Portal:Radiation astronomy/Resource/10
Protons
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"Proton astronomy should be possible; it may also provide indirect information on inter-galactic magnetic fields."[1]
Proton astronomy per se often consists of directly or indirectly detecting the protons and deconvoluting a spatial, temporal, and spectral distribution.
“[A]t the high end of the proton energy spectrum (above ≈ 1018 eV) [the Larmor radius] deflection becomes small enough that proton astronomy becomes possible.”[2]
"The third largest solar proton event in the past thirty years took place during July 14-16, 2000, and had a significant impact on the earth's atmosphere."[3]
References
[edit | edit source]- ↑ Francis Halzen and Dan Hooper (July 2002). "High-energy neutrino astronomy: the cosmic ray connection". Reports on Progress in Physics 65 (7): 1025-78. doi:10.1088/0034-4885/65/7/201. http://arxiv.org/pdf/astro-ph/0204527. Retrieved 2011-11-24.
- ↑ K. D. Hoffman (May 12, 2009). "High energy neutrino telescopes". New Journal of Physics 11 (5): 055006. doi:10.1088/1367-2630/11/5/055006. http://arxiv.org/pdf/astro-ph/0204527. Retrieved 2012-03-28.
- ↑ Charles H. Jackman, Richard D. McPeters, Gordon J. Labow, Eric L.Fleming, Cid J. Praderas, James M. Russell (August 2001). "Northern Hemisphere atmospheric effects due to the July 2000 solar proton event". Geophysical Research Letters 28 (15): 2883-6. http://cdaw.gsfc.nasa.gov/meetings/2009_gle/data/Jackman/Jackman_2001.pdf. Retrieved 2011-11-24.