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27-Day Modulation of Cosmic Ray Intensities During the Last Two Solar Minima

Leske, R. A. and Cummings, A. C. and Mewaldt, R. A. and Stone, E. C. and von Rosenvinge, T. T. and Wiedenbeck, M. E. (2019) 27-Day Modulation of Cosmic Ray Intensities During the Last Two Solar Minima. In: 36th International Cosmic Ray Conference (ICRC2019). Proceedings of Science. No.358. SISSA , Trieste, Italy, Art. No. 1105. https://resolver.caltech.edu/CaltechAUTHORS:20190821-075835551

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Abstract

Variations in both anomalous cosmic ray (ACR) and galactic cosmic ray (GCR) intensities at the solar rotation period (∼27 days) are often observed, and appear throughout much of 2016 into 2019 during the present A>0 polarity solar minimum. During the previous A<0 solar minimum, such variations were evident at energies from a few MeV to many GeV from mid-2007 through late 2008, and were much larger for ACRs than for GCRs at comparable energy. The particle intensities had an inverse power-law correlation with the solar wind speed, intensity peaks occurred only near alternate crossings of the heliospheric current sheet, and the variations in amplitudes were larger than typical for an A<0 epoch. The heliospheric environment was unusual compared with earlier cycles, with lower solar wind dynamic pressure, weaker interplanetary magnetic field strength, and record-setting GCR intensities. The present high-energy GCR intensities are higher than ever before reported in an A>0 cycle (although lower than in several A<0 cycles), indicating that unusual modulation conditions still prevail. Using high statistical precision measurements from the ACE spacecraft along with neutron monitor data, we present observations of the 27-day intensity variations in both ACRs and GCRs during the last two solar minima and describe how they depend on particle energy, rigidity, and spectrum, and on interplanetary conditions such as solar wind speed, magnetic field strength, andmcurrent sheet tilt. We compare the variations observed in this cycle with those in the previous opposite polarity cycle and discuss implications for particle transport in the heliosphere.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://pos.sissa.it/358/1105/PublisherArticle
ORCID:
AuthorORCID
Leske, R. A.0000-0002-0156-2414
Cummings, A. C.0000-0002-3840-7696
Mewaldt, R. A.0000-0003-2178-9111
Stone, E. C.0000-0002-2010-5462
Wiedenbeck, M. E.0000-0002-2825-3128
Additional Information:© 2019 owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License. Pre-published on: 2019 July 22. This work was supported by NASA under grant 80NSSC18K0223. We thank the ACE/SWEPAM and MAG instrument teams and the ACE Science Center (http://www.srl.caltech.edu/ACE/ASC) for making their solar wind and magnetic field data publicly available. We acknowledge the NMDB database (www.nmdb.eu), founded under the European Union's FP7 program (contract 213007) for hosting and distributing the Newark neutron monitor data from the Bartol Research Institute, supported by the NSF under grants ANT-0739620 and ANT-0838839. We thank Todd Hoeksema and the Wilcox Solar Observatory (http://wso.stanford.edu) for providing the HCS and coronal field map data.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASA80NSSC18K0223
European Research Council (ERC)213007
NSFANT-0739620
NSFANT-0838839
Series Name:Proceedings of Science
Issue or Number:358
Record Number:CaltechAUTHORS:20190821-075835551
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190821-075835551
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98059
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Aug 2019 16:24
Last Modified:09 Mar 2020 13:19

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