First predicted cosmic ray spectra, primary-to-secondary ratios, and ionization rates from MHD galaxy formation simulations

We present the first simulations evolving resolved spectra of cosmic rays (CRs) from MeV-TeV energies (including electrons, positrons, (anti)protons, and heavier nuclei), in live kinetic-magnetohydrodynamics galaxy simulations with star formation and feedback. We utilize new numerical methods including terms often neglected in historical models, comparing Milky Way analogues with phenomenological scattering coefficients upsilon to Solar-neighbourhood [Local interstellar medium (LISM)] observations (spectra, B/C, e(+)/e(-), (p) over bar /p, Be-10/Be-9, ionization, and gamma-rays). We show it is possible to reproduce observations with simple single-power-law injection and scattering coefficients (scaling with rigidity R), similar to previous (non-dynamical) calculations. We also find: (1) The circumgalactic medium in realistic galaxies necessarily imposes an similar to 10 kpc CR scattering halo, influencing the required upsilon(R). (2) Increasing the normalization of upsilon(R) re-normalizes CR secondary spectra but also changes primary spectral slopes, owing to source distribution and loss effects. (3) Diffusive/turbulent reacceleration is unimportant and generally sub-dominant to gyroresonant/streaming losses, which are sub-dominant to adiabatic/convective terms dominated by similar to 0.1-1 kpc turbulent/fountain motions. (4) CR spectra vary considerably across galaxies; certain features can arise from local structure rather than transport physics. (5) Systematic variation in CR ionization rates between LISM and molecular clouds (or Galactic position) arises naturally without invoking alternative sources. (6) Abundances of CNO nuclei require most CR acceleration occurs around when reverse shocks form in SNe, not in OB wind bubbles or later Sedov-Taylor stages of SNe remnants.

Automated summary

In this study, we utilized new numerical methods to simulate the evolution of cosmic rays, and discovered some characteristics and influencing factors of cosmic rays. The results showed that the scattering coefficient of cosmic rays is influenced by the circumgalactic medium in galaxies, and the impact of diffusive/turbulent reacceleration on cosmic rays is relatively minor. Additionally, cosmic ray spectra vary considerably across galaxies, and the ionization rate of cosmic rays also varies in different environments.