Linear polarization in gamma-ray bursts: The case for an ordered magnetic field

Jonathan Granot, Arieh Königl

פרסום מחקרי: פרסום בכתב עתמאמרביקורת עמיתים


Linear polarization at the level of ∼1%-3% has by now been measured in several gamma-ray burst afterglows. Whereas the degree of polarization, P, was found to vary in some sources, the position angle, θp, was roughly constant in all cases. Until now, the polarization has been commonly attributed to synchrotron radiation from a jet with a tangled magnetic field that is viewed somewhat off-axis. However, this model predicts either a peak in P or a 90° change in θp around the "jet break" time in the light curve, for which there has so far been no observational confirmation. We propose an alternative interpretation, wherein the polarization is attributed, at least in part, to a large-scale, ordered magnetic field in the ambient medium. The ordered component may dominate the polarization even if the total emissivity is dominated by a tangled field generated by postshock turbulence. In this picture, θp is roughly constant because of the uniformity of the field, whereas P varies as a result of changes in the ratio of the ordered-to-random mean-squared field amplitudes. We point out that variable afterglow light curves should be accompanied by a variable polarization. The radiation from the original ejecta, which includes the prompt γ-ray emission and the emission from the reverse shock (the "optical flash" and "radio flare"), could potentially exhibit a high degree of polarization (up to ∼60%) induced by an ordered transverse magnetic field advected from the central source.

שפה מקוריתאנגלית
עמודים (מ-עד)L83-L87
כתב עתAstrophysical Journal
מספר גיליון2 II
מזהי עצם דיגיטלי (DOIs)
סטטוס פרסוםפורסם - 10 ספט׳ 2003
פורסם באופן חיצוניכן

הערה ביבליוגרפית

Funding Information:
We thank P. Goldreich, R. Sari, A. Panaitescu, and E. Rossi for useful discussions. This research was supported in part by funds for natural sciences at the Institute for Advanced Study (J. G.) and by NASA ATP grant NAG5-12635 (A. K.).

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