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Gamma-Ray Bursts

0. Gamma-Ray Bursts. 0. Short (sub-second to minutes) flashes of gamma-rays, for ~ 30 years not associated with any counterparts in other wavelength bands First dedicated GRB detector: BATSE on the Compton Gamma-Ray Observatory. 0. GRB Light Curves. Long GRBs (duration > 2 s).

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Gamma-Ray Bursts

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  1. 0 Gamma-Ray Bursts

  2. 0 • Short (sub-second to minutes) flashes of gamma-rays, for ~ 30 years not associated with any counterparts in other wavelength bands • First dedicated GRB detector: BATSE on the Compton Gamma-Ray Observatory

  3. 0 GRB Light Curves Long GRBs (duration > 2 s) Short GRBs (duration < 1 s) Possibly two different types of GRBs: Long and short bursts

  4. 0 General Properties • Random distribution in the sky • Approx. 1 GRB per day observed • No repeating GRB sources

  5. 0 BeppoSAX (1996 – 2003) Wide-field Camera and Narrow-Field Instrument (NFI; X-ray telescope) allowed localization of GRBs to arc-minute accuracy First identification of X-ray and optical afterglows of g-ray bursts in 1997

  6. 0 Afterglows of GRBs On the day of the GRB 3 days after the GRB X-ray afterglow of GRB 970228 (GRBs are named by their date: Feb. 28, 1997) Most GRBs have gradually decaying afterglows in X-rays, some also in optical and radio.

  7. 1 day after GRB 2 days after GRB 0 Optical afterglow of GRB 990510 (May 10, 1999) Optical afterglows of GRBs are extremely difficult to localize: Very faint (~ 18 – 20 mag.); decaying within a few days.

  8. 0 Optical Afterglows of GRBs Host Galaxy Long GRBs are often found in the spiral arms (star forming regions!) of very faint host galaxies Optical Afterglow Optical afterglow of GRB 990123, observed with Hubble Space Telescope (HST/STIS)

  9. 0 Energy Output of GRBs Observed brightness combined with large distance implies huge energy output of GRBs, if they are emitting isotropically: E ~ 1054 erg L ~ 1051 erg/s Energy equivalent to the entire mass of the sun (E = mc2), converted into gamma-rays in just a few seconds! … another one, observed by us with the MDM 1.3 m telescope on Kitt Peak!

  10. 0 Beaming Evidence that GRBs are not emitting isotropically (i.e. with the same intensity in all directions), but they are beamed: E.g., achromatic breaks in afterglow light curves. GRB 990510

  11. 0 Models of GRBs (I) There’s no consensus about what causes GRBs. Several models have been suggested, e.g.: Hypernova: Supernova explosion of a very massive (> 25 Msun) star Iron core collapse forming a black hole; Material from the outer shells accreting onto the black hole Accretion disk => Jets =>GRB!

  12. 0 Models of GRBs (II) Supranova: If a neutron star is rotating extremely rapidly, it could escape collapse (for a few months) due to centrifugal forces. Neutron star will gradually lose angular momentum, then collapse into a black hole => collapse triggers the GRB

  13. 0 Results of the BeppoSAX Era • During the BeppoSAX era, X-ray, optical, radio afterglows were only found for long GRBs. • In afterglows and host galaxies, redshifts, clustered around ~ 1, were measured; unambiguously established the cosmological origin of GRBs. • Association with star-forming region, similarities of some optical light curves and spectra with type Ic supernovae provided strong support for hypernova/collapsar model for long GRBs

  14. 0 Swift (launched 2004) Dedicated GRB misssion with on-board soft g-ray, X-ray, and optical telescopes; Rapid automated localization and electronic distribution of GRBs with arc-second precision Localization of the first short GRBs; Some with significant offsets from host galaxies, favoring binary-compact-object merger models:

  15. 0 Models of GRBs (II) Black-hole – neutron-star merger: Black hole and neutron star (or 2 neutron stars) orbiting each other in a binary system Neutron star will be destroyed by tidal effects; neutron star matter accretes onto black hole => Accretion disk => Jets => GRB! Model works probably only for short GRBs.

  16. 0 Most successful model:

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