Table 1
Summary of the considered afterglow models.
| Spectral regime | βx − βopt | αx − αopt | Fν,opt/Fν,x |
|
|
|||
| Spherical expansion | |||
| νc < νopt < νx | 0 | 0 |
|
| νopt < νc < νx | 1/2 | ±1/4 |
|
| νopt < νx < νc | 0 | 0 |
|
| Jet with sideways expansion | |||
| νc < νopt < νx | 0 | 0 |
|
| νopt < νc < νx | 1/2 | 0 |
|
| νopt < νx < νc | 0 | 0 |
|
| Jet without sideways expansion | |||
| νc < νopt < νx | 0 | 0 |
|
| νopt < νc < νx | 1/2 | ±1/4 |
|
| νopt < νx < νc | 0 | 0 |
|
Notes. Theoretical differences in the spectral and temporal slopes as well as the flux-density ratio depend on the position of the cooling frequency, νc, with respect to the optical and the X-ray band (νopt,νx, respectively; valid for an electron index, p, of larger than 2; e.g., Zhang & Mészáros 2004; Panaitescu 2007). Depending on the circumburst medium the positive (ISM) or negative (wind) solution for αx − αopt applies.
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