Browsing by Autor "Pedro Miranda"

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Analysis of Background Cosmic Ray Rate in the 2010-2012 Period from the LAGO-Chacaltaya Detectors
(2016) C. Sarmiento‐Cano; Luis Arturo Nuñez-Castiñeyra; H. Asorey; Luis A. Núñez; Pedro Miranda; C. J. Solano Salinas; R. Ticona
The Latin American Giant Observatory (LAGO) is an extended Cosmic Rays observatory composed by a network of Cherenkov Detectors (WCDs) spread over Latin America. This work will report the analysis of three years of data from three LAGO WCD located in Cerro Chacaltaya, Bolivia, at 5200 m a.s.l. Background cosmic ray rate from these detectors is checked for DAQ issues and inconsistencies, and corrected for atmospheric effects. An analysis for short transients up to the minute timescale is performed, in search for coincidence with transients observed by satellites. Sidereal and solar long term epoch data analysis are also presented.
Detection of Solar Neutrons and Solar Neutron Decay Protons
(2023) Y. Muraki; Tatsumi Koi; Y. Matsubara; S. Masuda; Pedro Miranda; Shoko Miyake; T. Naito; Ernesto Ortiz Fragoso; A. Oshima; T. Sako
Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma-rays and neutrons produced by the impulsive flare. Under such circumstances, on November 7, 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma-rays and neutrons. These particles were received as neutrons and line gamma-rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar-terrestrial space. These secondary protons arrived at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4,600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare.
Detection of Solar Neutrons and Solar Neutron Decay Protons
(Multidisciplinary Digital Publishing Institute, 2023) Y. Muraki; Tatsumi Koi; S. Masuda; Y. Matsubara; Pedro Miranda; Shoko Miyake; T. Naito; E. Ortiz; A. Oshima; T. Sako
Solar flares are broadly classified as impulsive or gradual. Ions accelerated in a gradual flare are thought to be accelerated through a shock acceleration mechanism, but the particle acceleration process in an impulsive flare is still largely unexplored. To understand the acceleration process, it is necessary to measure the high-energy gamma rays and neutrons produced by the impulsive flare. Under such circumstances, on 7 November 2004, a huge X2.0 flare occurred on the solar surface, where ions were accelerated to energies greater than 10 GeV. The accelerated primary protons collided with the solar atmosphere and produced line gamma rays and neutrons. These particles were received as neutrons and line gamma rays, respectively. Neutrons of a few GeV, on the other hand, decay to produce secondary protons while traveling 0.06 au in the solar–terrestrial space. These secondary protons arrive at the magnetopause. Although the flux of secondary protons is very low, the effect of collecting secondary protons arriving in a wide region of the magnetosphere (the Funnel or Horn effect) has resulted in significant signals being received by the solar neutron telescope at Mt. Sierra Negra (4600 m). This information suggests that ions on the solar surface are accelerated to over 10 GeV with an impulsive flare.
Determinación de la línea meridiana en el observatorio geomagnético de Patacamaya
(1999) Deterlino Urzagasti; Edgar Ricadldi; Pedro Miranda; Erick Franck; Adolfo Aramayo; César Antonio Cabrera Tapia
Modelo dinámico del comportamiento térmico de un invernadero mediante un circuito eléctrico equivalente
(1996) Alfonso Velarde; Pedro Miranda; Marcelo Córdova; Luis Blacutt; Sergio Velarde; Javier Riera; Wilmar Velázquez; Carlos Ormachea
New air Cherenkov light detectors to study mass composition of cosmic rays with energies above knee region
(Elsevier BV, 2014) Y. Tsunesada; Ryoichi Katsuya; Yu Mitsumori; Keisuke Nakayama; F. Kakimoto; Hisao Tokuno; Norio Tajima; Pedro Miranda; Juan Salinas; Wilfredo Tavera
Observaciones geomagnéticas en el observatorio de Patacamaya
(1996) Gonzalo Gutiérrez; Edgar Ricaldi; A Cabrera; Pedro Miranda; J.L Telleria
Report on scipost_202207_00031v1
(2022) Shoko Miyake; T. Koi; Y. Muraki; Y. Matsubara; S. Masuda; Pedro Miranda; T. Naito; E. Ortiz; A. Oshima; T. Sakai
In association with a large solar flare on November 7, 2004, the solar neutron detectors located at Mt. Chacaltaya (5,250 m) in Bolivia and Mt.Sierra Negra (4,600 m) in Mexico recorded very interesting events.In order to explain these events, we have performed a calculation solving the equation of motion of anti-protons inside the magnetosphere.Based on these results, the Mt.Chacaltaya event may be explained by the detection of solar neutrons, while the Mt.Sierra Negra event may be explained by the first detection of very high energy solar neutron decay protons (SNDPs) around 6 GeV.