The cosmic ray and the 10.7 cm flux variations during solar cycles 19-23

 

J. E. Mendoza-Torres,¹ X. Luo,² and H. Salazar³

 

¹ Instituto Nacional de Astrofísica, Óptica y Electrónica, Apdo. Postal 51 y 216, Puebla 72000, México (mend@inaoep.mx).

² SIGMA Weather Group, State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190, China (xluo@spaceweather.ac.cn).

³ Facultad de Ciencias Físico-Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla 72592, México (hsalazar@fcfm.buap.mx).

 

Received 2013 December 18.
Accepted 2014 April 30.

 

RESUMEN

Estudiamos los flujos de rayos cósmicos (CRF) y de 10.7 cm (F10.7) para los ciclos solares 19-23. La correlación cruzada indica dependencia más prolongada en ciclos impares que en pares. El movimiento del máximo en los histogramas CRF¹/F10.7¹ (los cocientes de los valores normalizados), no depende de la polaridad del ciclo. El comportamiento de CRF¹ vs F10.7¹, difiere entre ciclos pares e impares y también en diferentes fases del ciclo. Ajustamos un perfil CRF¹ invertido (CRF^inv) a F10.7¹ con una función lineal. El histograma F10.7¹/CRF^inv difiere para ciclos pares e impares. Los resultados para el número de manchas solares (SSN) son similares a los de F10.7 pero no para los histogramas F10.7¹/SSN^inv. Resumiendo, hay diferencias entre ciclos pares e impares, también en las fases de los ciclos y otras independientes de la polaridad del ciclo; estas últimas tal vez se originan fuera de la heliosfera.

 

ABSTRACT

The cosmic ray flux (CRF) and 10.7 cm flux (F10.7) are studied for solar cycles 19-23. The cross-correlations show longer time-dependence at odd than at even cycles. A shift of the maximum at the histograms of CRF¹ /F10.7¹ (the ratios of normalized values), does not depend on the polarity of the cycle. The behavior of CRF¹ vs F10.7¹ differs for odd and even cycles and also for different cycle phases. We fitted an inverted CRF¹ profile to the F10.7¹ profile with a linear function. The F10.7¹/CRF^inv histogram differs for odd and even cycles. The results for sunspot number (SSN) are similar to F10.7 but differ for the F10.7¹ /CRF^inv histograms. Summarizing, besides the differences between odd and even cycles, there occur variations at different phases of the cycles and also variations independent of the polarity of the cycle, the latter perhaps arising outside the heliosphere.

Key Words: Sun: activity — Sun: heliosphere — Sun: particle emission — Sun: radio radiation.

 

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ACKNOWLEDGMENTS

We acknowledge the Bartol Research Institute neutron monitor program supported by the United States National Science Foundation under grants ANT-0739620 and ANT-0838839, and by the University of Delaware Department of Physics and Astronomy and Bartol Research Institute, for the use of McMurdo Neutron Monitor data; also, the New Hampshire University, "National Science Foundation Grant ATM-0339527" for the use of CLIMAX Neutron Monitor data; the SIDC-team, World Data Center for the Sunspot Index, the Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium, the International Sunspot Number, Monthly Report on the International Sunspot Number, online catalogue of the sunspot index: http://www.sidc.be/sunspot-data/, for the use of Sunspot data from 1951 to 2006; and the Penticton Dominion Radio Astrophysical Observatory, of the National Research Council of Canada for the use of the solar flux data at 10.7 cm.

 

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