Authors

A Falcone, University of New Hampshire - Main CampusFollow
R Atkins, University of UtahFollow
W Benbow, University of California - Santa Cruz
D Berley, University of Maryland - College Park
M L. Chen, University of Maryland - College Park
D G. Coyne, University of California - Santa Cruz
B L. Dingus, University of UtahFollow
D E. Dorfan, University of California - Santa Cruz
R W. Ellsworth, George Mason University
D Evans, University of Maryland - College Park
L Fleysher, New York UniversityFollow
R Fleysher, New York UniversityFollow
G Gisler, Los Alamos National Laboratory
J A. Goodman, University of Maryland - College Park
T J. Haines, Los Alamos National LaboratoryFollow
C M. Hoffman, Los Alamos National Laboratory
S Hugenberger, University of California - Irvine
L A. Kelley, University of California - Santa Cruz
I Leonor, University of California - Irvine
J R. Macri, University of New Hampshire - Main Campus
M L. McConnell, University of New Hampshire - Main CampusFollow
J F. McCullough, University of California - Santa Cruz
J E. McEnery, University of UtahFollow
R S. Miller, University of New Hampshire - Main CampusFollow
A I. Mincer, New York University
M F. Morales, University of California - Santa CruzFollow
P Nemethy, New York University
James Ryan, University of New Hampshire
B Shen, University of California - Riverside
A Shoup, University of California - Irvine
G Sinnis, Los Alamos National Laboratory
A J. Smith, University of California - RiversideFollow
G W. Sullivan, University of Maryland - College Park
O T. Tumer, University of California - Riverside
K Wang, University of California - Riverside
M O. Wascko, University of California - Riverside
S Westerhoff, University of California - Santa Cruz
D A. Williams, University of California - Santa CruzFollow
T Yang, University of California - Santa Cruz
G B. Yodh, University of California - Irvine

Abstract

Solar Energetic Particles (SEPs) with energies exceeding 10 GeV associated with the 6 November 1997 solar flare/CME (coronal mass ejection) have been detected with Milagrito, a prototype of the Milagro Gamma Ray Observatory. While SEP acceleration beyond 1 GeV is well established, few data exist for protons or ions beyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detector designed for observing very high energy gamma ray sources, can also be used to study the Sun. Milagrito, which operated for approximately one year in 1997/98, was sensitive to solar proton and neutron fluxes above ∼4 GeV. In its scaler mode, Milagrito registered a rate increase coincident with the 6 November 1997 ground level event observed by Climax and other neutron monitors. A preliminary analysis suggests the presence of >10 GeV particles.

Publication Date

2000

Journal Title

AIP Conference Proceedings

Publisher

AIP Publishing

Digital Object Identifier (DOI)

10.1063/1.1303268

Document Type

Conference Proceeding

Rights

© 2000 American Institute of Physics

Share

COinS