Shocks in Gamma-Ray Bursts - Girichidisgirichidis.com/shocks2018/talks/shocks2018-Nava.pdf · Kumar...
Transcript of Shocks in Gamma-Ray Bursts - Girichidisgirichidis.com/shocks2018/talks/shocks2018-Nava.pdf · Kumar...
![Page 1: Shocks in Gamma-Ray Bursts - Girichidisgirichidis.com/shocks2018/talks/shocks2018-Nava.pdf · Kumar &Barniol Duran 2009, 2010; Gao et al. 2009; ! Corsi, Guetta & Piro 2010; De Pasquale](https://reader036.fdocuments.net/reader036/viewer/2022081614/5fd0f504d1546910d149de6c/html5/thumbnails/1.jpg)
Shocks in!Gamma-Ray Bursts:!
from theory to observations Lara Nava!
Marie Skłodowska-Curie Fe$ow! !
INAF - OABrera!INAF - OATrieste
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GRBs: the standard model
PROMPT
or magnetic
reconnection ???
Rdiss=1013-1014cm
Rdiss=1015-1016cm
AFTERGLOW
Rdiss=1016-1017cm
PROMPTAFTERGLOW
Shocks take place in two different sites
•10 keV- 10 MeV!!
•< 1s to 103 s!!
•non-thermal ! spectra
• softX, OT, radio!!
• weeks, months!!• flux PL decay in ! time
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!’
Prompt !— internal shocks —!
mildly relativistic
electrons magnetic field
γ
N(γ)
γmin
-p
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PROMPT spectra:!synchrotron theory vs observations
�c �m �
F� �
4/31/2 -(p-2)/2
Typical prompt spectrumTheoretical synchro spectrum
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PROMPT spectra:!synchrotron theory vs observations
�c �m �
F� �
4/31/2 -(p-2)/2
Typical prompt spectrumTheoretical synchro spectruminformation on !
the electron spectrum
depends on !B, Lk, εe, ξe
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�m �
F� �
+1
Black: typical observed !prompt spectrum
Colours: predicted !synchrotron spectrum!
Inconsistency!!Observed spectra!
are harder than predicted
4/31/2
-(p-2)/2
�c
PROMPT spectra:!synchrotron theory vs observations
![Page 7: Shocks in Gamma-Ray Bursts - Girichidisgirichidis.com/shocks2018/talks/shocks2018-Nava.pdf · Kumar &Barniol Duran 2009, 2010; Gao et al. 2009; ! Corsi, Guetta & Piro 2010; De Pasquale](https://reader036.fdocuments.net/reader036/viewer/2022081614/5fd0f504d1546910d149de6c/html5/thumbnails/7.jpg)
Prompt emission !Light curves
Oganesyan, Nava, Ghirlanda, Celotti, 2017, ApJ
red = XRT 0.3 -10 keV!green = BAT 15 - 150 keV
Oganesyan, Nava, Ghirlanda, Celotti, submitted
![Page 8: Shocks in Gamma-Ray Bursts - Girichidisgirichidis.com/shocks2018/talks/shocks2018-Nava.pdf · Kumar &Barniol Duran 2009, 2010; Gao et al. 2009; ! Corsi, Guetta & Piro 2010; De Pasquale](https://reader036.fdocuments.net/reader036/viewer/2022081614/5fd0f504d1546910d149de6c/html5/thumbnails/8.jpg)
Comparison !between observed spectral shape and synchrotron spectrum
4/31/2 -(p-2)/2
�c �m �
F� �
Ebreak Epeak
α1
βα2
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Spectral breaks in Fermi bursts?!GRB 160625BRavasio,…LN et al., 2018, in press
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GBM GRB 160625B !results from time-resolved analysis
Spectral indices
¡3:5¡3:0¡2:5¡2:0¡1:5¡1:0¡0:5
Index
0
1
2
3
4
5
6
7
8
9
N
®1
®2
¯
®syn1=¡0:67
®syn2=¡1:5
¡3:5 ¡3:0 ¡2:5 ¡2:0 ¡1:5 ¡1:0 ¡0:5
Index
0
1
2
3
4
5
6
7
8
9
N
®1
®2
¯
®syn1 = ¡0:67
®syn2 = ¡1:5
1.5 1 0.5 0 -0.5 -2 -3
- - - - Synchrotron predictions
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Are we observing synchrotron radiation in marginally fast cooling regime?
4/31/2 -(p-2)/2
�c �m �
F� �
1
Theoretical models !marginally fast cooling:!
�c~�mDerishev 2007!Kumar & McMahon 2008!Daigne et al. 2011!Beniamini & Piran 2013,2014!Uhm & Zhang 2014
Implications: small B’~10 Glarge Γ > 500 large γmin > 104-5
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!
Afterglow !— external shocks —!
ultra-relativistic
electrons magnetic field
γ
N(γ)
γmin
-p
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!’ !
Prompt !— internal shocks —!
mildly relativistic
Afterglow !— external shocks —!
ultra-relativistic
B’ ~ 20 G!γe ~ 104B’ ~ 104 G!
γe ~ 400
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Afterglow !observations/modeling
Six (seven) free parameters in the model! εe, εB, (ξe), p, Ek, n = n0 R-s!
non simultaneous observations at different ν!radio observations available only for a small sample and at late time!observed features not included in the model (bumps, plateaus, flares,…)!
some of the parameters are fixed to what is believed is their typical value
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Six (seven) free parameters in the model! εe = 0.1, εB= 0.01 (ξe) p =2.3, Ek (from prompt), n=n0 R-s!
non simultaneous observations at different ν!radio observations available only for a small sample and at late time!observed features not included in the model (bumps, plateaus, flares,…)!
some of the parameters are fixed to what is believed is their typical value
Afterglow !observations/modeling
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same origin as the X-ray and Optical afterglow:!-- External Shocks --
Kumar &Barniol Duran 2009, 2010; Gao et al. 2009; !Corsi, Guetta & Piro 2010; De Pasquale et al. 2010
Ghisellini, Ghirlanda, Nava & Celotti 2010 — Ghirlanda, Ghisellini & Nava 2010
GeV AFTERGLOW!around 50 GRBs with GeV long lasting
emission
Fermi-LAT!0.1 - 10 GeV
optical !afterglow
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"i "c
SSC suppressed
"i "c
Slow Cooling
Density
uppe
r lim
its to
# B
Upper limits on εB!always smaller that the canonical value εB=10-1-10-2!
(Kumar & Barniol Duran 2009, Lemoine 2013a/b — Santana et al., 2014)
X-ray X-rayGeV GeV
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ConclusionsSmall B…? What is the value of B relevant for particle cooling?!
Maximum energy of accelerated electrons?!
Efficiency of the acceleration mechanism (= fraction of particles injected in the acceleration process)?
FutureSKA: radio observations at late time, when fireball isotropic, give direct estimate of the true energy!
CTA: cutoff in the afterglow synchrotron spectrum (=maximal energy of accelerated particles)? Inverse Compton component?