Probing maximum energy of cosmic rays in SNR through gamma rays and neutrinos from the molecular clouds around SNR W28. (arXiv:1905.07571v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Banik_P/0/1/0/all/0/1">Prabir Banik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhadra_A/0/1/0/all/0/1">Arunava Bhadra</a>
The galactic cosmic rays are generally believed to be originated in supernova
remnants (SNRs), produced in diffusive shock acceleration (DSA) process in
supernova blast waves driven by expanding SNRs. One of the key unsettled issue
in SNR origin of cosmic ray model is the maximum attainable energy by a cosmic
ray particle in the supernova shock. Recently it has been suggested that an
amplification of effective magnetic field strength at the shock may take place
in young SNRs due to growth of magnetic waves induced by accelerated cosmic
rays and as a result the maximum energy achieved by cosmic rays in SNR may
reach the knee energy instead of $sim 200$ TeV as predicted earlier under
normal magnetic field situation. In the present work we investigate the
implication of such maximum energy scenarios on TeV gamma rays and neutrino
fluxes from the molecular clouds interacting with the SNR W28. The authors
compute the gamma-ray and neutrino flux assuming two different values for the
maximum energy reached by cosmic rays in the SNR, from CR interaction in nearby
molecular clouds. Both protons and nuclei are considered as accelerated
particles and as target material. Our findings suggest that the issue of the
maximum energy of cosmic rays in SNRs can be observationally settled by the
upcoming gamma-ray experiment the Large High Altitude Air Shower Observatory
(LHAASO). The estimated neutrino fluxes from the molecular clouds are ,
however, out of reach of the present/near future generation of neutrino
telescopes.
The galactic cosmic rays are generally believed to be originated in supernova
remnants (SNRs), produced in diffusive shock acceleration (DSA) process in
supernova blast waves driven by expanding SNRs. One of the key unsettled issue
in SNR origin of cosmic ray model is the maximum attainable energy by a cosmic
ray particle in the supernova shock. Recently it has been suggested that an
amplification of effective magnetic field strength at the shock may take place
in young SNRs due to growth of magnetic waves induced by accelerated cosmic
rays and as a result the maximum energy achieved by cosmic rays in SNR may
reach the knee energy instead of $sim 200$ TeV as predicted earlier under
normal magnetic field situation. In the present work we investigate the
implication of such maximum energy scenarios on TeV gamma rays and neutrino
fluxes from the molecular clouds interacting with the SNR W28. The authors
compute the gamma-ray and neutrino flux assuming two different values for the
maximum energy reached by cosmic rays in the SNR, from CR interaction in nearby
molecular clouds. Both protons and nuclei are considered as accelerated
particles and as target material. Our findings suggest that the issue of the
maximum energy of cosmic rays in SNRs can be observationally settled by the
upcoming gamma-ray experiment the Large High Altitude Air Shower Observatory
(LHAASO). The estimated neutrino fluxes from the molecular clouds are ,
however, out of reach of the present/near future generation of neutrino
telescopes.
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