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Observation of intensity of cosmic rays and daily magnetic shifts near meridian 70 degrees in the South America
| Indexado |
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| DOI | 10.1016/J.JASTP.2016.02.015 | ||||
| Año | 2016 | ||||
| Tipo | artículo de investigación |
Citas Totales
Autores Afiliación Chile
Instituciones Chile
% Participación
Internacional
Autores
Afiliación Extranjera
Instituciones
Extranjeras
Abstract
Our magnetometer data shows that for each of the components, shifts in the magnetic field intensity for every station (even for those out of the SAMA) lasted between 3 and 4 h after sunrise and 1 and 2 h past sunset, which are the periods when the geomagnetic field is modulated by the transit of the dayside to nightside and nightside to dayside. We believe that, although the magnetometric data indicates the magnetic reconnection for the Chilean region, there is no direct influence from the SAMA other than the lower rigidity cut-off that leads to an increased count rate. Other details about the magnetic field components such as muon and neutron count rate, diurnal variation and"sunset enhancement' are reported in this work. (C) 2016 Elsevier Ltd. All rights reserved.
| Ord. | Autor | Género | Institución - País |
|---|---|---|---|
| 1 | CORDARO-CARDENAS, ENRIQUE GUILLERMO | Hombre |
Universidad de Chile - Chile
Universidad Autónoma de Chile - Chile |
| 2 | Galvez, D. | - |
Universidad de Chile - Chile
|
| 3 | LAROZE-NAVARRETE, DAVID NICOLAS | Hombre |
Universidad de Tarapacá - Chile
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| Fuente |
|---|
| Universidad de Tarapacá |
| CEDENNA |
| UTA |
| Universidad de Tarapacá |
| Basal Program Center for Development of Nanoscience and Nanotechnology (CEDENNA) |
| Basal Program Center for Development of Nanoscience and Nanotechnology |
| Centro para el Desarrollo de la Nanociencia y la Nanotecnologia |
| Agradecimiento |
|---|
| We thank E. Zesta and P. Venegas for their collaboration in this work. We acknowledge the use of the UCLA-IGPP fluxgate magnetometer. We are currently in collaboration with the South American Magnetometer B-field Array (SAMBA) project of the University of California Los Angeles (USA). All the geomagnetic data used in this work belongs to this collaboration (data can be found in http://magnetometers.bc.edu/index.php/78-magnetometers/78-home and can also be requested to the authors). All the cosmic ray data used in this work belong to the Chilean Cosmic Ray Network, and can be obtained by contacting the corresponding author. We also thank IGRF and Intermagnet for the development of the IAGA V-MOD geomagnetic field modeling system that we used in this work (model available in http://wdc.kugi.kyoto-u. acjp/igrf/). D.L. acknowledges the partial financial support from Basal Program Center for Development of Nanoscience and Nanotechnology (CEDENNA) and UTA Project 8750-12. |
| We thank E. Zesta and P. Venegas for their collaboration in this work. We acknowledge the use of the UCLA-IGPP fluxgate magnetometer. We are currently in collaboration with the South American Magnetometer B-field Array (SAMBA) project of the University of California Los Angeles (USA). All the geomagnetic data used in this work belongs to this collaboration (data can be found in http://magnetometers.bc.edu/index.php/78-magnetometers/78-home and can also be requested to the authors). All the cosmic ray data used in this work belong to the Chilean Cosmic Ray Network, and can be obtained by contacting the corresponding author. We also thank IGRF and Intermagnet for the development of the IAGA V-MOD geomagnetic field modeling system that we used in this work (model available in http://wdc.kugi.kyoto-u.ac.jp/igrf/ ). D.L. acknowledges the partial financial support from Basal Program Center for Development of Nanoscience and Nanotechnology (CEDENNA) and UTA Project 8750-12 . |
