6 research outputs found
Spectral evolution of GRB 060904A observed with Swift and Suzaku -- Possibility of Inefficient Electron Acceleration
We observed an X-ray afterglow of GRB 060904A with the Swift and Suzaku
satellites. We found rapid spectral softening during both the prompt tail phase
and the decline phase of an X-ray flare in the BAT and XRT data. The observed
spectra were fit by power-law photon indices which rapidly changed from to within a few hundred
seconds in the prompt tail. This is one of the steepest X-ray spectra ever
observed, making it quite difficult to explain by simple electron acceleration
and synchrotron radiation. Then, we applied an alternative spectral fitting
using a broken power-law with exponential cutoff (BPEC) model. It is valid to
consider the situation that the cutoff energy is equivalent to the synchrotron
frequency of the maximum energy electrons in their energy distribution. Since
the spectral cutoff appears in the soft X-ray band, we conclude the electron
acceleration has been inefficient in the internal shocks of GRB 060904A. These
cutoff spectra suddenly disappeared at the transition time from the prompt tail
phase to the shallow decay one. After that, typical afterglow spectra with the
photon indices of 2.0 are continuously and preciously monitored by both XRT and
Suzaku/XIS up to 1 day since the burst trigger time. We could successfully
trace the temporal history of two characteristic break energies (peak energy
and cutoff energy) and they show the time dependence of while the following afterglow spectra are quite stable. This fact
indicates that the emitting material of prompt tail is due to completely
different dynamics from the shallow decay component. Therefore we conclude the
emission sites of two distinct phenomena obviously differ from each other.Comment: 19 pages, 9 figures, accepted for publication in PASJ (Suzaku 2nd
Special Issue
HETE-2 Observations of the X-Ray Flash XRF 040916
A long X-ray flash was detected and localized by the instruments aboard the
High Energy Transient Explorer II (HETE-2) at 00:03:30 UT on 2004 September 16.
The position was reported to the GRB Coordinates Network (GCN) approximately 2
hours after the burst. This burst consists of two peaks separated by 200 s,
with durations of 110 s and 60 s. We have analyzed the energy spectra of the
1st and 2nd peaks observed with the Wide Field X-Ray Monitor (WXM) and the
French Gamma Telescope (FREGATE). We discuss the origin of the 2nd peak in
terms of flux variabilities and timescales. We find that it is most likely part
of the prompt emission, and is explained by the long-acting engine model. This
feature is similar to some bright X-ray flares detected in the early afterglow
phase of bursts observed by the Swift satellite.Comment: 9 pages, 4 figures, Accepted for publication in PAS
Development of A New Background Reduction Method for WXM/HETE-2 and Its Application for Bright GRB Spectra
Multiple-Component Analysis of the Time-Resolved Spectra of GRB 041006:A Clue to the Nature of the Underlying Soft Component of GRBs.
Spectral evolution of GRB 060904A observed with Swift and Suzaku
Abstract We observed an X-ray afterglow of GRB 060904A with the Swift and Suzaku satellites. We found a rapid spectral softening in the prompt tail observed by Swift. Adopting the absorbed power-law model to the observed spectra, the photon indices rapidly change from Γ = 1.2 ± 0.1 to Γ = 5.3 +0.7 −0.6 . It is quite difficult to explain this ultra soft spectrum by the simple electron acceleration and the synchrotron radiation. 1 Then we try to advanced spectral fitting with the broken power-law with exponential cutoff (BPEC) model, and the power-law with blackbody as seen in GRB 060218. The observed spectra can be explained by the both models. After the transition to the shallow decay phase, the spectral photon indices become steady as the typical value of Γ ∼ 2, and this value keeps flat toward the end of Suzaku observation. Through these observation, we confirmed that no significant spectral evolution was found during the shallow-classical-jet break phases