Limits on compression of cosmic rays in supernova remnants
arXiv:2302.10591 · doi:10.1093/mnras/stad584
Abstract
The spectral shape of the gamma-ray emission observed for dynamically old supernova remnants that interact with molecular clouds triggered an exciting scenario of adiabatic compression and farther re-acceleration of Galactic cosmic rays (GCRs) in radiative shells of the remnants, which was extensively discussed and applied to various sources over recent years. Indeed, the observed gamma-ray spectrum from a number of remnants strongly resembles the expected spectrum of the gamma-ray emission from the compressed population of Galactic cosmic rays. In the following we discuss the feasibility of this scenario and show that it is very unlikely that compressed GCRs could produce sufficient amount of gamma-rays and that the observed spectral shape is putting strong limits on the allowed compression factors. Further, absence of curvature in featureless power-law spectra of evolved supernova remnants at radio wavelengths is strongly disfavoring the compression scenario for electrons and hence for hadrons. Our calculations show that the contribution of compressed electrons to the observed radio-flux could reach at most ~10%.
8 pages, 3 figures, accepted for publication in MNRAS
References in corpus (14)
- Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
- Extended gamma-ray sources around pulsars constrain the origin of the positron flux at Earth
- The low frequency radio emission and spectrum of the extended SNR W44: new VLA observations at 74 and 324 MHz
- XMM-Newton observations of the supernova remnant IC443: I. soft X-ray emission from shocked interstellar medium
- Modeling Bright Gamma-ray and Radio Emission at Fast Cloud Shocks
- Numerical Simulations of Supernova Remnant Evolution in a Cloudy Interstellar Medium
- Imaging of SNR IC443 and W44 with the Sardinia Radio Telescope at 1.5 GHz and 7 GHz
- Negative and Positive Feedback from a Supernova Remnant with SHREC: A detailed Study of the Shocked Gas in IC443
- Spectral and morphological study of the gamma radiation of the middle-aged supernova remnant HB 21
- Gamma-Ray Emission from Supernova Remnant Interaction with Molecular Clumps
- Spectral softening in core-collapse supernova remnant expanding inside wind-blown bubble
- Time-dependent Diffusive Shock Acceleration in Slow Supernova Remnant Shocks
- SNR G39.2-0.3, an Hadronic Cosmic Rays Accelerator
- Production of secondary particles in heavy nuclei interactions in supernova remnants