2009/10/07 by Peter L. Biermann, Julia K. Becker, Gabriel Caceres +3 · 1 citation
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #CMB cold spot #Cosmic ray #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Energy spectrum #Galactic Center #Galaxy #Particle acceleration #Stars #Supernova #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.1088/2041-8205/710/1/l53
10 pages
arxiv created 2009/10/07 · openalex publication_date 2010/01/20 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
One important prediction of acceleration of particles in the supernova caused shock in the magnetic wind of exploding Wolf–Rayet and red supergiant stars is the production of an energetic particle component with an E −2 spectrum at a level on the order of 1% of the full cosmic ray electron population. After allowing for transport effects, so steepening the spectrum to E −7/3 , this component as cosmic ray electrons readily explains the WMAP haze from the Galactic center region in spectrum, intensity, and radial profile; this requires the diffusion timescale for cosmic rays in the Galactic center region to be much shorter than in the solar neighborhood: the energy for cosmic ray electrons at the transition between diffusion dominance and loss dominance is shifted to considerably higher particle energy. We predict that more precise observations will find a radio spectrum of ν −2/3 , at higher frequencies ν −1 , and at yet higher frequencies finally ν −3/2 .