Time-resolved spectroscopy of GRB 021004 reveals a clumpy extended wind
A high-resolution spectroscopy of GRB 021004 revealed a wealth of absorption lines from several intermediate-ionization species. The velocity structure of the absorber is complex and material with velocity up to ≳3000 km s−1 is observed. Since only the blueshifted component is observed, the absorber...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2006-11, Vol.372 (4), p.1791-1798 |
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| container_issue | 4 |
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| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 372 |
| creator | Lazzati, Davide Perna, Rosalba Flasher, Joseph Dwarkadas, Vikram V. Fiore, Fabrizio |
| description | A high-resolution spectroscopy of GRB 021004 revealed a wealth of absorption lines from several intermediate-ionization species. The velocity structure of the absorber is complex and material with velocity up to ≳3000 km s−1 is observed. Since only the blueshifted component is observed, the absorber is very likely to be material closely surrounding the gamma-ray burst. We use a time-dependent photoionization code to track the abundance of the ions over time. Thanks to the presence of absorption from intermediate-ionization states at long times, we can estimate the location and mass of the components of the absorber. We interpret those constraints within the hypernova scenario showing that the mass-loss rate of the progenitor must have been ∼10−4 M⊙ yr−1, suggestive of a very massive star. In addition, the wind termination shock must lie at a distance of at least 100 pc, implying a low-density environment. The velocity structure of the absorber also requires clumping of the wind at those large distances. |
| doi_str_mv | 10.1111/j.1365-2966.2006.10984.x |
| format | Article |
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The velocity structure of the absorber is complex and material with velocity up to ≳3000 km s−1 is observed. Since only the blueshifted component is observed, the absorber is very likely to be material closely surrounding the gamma-ray burst. We use a time-dependent photoionization code to track the abundance of the ions over time. Thanks to the presence of absorption from intermediate-ionization states at long times, we can estimate the location and mass of the components of the absorber. We interpret those constraints within the hypernova scenario showing that the mass-loss rate of the progenitor must have been ∼10−4 M⊙ yr−1, suggestive of a very massive star. In addition, the wind termination shock must lie at a distance of at least 100 pc, implying a low-density environment. 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| source | Wiley Online Library Journals Frontfile Complete; Oxford Journals Open Access Collection |
| subjects | Absorption rates Astronomy Earth, ocean, space Exact sciences and technology Gamma ray astronomy gamma-rays: bursts outflows Spectrum analysis stars: winds stars: winds, outflows stars: wolf–Rayet Wind |
| title | Time-resolved spectroscopy of GRB 021004 reveals a clumpy extended wind |
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