2004A&A...424..477F


Query : 2004A&A...424..477F

2004A&A...424..477F - Astronomy and Astrophysics, volume 424, 477-484 (2004/9-3)

The very early afterglow powered by ultra-relativistic mildly magnetized outflows.

FAN Y.Z., WEI D.M. and WANG C.F.

Abstract (from CDS):

In the Poynting Flux-dominated outflow (the initial ratio of the electromagnetic energy flux to the particle energy flux σ0≫1) model for gamma-ray bursts, particularly the γ-ray emission phase, nearly half of the internally dissipated magnetic energy is converted into the γ-ray energy emission and the rest is converted into the kinetic energy of the outflow. Consequently, at the end of the γ-ray burst, σ decreases significantly (σ∼1 or even smaller). We numerically investigate the very early reverse shock emission powered by such mildly magnetized outflows interacting with medium-uniform interstellar medium (ISM) or stellar wind (WIND). We show that for σ∼0.05-1 and typical parameters of gamma-ray bursts, both the ISM-ejecta interaction and the WIND-ejecta interaction can power very strong optical emission (mR∼10-12th mag or even brighter). Similar to the very early afterglow powered by the non-magnetized ejecta interacting with the external medium, the main difference between the ISM-ejecta interaction case and the WIND-ejecta interaction case is that, before the reverse shock crosses the ejecta, the R-band emission flux increases rapidly for the former, but for the latter it increases only slightly. At the very early stage, the ejecta are ultra-relativistic. Due to the beaming effect, the random magnetic field generated in shocks contained in the viewing area is axisymmetric, unless the line of sight is very near the edge of ejecta. The formula Πnet≃0.60b2/(1+b2) (where b is the ratio of the ordered magnetic field strength to that of random one) has been proposed to describe the net linear polarization of the synchrotron radiation coming from the viewing area. For σ∼0.05-1, the ordered magnetic field dominates over the random one generated in the reverse shock (As usual, we assume that a fraction εB∼0.01 of the thermal energy of the reverse shock has been converted into the magnetic energy), the high linear polarization is expected. We suggest that the linear polarization detection of the early multi-wavelength afterglow is required to see whether the outflows powering GRBs are magnetized or not.

Abstract Copyright:

Journal keyword(s): gamma-rays: bursts - magnetic fields - magnetohydrodynamics (MHD) - shock waves - relativity

Simbad objects: 4

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Number of rows : 4
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 GRB 021004 gB 00 26 54.68 +18 55 41.6           ~ 529 0
2 SN 2002lt SN* 08 08 59.858 +06 43 37.52           SNIc: 342 1
3 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 973 1
4 GRB 021206 gB 16 00 46.8 -09 42 36           ~ 103 0

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2022.05.20-02:03:43

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