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The Cosmic Ray Observatories at IGEF-UNAM. José Fco Valdés-Galicia- PI Octavio Musalem Alejandro Hurtado Luis Xavier Gonzalez Jesús Alvarez Bernardo Vargas Ernesto Ortiz Rocío García Marcos Anzorena. Neutron Monitor And Muon Telescope. Monitor Type 6-NM64
José Fco Valdés-Galicia- PI
Luis Xavier Gonzalez
Monitor Type 6-NM64
Geographic Latitude = 19.33 °
W Longitude = 99.18 °
Altitude (asl) = 2274 m
Cutoff Rigidity = 8.23 GV
AÑO HELIOFÍSICO INTERNACIONAL (Naciones Unidas, 19 de febrero de 2007)
VESO (Instituto de Geofísica UNAM):
RIS Radio Interferómetro Solar (Investigaciones Solares y Planetarias)
MEXART (Mexican Array Radio Telescope)
Radiotelescopio de Centelleo Interplanetario (Física Espacial)
RC Observatorio de Rayos Cósmicos (Investigaciones Solares y Planetarias)
TEO Observatorio Geomagnético de Teoloyucan (Geomagnetismo y Exploración Geofísica)
From September 1, 1989 to December 31, 1996 upon request
COSMIC RAY DETECTION
AMPLIFICATION AND DISCRIMINATION
EMBEDDED DATA ADQUISITION
- Lead rings.
- Moderator material.
- Four high voltage and two low voltage power supplies.
- Miscellaneous components.
PC are veto for protons
Energy is resolved by
peak signal height
Direction is resolved by
PC in coincidence w/plastic
Graphical output of the simulation of a vertical impinging neutron of 500 MeV.
■ n + 12CSci → p+ Triggers four PRCs underneath the Sci (marked in red).
■ Production of low energy γby nuclear reaction inside the Sci
■ A strong solar flare occurred on Sept 7 2005
( X17.0, E= 17x10-1 erg cm2 seg-1).
■ Maximum at 17:40 UT (GOES),
■ Sierra Negra, was a suitable site to observe
solar neutrons 11:36:40 LT,
Solar zenith angle ~0°.
solar neutron channels, after the
hard X-ray peak time.
■ The statistical significance of the
(mid-day incoming flux, zenith angle = 0°).
b) The real proportion of SNT counting rates during the event on Sept 7,
2005 at 17:36:40 UT (11:36:40 LT ~0° of zenith angle).
Sako, et. al., 2006, & Watanabe, et. al., 2007, based on the time evolution profile
observed at Chacaltaya, assuming a power law functional form, calculated the spectral
index α. First using an impulsive injection and then using the 4 MeV gamma ray profile
as injection function.
Sako (2007) used 1 hr (17:30 to 18:30 UT) data from the Sierra Negra SNT, a detector
simulation based on GEANT3, and the atmospheric neutron atenuation calculated
by Shibata (1994) to make an estimate of α.
Spectral index results were:α= 3.1 & 3.2.
Based on GEANT4, the neutron atmospheric atenuation of Dorman & Valdés-Galicia
(1999), and 45 minute data (17:30 to 18:15 UT) from the Sierra Negra SNT,
we recalculated α.
■ The angular resolution of our SNT simulation is in very good agreement with real data taken during the event of September 7, 2005, constituting a validation of the simulation code.
■ From the simulation we may conclude that neutrons of ~1 GeV were observed.
■ Protons of at least 10GeV must have been produced. They were not observed as it was an east limb flare.
■ The spectral indexα of the september 7 2005 event is most likely close to 3.
PROTOTYPE NEXT WEEK
SSNT, NEXT MARCH IN TONANZINTLA,PUE