THE WMAP HAZE FROM THE GALACTIC CENTER REGION DUE TO MASSIVE STAR EXPLOSIONS AND A REDUCED COSMIC RAY SCALE HEIGHT

被引：21

作者：

Biermann, Peter L. ^{[1
]}

Becker, Julia K. ^{[2
]}

Caceres, Gabriel ^{[3
]}

Meli, Athina ^{[4
]}

Seo, Eun-Suk ^{[5
]}

Stanev, Todor ^{[6
]}

机构：

[1] MPI Radioastron, Bonn, Germany

[2] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany

[3] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[4] Univ Erlangen Nurnberg, Inst Phys, ECAP, D-8520 Erlangen, Germany

[5] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[6] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 710卷 / 01期

关键词：

acceleration of particles; cosmic rays; radio continuum: general; shock waves; stars:; winds; outflows; supernovae: general; GAMMA-RAYS; MAGNETOHYDRODYNAMIC TURBULENCE; INTERSTELLAR-MEDIUM; EMISSION; RADIO; ENERGIES; SPECTRUM; ORIGIN; ACCELERATION; DISCOVERY;

D O I：

10.1088/2041-8205/710/1/L53

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

One important prediction of acceleration of particles in the supernova caused shock in the magnet ic 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 high er particle energy. We predict that more precise observations will find a radio spectrum of nu(-2/3), at higher frequencies nu(-1), and at yet higher frequencies finally nu(-3/2).

引用

页码：L53 / L57

页数：5