Kinetic theory of cosmic ray and gamma-ray production in supernova remnants expanding into wind bubbles
A kinetic model of particle acceleration in supernova remnants (SNRs) is - extended to study the cosmic ray (CR) and associated high-energy gamma - -ray production during SN shock propagation through the inhomogeneous - circumstellar medium of a progenitor star that emits a wind. The wind - forms a...
Gespeichert in:
| Hauptverfasser: | , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
May 2000
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| In: |
Astronomy and astrophysics
Year: 2000, Jahrgang: 357, Pages: 283-300 |
| ISSN: | 1432-0746 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: http://adsabs.harvard.edu/abs/2000A%26A...357..283B
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| Verfasserangaben: | E.G. Berezhko, H.J. Völk |
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| 100 | 1 | |a Berezhko, Evgeny |e VerfasserIn |0 (DE-588)1222982544 |0 (DE-627)1742238793 |4 aut | |
| 245 | 1 | 0 | |a Kinetic theory of cosmic ray and gamma-ray production in supernova remnants expanding into wind bubbles |c E.G. Berezhko, H.J. Völk |
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| 520 | |a A kinetic model of particle acceleration in supernova remnants (SNRs) is - extended to study the cosmic ray (CR) and associated high-energy gamma - -ray production during SN shock propagation through the inhomogeneous - circumstellar medium of a progenitor star that emits a wind. The wind - forms a low-density bubble surrounded by a swept-up shell of - interstellar matter. gamma -rays are produced as a result of decay of - pions which in turn are the result of collisions of CRs with nuclei of - the thermal plasma. The time evolution of the SNRs is followed - numerically, taking into account the nonlinear backreaction of the - accelerated CRs. The model for SNRs includes injection of suprathermal - particles at the shock front and heating of the thermal plasma due to - dissipation of Alfvén waves in the precursor region. Examples - typical for SN type Ib and SN type II explosions are considered. Apart - from the confirmation of the known fact that acceleration is extremely - rapid and that the upper momentum cutoff is reached almost immediately - after the explosion due to the high wind magnetic field, it is also - shown that the CRs are accelerated with a high efficiency. Depending on - the circumstellar parameters, 20% to 40% of the SN explosion energy is - absorbed by CRs during the SNR evolution for a moderate injection rate, - when a fraction eta = 10-3 of the gas particles, swept up by - the supernova shock, is accelerated. The CR momentum spectrum, - ultimately produced in the SNRs, has a power law form N~ p-gamma - with an index gamma =2.0 to 2.1 in a wide energy range up to a - maximum energy, which is about 1014 eV, if the CR diffusion - coefficient is as small as the Bohm limiting value. It is to be expected - that the resulting CR chemical composition at high energies reflects - more the stellar wind composition, whereas at lower energies it - corresponds more to that of the average interstellar medium. The - expected pi 0-decay gamma -ray flux is however considerably - lower than in the case of a uniform interstellar medium; a relatively - high gamma -ray luminosity in the band epsilon gamma > 1 - TeV, detectable at distances of several kpc, is only expected in the - case of a relatively dense ISM with a number density above 10 - cm-3. Extremely high gamma -ray emission may be produced when - the SN shock propagates through the slow dense wind of a red supergiant, - the progenitor of a SN type II. In this case SNRs might be visible in - gamma -rays for several hundred years out to distances of tens of kpc. - For the case of a SN type Ib the expected pi 0-decay - gamma-ray TeV-energy flux during the whole SNR evolution remains lower - than 10-11 cm-2s-1 if the interstellar - number density is less than 0.3 cm-3. | ||
| 650 | 4 | |a COSMIC RAYS | |
| 650 | 4 | |a GAMMA -RAYS: THEORY | |
| 650 | 4 | |a ISM: SUPERNOVA REMNANTS | |
| 650 | 4 | |a SHOCK WAVES | |
| 650 | 4 | |a SUPERNOVA: GENERAL | |
| 700 | 1 | |a Völk, Heinrich J. |d 1936- |e VerfasserIn |0 (DE-588)1080938117 |0 (DE-627)84540542X |0 (DE-576)453843468 |4 aut | |
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