Strong signals of neutral emissions were detected in association with a solar flare that occurred on 2005 September 7. They were produced by both relativistic ions and electrons. In particular, relativistic neutrons were observed with the solar neutron telescopes (SNTs) located at Mount Chacaltaya in Bolivia and Mount Sierra Negra in Mexico and with neutron monitors (NMs) at Chacaltaya and Mexico City with high statistical significances. At the same time, hard X-rays and g-rays, which were predominantly emitted by high-energy electrons, were detected by the Geotail and the INTEGRAL satellites. We found that a model of the impulsive neutron emission at the time of the X-ray/ g-ray peak can explain the main peaks of all the detected neutron signals, but failed to explain the long tailed decaying phase. An alternative model, in which the neutron emission follows the X-ray/g-ray profile, also failed to explain the long tail. These results indicate that the acceleration of ions began at the same time as the electrons but that ions were continuously accelerated or trapped longer than the electrons in the emission site. We also demonstrate that the neutron data observed by multienergy channels of SNTs put constraints on the neutron spectrum.
Un Telescopio de Neutrones Solares (TNS) fue instalado en la cima del volcán Sierra Negra, Pue., México (19.0º N , 97.3º W, 4580 m sobre el nivel del mar); el cual se encuentra en operación desde el 2004. En este trabajo, utilizamos los valores de la presión barométrica, de la presión dinámica, de la temperatura ambiental y de la humedad relativa obtenidos por una estación meteorológica cercana al TNS, para calcular los coeficientes de corrección atmosféricos para el flujo registrado de rayos cósmicos. Cuando los datos de rayos cósmicos están libres de las variaciones de origen atmosférico, analizamos los perfiles de tiempo observados por el TNS durante seis decrecimientos tipo Forbush seleccionados para el período 2011-2013. Los resultados obtenidos por varios canales de depósito de energía (30,60,90 MeV) son discutidos para establecer la confiabilidad del TNS para este tipo de eventos.
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