Inverse Compton gamma-ray models for remnants of Galactic type Ia supernovae?
arXiv:0809.2432 · doi:10.1051/0004-6361:200810501
Abstract
We theoretically and phenomenologically investigate the question whether the gamma-ray emission from the remnants of the type Ia supernovae SN 1006, Tycho's SN and Kepler's SN can be the result of electron acceleration alone. The observed synchrotron spectra of the three remnants are used to determine the average momentum distribution of nonthermal electrons as a function of the assumed magnetic field strength. Then the inverse Compton emission spectrum in the Cosmic Microwave Background photon field is calculated and compared with the existing upper limits for the very high energy gamma-ray flux from these sources. It is shown that the expected interstellar magnetic fields substantially overpredict even these gamma-ray upper limits. Only rather strongly amplified magnetic fields could be compatible with such low gamma-ray fluxes. However this would require a strong component of accelerated nuclear particles whose energy density substantially exceeds that of the synchrotron electrons, compatible with existing theoretical acceleration models for nuclear particles and electrons. Even though the quantitative arguments are simplistic, they appear to eliminate simplistic phenomenological claims in favor of a inverse Compton gamma-ray scenario for these sources.
6 pages, 1 figure, accepted for publication in Astronomy and Astrophysics
References in corpus (13)
- H.E.S.S. observations of the supernova remnant RX J0852.0-4622: shell-type morphology and spectrum of a widely extended VHE gamma-ray source
- HESS Observations and VLT Spectroscopy of PG 1553+113
- Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field
- Spectrum of cosmic rays, produced in supernova remnants
- Variation of cosmic ray injection across supernova shocks
- The gas density around SN 1006
- Suzaku wide-band observations of SN 1006
- Cosmic Ray Acceleration by Supernova Shocks
- H.E.S.S. upper limits for Kepler's supernova remnant
- Arguments against a dominantly hadronic origin of the VHE radiation from the supernova remnant RX J1713-3946
- Dependence of the gamma-ray emission from SN 1006 on the astronomical parameters
- Gamma-ray emission expected from Kepler's SNR
- CANGAROO-III Search for Gamma Rays from Kepler's Supernova Remnant
Cited by in corpus (9)
- Broad-band nonthermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants
- Cosmic ray acceleration parameters from multi-wavelength observations. The case of SN 1006
- Hadronic versus leptonic origin of the gamma-ray emission from Supernova Remnant RX J1713.7-3946
- Saturated magnetic field amplification at supernova shocks
- Predicted gamma-ray image of SN 1006 due to inverse Compton emission
- Observational constraints on the modeling of SN1006
- Nonthermal properties of supernova remnant G1.9+0.3
- Hadronic gamma-ray images of Sedov supernova remnants
- Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes