Neutrino observatories can characterize cosmic sources and neutrino properties

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 67, Issue 7, 2003, Pages

  Barenboim, Gabriela ^a   Quigg, Chris ^a,b  

^a FERMI NATIONAL ACCELERATOR LABORATORY   (United States)

^b UNIVERSITY OF CALIFORNIA   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; CALCULATION; ELEMENTARY PARTICLE; ENERGY TRANSFER; MEASUREMENT; MOLECULAR INTERACTION; MOLECULAR STABILITY; OSCILLATION; SIGNAL TRANSDUCTION; TECHNIQUE;

EID: 3342932931     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.67.073024     Document Type: Article

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26. The interaction length of a 1-TeV neutrino is about 2.5 million kilometers of water, or (Formula presented) whereas high-energy photons are blocked by a few hundred (Formula presented)
27. We use the symbols (Formula presented) and (Formula presented) to denote the sum of neutrinos and antineutrinos except when we discuss implications of possible CPT violation, where (Formula presented) refer to neutrinos, and (Formula presented) to antineutrinos.
28. Muon cooling within the source, as discussed in Ref. 12, would deplete the source flux of (Formula presented) We have no candidate mechanism to produce an ultrahigh-energy flux like (Formula presented) In view of the current puzzlement over the origins of ultrahigh-energy cosmic rays, we think it prudent to keep an open mind about the range of possibilities.
29. The barred quantities refer to antineutrinos.
30. A similar phenomenon is familiar for cosmic-ray muons.
31. Our assumption that (Formula presented) is also a special case.