1. Gamma-Ray Bursts (GRBs) and collisionless shocks Ehud Nakar Krakow Oct. 6, 2008

2. NASA web site Gamma-Ray Bursts Flash of  -rays that last several seconds – the prompt emission Fox et. al., 05 long lasting decaying radio- optical-X-ray emission – the afterglow NASA

3. Longs & shorts Kouveliotou et al. 1993 Long GRBs collapse of a massive star Short GRBs Unknown – possibly NS-NS or BH-NS coalescence ?

4. Prompt emission - observations (long GRBs) uDuration 1-1000s u10 52 -10 54 erg (isotropic equivalent) 10 50 -10 52 erg/s (isotropic equivalent) u~0.01-2 MeV photons Non-thermal spectrum; very high energy tail (at least up to GeV) uRapid variability (less than 10ms)

5. Relativistic Wind (p-e - or p-e + -e - or EM) Prompt emission in the fireball model Internal dissipation  -rays 10 13 -10 16 cm Inner Engine 10 6 cm  >100

6. Prompt emission - theory (long GRBs) The emission source is internal dissipation within a relativistic outflow,  >100! Radiation process – Unknown Leading candidates are synchrotron and IC Outflow composition and magnetization – Unknown Unmagentized pair plasma is unlikely Collisionless shocks ? – only if the outflow is baryonic  mildly relativistic internal shocks

7. Afterglow - Observations Peaks in X-ray first (minutes-hour), then in optical (hours-days) and finally in radio (days-years) Temporal & spectral structure: Broken power law Stanek et al. 99 F t (days) Galama et al. 99 B, V, R, I

8. Relativistic Wind (p-e - or p-e + -e - or EM) The internal-external fireball model Internal dissipation  -rays 10 13 -10 16 cm Inner Engine 10 6 cm External Shock Afterglow 10 16 -10 18 cm

9. External shock afterglow model Hydrodynamics: A relativistic blast-wave that propagates into a perfect fluid (shocked fluid energy concentrated in –  R ~ R/  2 ) Blast wave decelerates while shoveling mass -  R -3/2 (for a constant external density). The burst emission ionize and destruct dust in the circum-burst medium  upstream is ionized, unmagnetized, p-e plasma.  Shocked plasma pressure upstream pressure pressure R  

10. Radiation modeling: Shock crossing  electron acceleration N(  )   -p for  >  m  e - fraction of electrons energy out of the internal energy at the shock crossing  B - fraction magnetic field energy out of the internal energy at any time  synchrotron + Synchrotron Self-Compton radiation The model fit for five free parameters: E k, n, p,  e and  B

11. The basic (slow cooling) Synchrotron Afterglow Spectrum and its time evolution: Low energy F  -1/3 Synch self Absorption t -1/2 t -3/2 t0t0 Sari et al 1998 High Energy F  -p/2 F Galama et al. 99 Model Observations

12. The typical parameters that fit the data  e ~ 0.1  B ~ 0.01-0.001 p = 2-2.7 E k,iso = 10 52 -10 54 erg (Comparable to E  iso  n ~ 0.01-10 cm -3 (expected in ISM)

13. Typical scales shock Lorentz factor -  ~100 @ t=100s  ~10 @ t=1 day  ~2 @ t=1 month (t – observer time since the burst) B Downstream B d ~ mG-G B Upstream B u ~  G (  B,up ~10 -9 ) Width of shocked plasma ~10 12 cm @ t=100s ~10 16 cm @ t=1week Skin depth ~10 7 cm

14. Main microphysical assumptions in the basic model: The shock is thin compared to the emitting region. Electrons are coupled to the protons just through the shock. All Electrons are accelerated – relaxing this assumption can change the best fit parameters by a factor f<m p /m e (Eichler & Waxman 05)  e and  B are constant in time and space –  B cannot drop significantly far in the downstream (Rossi & Rees 02)

15. Afterglow observations strongly suggest that weakly magnetized relativistic collisionless shocks: Generate magnetic field with ~10 -4 -10 -2 of equipartition. This magnetic field survives long after crossing the shock (>10 7 skin depths). Polarization indicate that the magnetic field is anisotropic on large scales with ratio ~2:1 Efficiently accelerate electrons (in equipartitoin with protons energy) at least up to TeV Note: External shock is the most popular and successful afterglow model. But, it is not the only model and it cannot explain all afterglow observations in all bursts.

16. Short GRBs Prompt emission is similar to long GRBs About dozen observed afterglows (mostly in X-ray) suggest a similar mechanism and physical properties as in long GRB afterglows The progenitor is an old stellar system and therefore the expected circum burst medium is the interstellar medium – unaffected by massive stellar wind. The ability of collisionless shocks to generate field an accelerate particles is not unique to upstream which is shaped by stellar wind (e.g., with high density clumps) Nakar 07

17. Magnetic field generation in GRB external shocks Equipartion field on a skin depth scale is thought to be generated in unmagnetized shocks by the Weibel instability (Moiseev & Sagdeev 63; Kazimura et al 98; Medvedev & Loeb 99, …) But … without sustaining process it is expected to decay over a similar scale (Gruzinov 01; Chang et al., 08) How can the shock generate strong magnetic field that survives over ~10 9 skin depths?

18. Suggested processes: Interaction of the thermal plasma (upstream and/or downstream) with accelerated particles via kinetic instabilities (e.g., recent numerical results by Keshet et al. 08 and Spitkovsky 08) Amplification of the downstream field via downstream vorticity generated by Density inhomogeneity in the upstream (e.g., Sironi & Goodman 07) Angular energy anisotropy of decelerating blast wave (Milosavljevic, Nakar & Zhang 07) Interaction between streaming protons and the upstream plasma via nonresonant streaming instability (e.g., Bell 2004, Milosavljevic & Nakar 06, Reville et al 06, …)

19. Generation of upstream density inhomogeneies by streaming protons (Couch, Milosavljevic & Nakar 2008) assumption: protons are accelerated in the shock by Fermi process ` shock frame ~R/  e p upstream IC cooling grantee that if protons are accelerated to  p >10 3 then protons stream farther upstream then electrons Upstream frame ~R/   e p upstream p 

20. Nonresonant streaming instability amplifies the magnetic field and produces density inhomogeneities (e.g., Bell 04) Even if the field is not amplified by orders of magnitude (e.g., Pelletier et al 08), density contrast of order unity is generated. Such contrast is enough in order to amplify the downstream field to the observed levels by generating downstream vorticity. In GRB external shocks there is enough time to generate order unity density contrast even if the seed field is the pre-existing  G field

21. Summary GRB prompt emission may be a result of mildly relativistic collisionless shocks (if GRB jets are baryonic). GRB external shocks are unmagnetized ultra-relativistic collisionless shocks and are the prime candidates to be the source of the observed afterglows, in which case these shocks: Generate long lasting magnetic field to sub-equipartition level Efficiently accelerate electrons at least to Tev energies Several processes were suggested as the source of the generated magnetic field in these shocks. None of which is confirmed yet.

22. Thank!

23. Are all the electrons need to be accelerated?  e  f  e  B  f  B   E/f n  n/f If only a fraction m e /m p <f<1 is accelerated the above mapping results in similar fit to f=1 (Eichler & Waxman 05).   dn/d 

24. Can the magnetic field decay after the shock? A decay of the magnetic field after the plasma crosses much less than 1% of the shocked shell is hard to explain by the observations (Rossi & Rees 02) No decay Decay after crossing 1% Decay after crossing 1%