000km
B0= 1.4x107-8x107G
vB
v
B
v
v
v
Numerical simulations II: Collapsar model
GR MHD2D
black holeM=10 Msun
a=0.45-0.6
Setup
Bethe’s free fall model,T=17 s, C1=23
Initially solid body rotation
Dipolar magnetic field
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Barkov & Komissarov (2010)
9/1/2015
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GRB-Workshop, RIKEN 24
In some cases (30%) one side jets are formed.
9/1/2015
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9/1/2015 GRB-Workshop, RIKEN
2 Side jets 1 Side jet
25
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a=0.6 Ψ=3x1028 a=0.45 Ψ=6x1028
Model a Ψ28 B0,7 L51 dMBH /dt ηA 0.6 1 1.4 - - -B 0.6 3 4.2 0.44 0.017 0.0144C 0.45 6 8.4 1.04 0.012 0.049
152
1010
170
skm
MM
ergsEV
bh
sunkick
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9/1/2015 GRB-Workshop, RIKEN 27
Neutrino heating vs Magnetic jets
Zalamea & Beloborodov (2011)
𝐸𝐵𝑍 = 𝐶(𝑎)𝛽 𝑚𝑐2
Komissarov & BMV (2011)
Magnetically driven jets can last much longer compare to neutrinoheating jets.
22
2
11 a
aaf
𝐶 𝑎 = 2 ∗ 1054𝑓(𝑎) ergs/s
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Normal WRSAnd
Black Hole
black hole spiralling
jets produced
MBH left behind
few seconds
< 1000 seconds
5000 seconds
28
disk formed
Common Envelop (CE):
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log10F x(0.
3 –10k
eV)
log10(t/sec)2 3 4 51
0
1
2 3
4
“Canonical” X-ray afterglow lightcurve (Swift)
Zhang (2007)
5
• During CE stage a lot of angular momentum is transferred to the envelop of normal star.
• Accretion of the stellar core can give the main gamma ray burst driven by neutrino heating.
• BZ could work effectively much longer with low accretion rates.
• Long accretion disk phase could be as long as 104 s, i.e. a feasible explanation for X-Ray plateau phase.
see for review(Taam & Sandquist 2000)
st
sMtM
MM
d
sunsun
8000
110
4.1 1
�
29
(Barkov & Komissarov 2010)
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9/1/2015 30
Short GRBs have extended Emission up to 100 s.
We suggest a two componentJet model.
BMV & Pozanenko 2011
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Conclusions
+ Black holes of failed supernovae can drive very powerful GRB jets via Blandford-Znajek mechanism if the progenitor star has strong poloidal magnetic field;
+ Blandford-Znajek mechanism of GRB has much lower limit on accretion rate to BH then neutrino driven one (excellent for very long GRBs >100s);
+ One side jet can be formed (kick velocity order of V=200 km/s).
• The Collapsar is a promising model for the central engine of long GRBs.• Theoretical models are sketchy and numerical simulations are only now
beginning to explore them. • Our results suggest that:
All Collapsar and NS based models need high angular momentum, the common envelop stage could help.
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Neutrino driven jet and magnetically driven jet can be in operation in the same event. Magnetically driven jet can be feasible explanation for extended emission.
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9/1/2015 GRB-Workshop, RIKEN 32
Beskin 2010
Unipolar inductor
𝑊𝑡𝑜𝑡 ∝ 𝑓(𝑎) Ψ2𝑀𝐵𝐻−2
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Red GiantAnd
Neutron Star
Neutron star spiralling
jets produced, SNIIn
MBH left behind
few seconds
< 1000 seconds
5000 seconds
33
NS recycled,Field generated
NS in Common Envelop:
GRB-Workshop, RIKEN
NS + WR
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The accretion to NS: the sensitivity to parameters.
34GRB-Workshop, RIKEN
Chevalier (1996)
Barkov & Komissarov (2011)
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The NS penetration to the envelop of RG
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Chevalier (1996)
De Marco et al (2011)
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GRB-Workshop, RIKEN 36
NS with dipole field:
P=4 ms
𝐿 = 3.7 × 1049 erg/sB=1015 G
The intensive accretion to NS of matter with accretion rate of 103
Msun/yr can lead to the generation of strong magnetic field.
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37GRB-Workshop, RIKEN
The complex topology of the NS magnetic field can lead to asymmetric explosion. Here is presented the explosion driven by NS with magnetosphere containing both dipole and quadruple harmonics (see also Lovelace et al. 2010)
Energy flux depends on polar angle
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38GRB-Workshop, RIKEN
The NS activity after the explosion:
1 year after the beginning of the explosion we expect TeV and GeVphotons with total luminosity of 1040 erg/s
Such an emission can be detected at distances about 10 Mpc.
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9/1/2015 GRB-Workshop, RIKEN 39
Neutrino heating
Harikae et al 2010
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Free fall model of collapsing star (Bethe, 1990)
radial velocity:
mass density:
accretion rate:
Gravity: gravitational field of Black Hole only (Kerr metric); no self-gravity;
Microphysics: neutrino cooling ;realistic equation of state, (HELM, Timmes & Swesty, 2000);dissociation of nuclei (Ardeljan et al., 2005);Ideal Relativistic MHD - no physical resistivity (only numerical);
12/11
1 1011.0
sM
MM
stCM sun
sun
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40GRB-Workshop, RIKEN9/1/2015
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GRBs Jet magnetic acceleration:
•We get MHD acceleration of relativistic jet up to ≈300•Conversion of magnetic energy to kinetic one more than 50%•Acceleration have place on long distance req≈2rlc•The main part of the jet is very narrow θ<2(Komissarov et al 2009)
01/09/2015 41GRB-Workshop, RIKEN
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• Jets are formed when BH accumulates sufficient magnetic flux.• Jets power• Total energy of BH • Expected burst duration (?)• Jet advance speed • Expected jet break out time • Jet flow speed (method limitation) • Jets are powered by the Blandford-Znajek mechanism
Summary:
Good news for the collapsar model of long duration GRBs !
15110134.0 serg
cVs 5.01.0
42GRB-Workshop, RIKEN9/1/2015