Prompt optical emission and synchrotron self-absorption constraints on emission site of GRBs
نویسندگان
چکیده
منابع مشابه
Gamma-ray burst prompt emission variability in synchrotron and synchrotron self-Compton light curves
Gamma-ray burst prompt emission is believed to originate from electrons accelerated in a highly relativistic outflow. Internal shocks, which are a result of collisions between shells ejected by the central engine, are the leading candidates for electron acceleration. While synchrotron radiation is generally invoked to interpret prompt gamma-ray emission within the internal shock model, the sync...
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Detecting high-z GRBs is important for constraining the GRB formation rate, and tracing the history of re-ionization and metallicity of the universe. Based on the current sample of GRBs detected by Swift with known redshifts, we investigated the relationship between red-shift, and spectral and temporal characteristics, using the BAT event-by-event data. We found red-shift trends for the peak-fl...
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Aims. The prompt optical emission contemporaneous with the γ-rays from γ-ray bursts (GRBs) carries important information on the central engine and explosion mechanism. We study the time lag between prompt optical emission and γ-rays in GRB 990123 and GRB 041219a, which are the only two GRBs had been detected at optical wavelengths during the ascending burst phase. Methods. Assuming profiles of ...
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We report on observations of correlated behavior between the prompt γ-ray and optical emission from GRB 080319B, which (i) strongly suggest that they occurred within the same astrophysical source region and (ii) indicate that their respective radiation mechanisms were most likely dynamically coupled. Our preliminary results, based upon a new cross-correlation function (CCF) methodology for dete...
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We calculate the prompt x–ray emission as a function of viewing angle for beamed Gamma–Ray Burst (GRB) sources. Prompt x-rays are inevitable due to the less highly blueshifted photons emitted at angles ∼> 1/γ relative to the beam symmetry axis, where γ is the expansion Lorentz factor. The observed flux depends on the combinations γ∆θ and γθv, where ∆θ is the beaming angle and θv is the viewing ...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2009
ISSN: 0035-8711,1365-2966
DOI: 10.1111/j.1365-2966.2009.15212.x