SIMBAD references

2013ApJ...773..139V - Astrophys. J., 773, 139 (2013/August-3)

Time-dependent modeling of pulsar wind nebulae.

VORSTER M.J., TIBOLLA O., FERREIRA S.E.S. and KAUFMANN S.

Abstract (from CDS):

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.

Abstract Copyright:

Journal keyword(s): ISM: individual (G21.5-0.9, HESS J1427-608, HESS J1507-622) - ISM: supernova remnants - radiation mechanisms: non-thermal

Simbad objects: 15

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2021.02.26-19:16:55

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