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Core-collapse supernovae as cosmic ray sources.

Alexandre Marcowith1, Vikram V Dwarkadas2, Matthieu Renaud1

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Core-collapse supernovae shocks accelerate cosmic rays (CRs), driving instabilities and magnetic field amplification. This process can boost CRs to PeV energies within days, crucial for understanding supernova remnants.

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Area of Science:

  • Astrophysics
  • Plasma Physics
  • High-Energy Astrophysics

Background:

  • Core-collapse supernovae generate powerful shocks that interact with the dense circumstellar medium (CSM).
  • Cosmic rays (CRs) accelerated at these shocks can trigger electromagnetic instabilities in the foreshock region.

Purpose of the Study:

  • To calculate the growth timescales of CR-driven instabilities using a self-similar shock evolution model.
  • To investigate the potential for magnetic field amplification and CR acceleration in nearby core-collapse supernovae.

Main Methods:

  • Utilized a self-similar description of shock evolution to calculate instability growth times.
  • Analyzed radio data from Type II, Ib/Ic supernovae to infer parameters for instability calculations.
  • Examined the non-resonant streaming instability's contribution to magnetic field intensity.

Main Results:

  • Extended Type IIb supernova shocks can induce intra-day instabilities, significant magnetic field amplification, and CR acceleration (1-10 PeV) within days.
  • The non-resonant streaming instability accounts for approximately 50% of the deduced magnetic field intensity.
  • SN 2009bb accelerated CRs to 2-3 PeV within 20 days, despite more modest magnetic field amplification.

Conclusions:

  • Fast shocks in dense CSM are necessary for strong magnetic field amplification and CR acceleration.
  • Type IIn supernovae are potential candidates, but require detailed blast wave and particle acceleration modeling.
  • CR acceleration to PeV energies occurs rapidly after shock breakout in certain supernova types.