Time-dependent modeling of pulsar wind nebulae
A spatially independent model that calculates the time evolution of the electron spectrum in a spherically expanding pulsar wind nebula (PWN) is presented, allowing one to make broadband predictions for the PWN's non-thermal radiation. The source spectrum of electrons injected at the terminatio...
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| Main Authors: | , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
2013 August 5
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| In: |
The astrophysical journal
Year: 2013, Volume: 773, Issue: 2, Pages: 1-11 |
| ISSN: | 1538-4357 |
| DOI: | 10.1088/0004-637X/773/2/139 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1088/0004-637X/773/2/139
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| Author Notes: | M.J. Vorster, O. Tibolla, S.E.S. Ferreira, and S. Kaufmann |
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| 245 | 1 | 0 | |a Time-dependent modeling of pulsar wind nebulae |c M.J. Vorster, O. Tibolla, S.E.S. Ferreira, and S. Kaufmann |
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| 520 | |a A spatially independent model that calculates the time evolution of the electron spectrum in a spherically expanding pulsar wind nebula (PWN) is presented, allowing one to make broadband predictions for the PWN's non-thermal radiation. The source spectrum of electrons injected at the termination shock of the PWN is chosen to be a broken power law. In contrast to previous PWN models of a similar nature, the source spectrum has a discontinuity in intensity at the transition between the low- and high-energy components. To test the model, it is applied to the young PWN G21.5−0.9, where it is found that a discontinuous source spectrum can model the emission at all wavelengths better than a continuous one. The model is also applied to the unidentified sources HESS J1427−608 and HESS J1507−622. Parameters are derived for these two candidate nebulae that are consistent with the values predicted for other PWNe. For HESS J1427−608, a present day magnetic field of Bage = 0.4 μG is derived. As a result of the small present day magnetic field, this source has a low synchrotron luminosity, while remaining bright at GeV/TeV energies. It is therefore possible to interpret HESS J1427−608 within the ancient PWN scenario. For the second candidate PWN HESS J1507−622, a present day magnetic field of Bage = 1.7 μG is derived. Furthermore, for this candidate PWN a scenario is favored in the present paper in which HESS J1507−622 has been compressed by the reverse shock of the supernova remnant. | ||
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