GRB Host Galaxies S. R.Kulkarni, E. J. Berger & Caltech GRB group
Radiative transfer and photospheric emission in GRB jets
description
Transcript of Radiative transfer and photospheric emission in GRB jets
Radiative transferRadiative transferand photospheric emissionand photospheric emission
in GRB jetsin GRB jets
Indrek VurmIndrek Vurm((Columbia UniversityColumbia University))
in collaboration within collaboration with
Andrei M. Beloborodov (Columbia University)Andrei M. Beloborodov (Columbia University)Tsvi Piran Tsvi Piran ((Hebrew UniversityHebrew University))
Yuri Lyubarsky Yuri Lyubarsky ((Ben-Gurion UniversityBen-Gurion University))Romain Hascoet (Columbia University)Romain Hascoet (Columbia University)
MoscowMoscow 201 20133
OutlineOutline
Prompt emission: optically thin vs. thickPrompt emission: optically thin vs. thick Photospheric emission from dissipative Photospheric emission from dissipative
jets:jets: Photon number and spectral peaksPhoton number and spectral peaks Non-thermal spectraNon-thermal spectra
GeV emissionGeV emission GeV flash from pair-loaded progenitor windGeV flash from pair-loaded progenitor wind Example: 080916CExample: 080916C
RR00~10~107 7 cmcm
ττTT=1=1L~10L~1051 51 erg/serg/s
ΓΓff
ΓΓss
InternalInternalshocksshocks
PhotosphericPhotosphericemissionemission
heatingheating
GRB prompt emission:GRB prompt emission:optically thin vs. thickoptically thin vs. thick
??
Hardness problemHardness problem
N~F / ~
EFEFEE
EE
Preece et al. Preece et al. ((20002000))
FORBIDDEN
=-2/3=-3/2
coolin
g
death
line
syn
chro
tron
death
line
Optically thin + radiatively Optically thin + radiatively
efficientefficient
> -1.5 (synch. or IC)> -1.5 (synch. or IC)
Peak sharpness and positionPeak sharpness and positionGhisellini (2006)Ghisellini (2006)BlazarsBlazars
Briggs et al. (1999)Briggs et al. (1999)
GRB 990123GRB 990123
GRB spectra narrowGRB spectra narrow
Peak energies clusterPeak energies cluster
EEpkpk
Synch. peakSynch. peak
Goldstein et al. Goldstein et al.
(2012)(2012)
Photospheric emissionPhotospheric emission
Spectral peaksSpectral peaks Narrow: Narrow: cancan be as narrow as be as narrow as
PlanckPlanck PositionPosition
Natural scale Natural scale
Observed Observed
Non-thermal shape:Non-thermal shape:DissipationDissipation
photon productionphoton production
Morsony, Lazzati, Begelman (2007)Morsony, Lazzati, Begelman (2007)
““Disturbed” jetDisturbed” jet
Dissipative jetDissipative jetss
RecollimationRecollimationshocksshocks
Jets could be dissipative Jets could be dissipative throughout their expansionthroughout their expansionRecollimation shocksRecollimation shocksInternal shocksInternal shocksCollisional dissipationCollisional dissipationMagnetic reconnectionMagnetic reconnection
Emerging radiation shaped over Emerging radiation shaped over a broad range of radii, i.e. knows a broad range of radii, i.e. knows about expansion historyabout expansion history
Photon production and Photon production and spectral peaksspectral peaks
RR00
PHOTON PHOTON GENERATIONGENERATION
TT=1=1
EEphph~5 MeV~5 MeV
Observed photons must be produced in the jetObserved photons must be produced in the jet
EEpkpk~500 keV~500 keV
Thermalization/photon- production locationThermalization/photon- production location
Blackbody relationBlackbody relation
ObservationsObservations
ThermalizationThermalization
Photons from the central engine insufficientPhotons from the central engine insufficient
(e.g. Thompson, Meszaros, Rees 2007,(e.g. Thompson, Meszaros, Rees 2007,Pe’er et al. 2007, Eichler & Levinson 2000)Pe’er et al. 2007, Eichler & Levinson 2000)
““Yonetoku”Yonetoku”
- jet launch radius- jet launch radius
FF
hh4kT4kTee
em/absem/abs
ICIC
BBBB
ThermalizationThermalization
absabs=1=1
RR00
TT=1=1
y~10y~10
FF
hh4kT4kTee
em/absem/abs
BBBB
PLANCPLANCKK
WIENWIEN
rrbbbb
FF
hh
BBBB WieWienn
ICIC
em/absem/abs
ThermalizationThermalization
absabs=1=1
RR00
TT=1=1
y~10y~10
FF
hh4kT4kTee
em/absem/abs
BBBB
PLANCPLANCKK
WIENWIEN
rrbbbb
Neither Neither TT»1 nor y»1 are sufficient conditions for »1 nor y»1 are sufficient conditions for thermalizationthermalization
TT~10~1022
Photon sourcesPhoton sources
Non-magnetized flows:Non-magnetized flows: BremsstrahlungBremsstrahlung Double-Compton Double-Compton
scatteringscattering Magnetized flowsMagnetized flows
CyclotronCyclotron
Synchrotron Synchrotron
- thermal- thermal
NNee(())
3kT3kTeenthnth
Photon production: summaryPhoton production: summary
RR00
TT=1=1
~10~1010101010 cm cm
10101212 cm cm
synchrotronsynchrotronbremsstrahlungbremsstrahlung
double Comptondouble Compton
cyclotroncyclotron
TT~10~1022
TT~10~1044
y~10y~1033
y~10y~10
rrWienWien
Photon production occurs in a limited range of radii, at Photon production occurs in a limited range of radii, at TT»1»1
Observed EObserved Epkpk -s -s modest modest ~10 at r~10~10 at r~101111 cm cm
Most efficient mechanism: synchrotronMost efficient mechanism: synchrotron
Number of photons at the peak established below/near the Wien radiusNumber of photons at the peak established below/near the Wien radius
PLANCPLANCKK
WIENWIEN
Spectral shapeSpectral shape
Spectrum broadened by:Spectrum broadened by: Large-angle emissionLarge-angle emission `Fuzzy` photosphere`Fuzzy` photosphere Diffusion in frequency space Diffusion in frequency space
Photospheric emission from a dissipative jetPhotospheric emission from a dissipative jetdoes NOT resemble a Planck spectrum does NOT resemble a Planck spectrum
Low-energy slope: dissipative Low-energy slope: dissipative
jetjet
PLANCPLANCKK
WIENWIEN
DISSIPATIONDISSIPATION
ττTT==
11
Low-energy spectrum is shaped in an extended Low-energy spectrum is shaped in an extended
region between the Wien radius and the Thomson region between the Wien radius and the Thomson
photospherephotosphere
FF
FF
y~1y~1
Low-energy slope: dissipative jetLow-energy slope: dissipative jet
2 F
Wien/Planck spectrum at y»1Wien/Planck spectrum at y»1is broadened by the combinedis broadened by the combinedeffect of Comptonizationeffect of Comptonizationand adiabatic coolingand adiabatic cooling
Photospheric spectrumPhotospheric spectrumsubstantially softer than Plancksubstantially softer than Planck
ττTT=1=1
WIENWIEN
DISSIPATIONDISSIPATION
y~1y~1
Low-energy slope: dissipative Low-energy slope: dissipative jet; with a soft photon sourcejet; with a soft photon source
photon injectionphoton injection
αα=-1 slope is a slow =-1 slope is a slow attractorattractor
saturated Comptonizationsaturated Comptonization
9.0
Dissipative jet: high-energy Dissipative jet: high-energy spectrumspectrum
Non-thermal spectrum above the peak: dissipation near Non-thermal spectrum above the peak: dissipation near ττTT~~11
Possible mechanism: collisional heating (Beloborodov Possible mechanism: collisional heating (Beloborodov 2010)2010) Proton and neutron flows decouple at Proton and neutron flows decouple at TT2020
Drifting neutron and proton flows Drifting neutron and proton flows nuclear collisions:nuclear collisions: Elastic: Thermal heating of eElastic: Thermal heating of e±± via Coulomb collisions via Coulomb collisions
Inelastic: Injection of relativistic eInelastic: Injection of relativistic e± ± with with ~300~300via pion production and decayvia pion production and decay Other models:Other models:
Thompson (1994)Thompson (1994)Pe’er, MPe’er, Méészszááros & Rees ros & Rees
(2005)(2005)Giannios & Spruit (2006)Giannios & Spruit (2006)Ioka et al. (2007)Ioka et al. (2007)etc.etc.
0,, MeV1402 cm
0;;
ee ee ;
Spectra: non-magnetized flowsSpectra: non-magnetized flows
ThermalThermalComptonCompton
Non-thermalNon-thermalComptonCompton γγγγ - absorption - absorption
GeVMeV
kT=15 keV
Heating-cooling balance
injection
cooling,pair cascades
2 EEL PairsPairs
Dissipative jet: summaryDissipative jet: summary
FF
hh4kT4kTee
WienWien
RR00
PH. PH. GENERATIONGENERATION
TT=1=1
~10~10
SPECTRUM FORMATIONSPECTRUM FORMATION
TT~10~1022
y~10y~10
DISSIPATIONDISSIPATION
rrWienWien
FF
hhEEpkpk
FF
hhEEpkpk
Generic model for a dissipative jetGeneric model for a dissipative jet
ττTT=1=1rrcollcoll
WIENWIEN
(r(rcollcoll)~1)~1
00
Continuous dissipationContinuous dissipationthroughout the jetthroughout the jet Thermal and non-thermalThermal and non-thermal
channels:channels:
Acceleration:Acceleration:
Magnetization:Magnetization: Initial radius rInitial radius rcollcoll=10=101111 cm cm
DISSIPATIONDISSIPATIONACCELERATION
ACCELERATION
- terminal Lorentz factor- terminal Lorentz factor
Radiative transferRadiative transfer
- intensity- intensity - photon angle- photon angle
Processes: Compton, Processes: Compton, synchrotron, synchrotron,
pair-production/annihilationpair-production/annihilation
Spectral formationSpectral formation
Spectra at different stages of expansionSpectra at different stages of expansion
rrcollcoll=10=101111
cmcm
TT(r(rcollcoll)=40)=40
00
(r(rcollcoll)~50)~50
=300=300
Initial spectrum: WienInitial spectrum: Wien
Peak shifted to lower energiesPeak shifted to lower energies
due to photon productiondue to photon production
Broadening starts nearBroadening starts near
the Wien radius, proceedsthe Wien radius, proceeds
through the photospherethrough the photosphere
Final spectrum: BandFinal spectrum: Band
rrWienWien
ττTT=1=1rrcollcoll
WIENWIEN
Parameters:Parameters:
Spectra: varying LF at the base Spectra: varying LF at the base
ττTT=1=1rrcollcoll
WIENWIEN
(r(rcollcoll))
rrcollcoll=1=1001111
cmcm Canonical Band shapeCanonical Band shape
Low-energy slope stays near Low-energy slope stays near 11
Spectral peak sensitive to Spectral peak sensitive to (r(rcollcoll))
via photon production efficiencyvia photon production efficiency
BB= 10= 10-2-2
Photospheric emission typically NOT thermal-lookingPhotospheric emission typically NOT thermal-looking
Dissipative jetsDissipative jets Naturally lead to Band-like spectraNaturally lead to Band-like spectra
Photon index Photon index =-1 is an attractor for the Comptonization =-1 is an attractor for the Comptonization
problemproblem
Typical ETypical Epkpk -s require -s require
efficient dissipation efficient dissipation at r~10at r~101111 cm. Recollimation shocks? cm. Recollimation shocks?
bulk Lorentz factor bulk Lorentz factor ~10 at the same radii~10 at the same radii
At least moderate magnetization At least moderate magnetization BB>>1010-3-3
SummarySummary
Continuous dissipation throughout the jet?Continuous dissipation throughout the jet?
GeV flashesGeV flashes
withwith
Andrei Beloborodov and Romain HascoetAndrei Beloborodov and Romain Hascoet
Observations: GRB 080916CObservations: GRB 080916C
Fermi collaboration (2013)Fermi collaboration (2013)
LATLAT
GBMGBM
GRB 080916CGRB 080916C
Observations: LAT lightcurvesObservations: LAT lightcurves
080916C080916C
090902B090902B090926A090926A
TT95 95 (GBM)(GBM)
Fermi LAT collaboration Fermi LAT collaboration
(2013)(2013)
‘‘Regular’ behaviour: Regular’ behaviour: external origin external origin ((forward shock)?forward shock)?
LAT emission peaks LAT emission peaks duringduring the prompt: the prompt: likely not assoc. with decelerationlikely not assoc. with deceleration
Lasts well beyond TLasts well beyond T9595
Emission mechanismEmission mechanism
Synchrotron?Synchrotron?
Theoretical limit: a few 10 MeV (comoving)Theoretical limit: a few 10 MeV (comoving) ~ 10 GeV (observed); limit tighter at late times ~ 10 GeV (observed); limit tighter at late times
Observed: 95 GeV (GRB 130427A) Observed: 95 GeV (GRB 130427A)
Inverse ComptonInverse Compton GeV peak during prompt GeV peak during prompt intense IC cooling by prompt intense IC cooling by prompt
radiationradiation
e.g. Nakar & Piran (2010)e.g. Nakar & Piran (2010)
Kumar & Barniol Duran (2009)Kumar & Barniol Duran (2009)
Asano et al. (2009)Asano et al. (2009)
Razzaque et al. (2010)Razzaque et al. (2010)
Ghisellini (2010)Ghisellini (2010)
Number of IC photonsNumber of IC photons
Wind velocityWind velocity
Bright GeV flashes:Bright GeV flashes:
No. of emitted IC photons:No. of emitted IC photons:
Photon multiplicityPhoton multiplicity
Required pair multiplicity:Required pair multiplicity:
Proposed mechanism: inverse Compton Proposed mechanism: inverse Compton
scattering of prompt MeV radiation in the scattering of prompt MeV radiation in the
forward shockforward shock
in a pair-enriched external mediumin a pair-enriched external medium
PROMPT RADIATIONPROMPT RADIATION
Forward shockForward shock
GeGeVV
EXTERNAEXTERNAL L MEDIUMMEDIUM
Prompt radiation pair-loads and pre-accelerates Prompt radiation pair-loads and pre-accelerates the ambient medium ahead of the FSthe ambient medium ahead of the FS
Pair-enrichment of the external Pair-enrichment of the external mediummedium
PROMPT RADIATIONPROMPT RADIATION
FSFS
1. ISM particle scatters a prompt photon1. ISM particle scatters a prompt photon
2. Scattered photon pair-produces with another prompt photon2. Scattered photon pair-produces with another prompt photon
3. New pairs scatter further photons etc.3. New pairs scatter further photons etc.
e-
e± e-
Loading and pre-acceleration controlled by Loading and pre-acceleration controlled by
the column density of prompt radiationthe column density of prompt radiation
ZZ±±,,prepre
e.g Thompson & Madau (2000) e.g Thompson & Madau (2000)
Beloborodov (2002)Beloborodov (2002)
Kumar & Panaitescu (2004)Kumar & Panaitescu (2004)
GRB 080916C:GRB 080916C:pair-loading and pre-accelerationpair-loading and pre-acceleration
Pair loading at the forward shockPair loading at the forward shock Pre-acceleration and blastwave Lorentz factorsPre-acceleration and blastwave Lorentz factors
Beloborodov, Hascoet, IV (2013)Beloborodov, Hascoet, IV (2013)
GRB 080916C:GRB 080916C:thermal injection Lorentz factorthermal injection Lorentz factor
Flash peaks when:Flash peaks when:
Early decay due to fast Early decay due to fast evolution of evolution of injinj and Z and Z±±
- pair loading- pair loading
Thermal heating:Thermal heating:
GRB 080916C: lightcurveGRB 080916C: lightcurve
Delayed riseDelayed rise Peak during the Peak during the
promptprompt Persists well after TPersists well after T9595
T95 (GBM)
Flux above 100 MeV Flux above 100 MeV
Wind parameterWind parameter
Peak radius RPeak radius R10101616 cm cm
Non-thermal acceleration NOT requiredNon-thermal acceleration NOT required
GRB 080916C: spectraGRB 080916C: spectra
Fermi LAT collaboration Fermi LAT collaboration
(2013)(2013)
-2
-2
SpectraSpectra LAT photon indexLAT photon index
SummarySummary
Proposed mechanism: GeV flashes from FS Proposed mechanism: GeV flashes from FS
running into pair-loaded external mediumrunning into pair-loaded external medium Radiative mechanism: IC of prompt MeV Radiative mechanism: IC of prompt MeV
photonsphotons Standard wind medium consistent with Standard wind medium consistent with
observationsobservations