Gamma Ray Bursts Joo Braga INPE Dark ages
Gamma Ray Bursts João Braga - INPE Dark ages of GRBs n BATSE/CGRO: some light n GRBs x SGRs, magnetars n Beppo. SAX: afterglows and IDs n Progenitors n Host galaxies and cosmology n HETE, SWIFT and the future n
Dark Ages n July 1967: Vela satellites detect gamma ray outbursts n n 16 peculiar events of cosmic origin short (~s) photon flashes with E > 100 Me. V publication only in 1973
Dark Ages After ~30 ys only a reasonable idea of what they are n Phenomenology of bursts in the DAs: n n almost no association with known objects statistically poor distribution no clue
Dark Ages Burst of March 5 th, 1979 n SNR N 49 in LMC (~10, 000 ys) n 8 s oscillations in ~200 s Nature of GRBs associated with Galactic neutron stars: n rapid variability compact object (light-seconds) n cyclotron lines @ tens of ke. V B ~ 1012 G : = e. B/mc n emission lines @ hundreds of Ke. V redshifted 511 ke. V zobs = z 0 (1 – 2 GM/c 2 R) n periodicity rotation of a NS : R 3 < (GM/4 2) T 2
BATSE – COMPTON GRO • • ~3000 bursts (~1 each day) Isotropic distribution - No concentration towards LMC, M 31 or nearby clusters - No dipole and quadupole moments • • No spectral lines No periodicity Hundreds of models proposed
BATSE – COMPTON GRO Euclidean • Bimodal distribution — most are longer than 2 s — ~1/3 are shorter than 2 s • Spectra: combination of two power-laws - spectrum softens with time - Ep decreases with time (in the E. f(E) x E plot) • Fluence: ~ 10 -6 — 10 -4 erg cm-2 long duration and hard spectrum bursts deviate more from a 3 -D Euclidean brightness distribution
Soft Gamma Ray Repeaters SGR Burst of March 9 th, 1979 n SNR N 49 in LMC (~10, 000 ys) n 8 s oscillations in ~200 s SOFT GAMMA RAY REPEATERS n bursts repeat n soft spectra (E 100 ke. V) n short duration (~100 ms) n Galactic “distribution”, associated with SNRs
Soft Gamma Ray Repeaters SGR
Soft Gamma Ray Repeaters SGR
Rotating magnetized neutron stars d. E B 2 R 6 4 sin 2 = dt 6 c 3 Erot= I 2/2 ; P = 2 / d. E . = I dt . c 3/2 3 IPP 1/2 B = 3 R sin 2
Rotating magnetized neutron stars for SGR 0525 -66 (5/3/79): ~1 ms 8 s in ~10 kys. P ~ 3 x 10 -11 s s-1 B ~1015 G !! MAGNETAR
Rotating magnetized neutron stars Very high fields Fast spindown SGRs are young NSs which should still be associated to SNRs
MAGNETARS
MAGNETARS How do the bursts happen? n NS crust brakes due to EM tensions (starquakes) Alfvén waves injected in the magnetosphere particle acceleration optically thick pair plasma forms gamma-ray emission
MAGNETARS Problems: In 1900+14, RXTE measured a much. smaller P 2 ys before the 1998 active period EB increased by more than 100% Spindown is not magnetic and may be due to relativistic winds (no magnetar!)
Beppo. SAX and Afterglows n Beppo. SAX: - 4 narrow field instruments (. 1 to 300 ke. V; ~arcminute res. ) - Wide Field Camera (2 to 25 ke. V; 200 x 200 ; 5’; coded-mask) - Gamma Ray Burst Monitor (60 to 600 ke. V; side shield)
Beppo. SAX and Afterglows n 97 Feb 28: GRB 970228 n n Discovered by GRBM and WFC NFIs observe 1 SAX J 0501. 7+1146 First clear evidence of a GRB X-ray tail Non-thermal spectra X-ray fluence is 40% of -ray fluence
Beppo. SAX and Afterglows n n Beppo. SAX and RXTE discovered several other afterglows Optical transients: n n Observed in appr. ½ of the well localized bursts GRB 990123 is the only one observed in the optical when the gamma-ray flash was still going on
GRB 990123
GRB 011121
GRB 011121
Host galaxies n Optical IDs distant galaxies (low luminosity, blue) n n n ~20 measured redshifts All in the z = 0. 3 – 4. 5 range, with the exception of GRB 980425, possibly associated with SN 1998 bw @ z = 0. 008 OT is never far from center
redshifts
Progenitors Long GRBs are probably associated with massive and short-lived progenitors GRBs may be associated with rare types of supernovae n Hypernovae: colapse of rotating massive star black hole accreting from a toroid n Collapsar: coalescence with a compact companion GRBs and SN-type remnant n
Progenitors n Short GRBs are probably associated with mergers of compact objects
The fireball model n Observed fluxes require 1054 erg emitted in seconds in a small region (~km) Relativistic expanding fireball (e± , ) Problem: energy would be converted into Ek of accelerated baryons, spectrum would be quasithermal, and events wouldn’t be much longer than ms. Solution: fireball shock model: model shock waves will inevitably occur in the outflow (after fireball becomes transparent) reconvert Ek into nonthermal particle and radiation energy.
The fireball model n n n Complex light curves are due to internal shocks caused by velocity variations. Turbulent magnetic fields built up behind the shocks synchrotron power-law radiation spectrum Compton scattering to Ge. V range. Jetted fireball: fireball can be significantly collimated if progenitor is a massive star with rapid rotation escape route along the rotation axis jet formation alleviate energy requirements higher burst rates
High Energy Transient Explorer 1. First dedicated GRB mission, X- and -rays Equatorial orbit, antisolar pointing launched on Oct 9 th, 2000 - Pegasus 3 instruments, 1. 5 sr common FOV 1. SXC (0. 5 -10 ke. V) - < 30” localization WXM (2 – 25 ke. V) - < 10’ localization FREGATE (6 -400 ke. V) - sr localization Rapid dissemination ( 1 s) of GRB positions 1. 2. (Internet and GCN)
HETE
HETE Investigator Team MIT George R. Ricker (PI) Geoffrey Crew John P. Doty Al Levine Roland Vanderspek Joel Villasenor LANL Edward E. Fenimore Mark Galassi UC Santa Cruz Stanford Woosley RIKEN UC Berkeley Masaru Matsuoka Kevin Hurley Nobuyuki Kawai J. Garrett Jernigan Atsumasa Yoshida UChicago CESR Donald Q. Lamb Jean-Luc Atteia Carlo Graziani Gilbert Vedrenne INPE Jean-Francois Olive João Braga Michel Boer CNR CNES Graziella Pizzichini Jean-Luc Issler TIRF SUP’AERO Christian Colongo Ravi Manchanda
HETE in the Pegasus
Ground station network
GRB 010921 n n n Bright (>80 ) burst detected on Sept 21, 2001 05: 15: 50. 56 UT by FREGATE First HETE-discovered GRB with counterpart Detected by WXM, giving good X position (10 o x 20’ strip) Cross-correlation with Ulysses time history IPN annulus (radius 60 o ± 0. 118 o) intersection gives error region with 310 arcmin 2 centered at ~ 22 h 55 m 30 s, ~ 40052’
GRB 010921
GRB 010921 n Highly symmetric at high energies n Lower S/N for WXM due to offset n Durations increase by 65% at lower energies n Hard-to-soft spectral evolution n Peak energy flux in the 4 -25 ke. V band is 1/3 of 50 -300 ke. V n Peak photon flux is ~4 times higher in the 4 -25 ke. V
Discussion n Long duration GRB n X-ray rich, but no XRF (high 50 -300 ke. V flux) n z = 0. 450 isotropic energy of 7. 8 x 1051 erg ( M=0. 3, =0. 7, H 0=65 km s-1 Mpc-1) - less if beamed n Second lowest z strong candidate for extended searches for possible associated supernova n Final position available 15. 2 h after burst ground-based observations in the first night counterpart established well within HETE-IPN error region
Conclusions n GRBs occur at a rate of (no beaming) a few/day/universe or 1/few million ys/average galaxy or ~10 -91 cm-3 s-1 (since observed GRBs are detectable out to z ~10) n New missions are very important SWIFT: 3 instruments, 250 -300 bursts/yr, coverage from optical to gamma-rays, arcsecond positions, will detect bursts up to z ~20. INTEGRAL, EXIST, MIRAX n Cosmology: burts can proble early universe and some could be related to Pop III stars metal enrichment and ionization of the primordial gas.
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