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Title: Variations in Solar Parameters and Cosmic Rays with Solar Magnetic Polarity

Abstract

The sunspot number varies with the 11-year Schwabe cycle, and the solar magnetic polarity reverses every 11 years approximately at the solar maximum. Because of polarity reversal, the difference between odd and even solar cycles is seen in solar activity. In this study, we create the mean solar cycle expressed by phase using the monthly sunspot number for all solar cycles 1–23. We also generate the mean solar cycle for sunspot area, solar radio flux, and cosmic ray flux within the allowance of observational range. The mean solar cycle has one large peak at solar maximum for odd solar cycles and two small peaks for most even solar cycles. The odd and even solar cycles have the statistical difference in value and shape at a confidence level of at least 98%. For solar cycles 19–23, the second peak in the even solar cycle is larger than the first peak. This result is consistent with the frequent solar events during the declining phase after the solar maximum. The difference between odd and even solar cycles can be explained by a combined model of polarity reversal and solar rotation. In the positive/negative polarity, the polar magnetic field introduces angular momentum in themore » same/opposite direction as/to the solar rotation. Thus the addition/subtraction of angular momentum can increase/decrease the motion of plasma to support the formation of sunspots. Since the polarity reverses at the solar maximum, the opposite phenomenon occurs in the declining phase.« less

Authors:
 [1];  [2]
  1. Department of Earth Science Education, Chonnam National University, Gwangju, 61186 (Korea, Republic of)
  2. Department of Astronomy, Space Science and Geology, Chungnam National University, Daejeon, 34134 (Korea, Republic of)
Publication Date:
OSTI Identifier:
22663665
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 840; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANGULAR MOMENTUM; APPROXIMATIONS; COSMIC RADIATION; COSMIC RAY FLUX; MAGNETIC FIELDS; PLASMA; ROTATION; SOLAR CYCLE; SUN; SUNSPOTS

Citation Formats

Oh, S., and Yi, Y., E-mail: suyeonoh@jnu.ac.kr. Variations in Solar Parameters and Cosmic Rays with Solar Magnetic Polarity. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA6C62.
Oh, S., & Yi, Y., E-mail: suyeonoh@jnu.ac.kr. Variations in Solar Parameters and Cosmic Rays with Solar Magnetic Polarity. United States. doi:10.3847/1538-4357/AA6C62.
Oh, S., and Yi, Y., E-mail: suyeonoh@jnu.ac.kr. Mon . "Variations in Solar Parameters and Cosmic Rays with Solar Magnetic Polarity". United States. doi:10.3847/1538-4357/AA6C62.
@article{osti_22663665,
title = {Variations in Solar Parameters and Cosmic Rays with Solar Magnetic Polarity},
author = {Oh, S. and Yi, Y., E-mail: suyeonoh@jnu.ac.kr},
abstractNote = {The sunspot number varies with the 11-year Schwabe cycle, and the solar magnetic polarity reverses every 11 years approximately at the solar maximum. Because of polarity reversal, the difference between odd and even solar cycles is seen in solar activity. In this study, we create the mean solar cycle expressed by phase using the monthly sunspot number for all solar cycles 1–23. We also generate the mean solar cycle for sunspot area, solar radio flux, and cosmic ray flux within the allowance of observational range. The mean solar cycle has one large peak at solar maximum for odd solar cycles and two small peaks for most even solar cycles. The odd and even solar cycles have the statistical difference in value and shape at a confidence level of at least 98%. For solar cycles 19–23, the second peak in the even solar cycle is larger than the first peak. This result is consistent with the frequent solar events during the declining phase after the solar maximum. The difference between odd and even solar cycles can be explained by a combined model of polarity reversal and solar rotation. In the positive/negative polarity, the polar magnetic field introduces angular momentum in the same/opposite direction as/to the solar rotation. Thus the addition/subtraction of angular momentum can increase/decrease the motion of plasma to support the formation of sunspots. Since the polarity reverses at the solar maximum, the opposite phenomenon occurs in the declining phase.},
doi = {10.3847/1538-4357/AA6C62},
journal = {Astrophysical Journal},
number = 1,
volume = 840,
place = {United States},
year = {Mon May 01 00:00:00 EDT 2017},
month = {Mon May 01 00:00:00 EDT 2017}
}