The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation
The ability to predict times of greater galactic cosmic ray (GCR) fluxes is important for reducing the hazards caused by these particles to satellite communications, aviation, or astronauts. The 11-year solar-cycle variation in cosmic rays is highly correlated with the strength of the heliospheric m...
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| Veröffentlicht in: | Solar physics 2014, Vol.289 (1), p.407-421 |
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| creator | Thomas, S. R. Owens, M. J. Lockwood, M. |
| description | The ability to predict times of greater galactic cosmic ray (GCR) fluxes is important for reducing the hazards caused by these particles to satellite communications, aviation, or astronauts. The 11-year solar-cycle variation in cosmic rays is highly correlated with the strength of the heliospheric magnetic field. Differences in GCR flux during alternate solar cycles yield a 22-year cycle, known as the Hale Cycle, which is thought to be due to different particle drift patterns when the northern solar pole has predominantly positive (denoted as
qA
>0 cycle) or negative (
qA
0 cycles than for
qA
0 and more sharply peaked for
qA |
| doi_str_mv | 10.1007/s11207-013-0341-5 |
| format | Article |
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qA
>0 cycle) or negative (
qA
<0) polarities. This results in the onset of the peak cosmic-ray flux at Earth occurring earlier during
qA
>0 cycles than for
qA
<0 cycles, which in turn causes the peak to be more dome-shaped for
qA
>0 and more sharply peaked for
qA
<0. In this study, we demonstrate that properties of the large-scale heliospheric magnetic field are different during the declining phase of the
qA
<0 and
qA
>0 solar cycles, when the difference in GCR flux is most apparent. This suggests that particle drifts may not be the sole mechanism responsible for the Hale Cycle in GCR flux at Earth. However, we also demonstrate that these polarity-dependent heliospheric differences are evident during the space-age but are much less clear in earlier data: using geomagnetic reconstructions, we show that for the period of 1905 – 1965, alternate polarities do not give as significant a difference during the declining phase of the solar cycle. Thus we suggest that the 22-year cycle in cosmic-ray flux is at least partly the result of direct modulation by the heliospheric magnetic field and that this effect may be primarily limited to the grand solar maximum of the space-age.</description><identifier>ISSN: 0038-0938</identifier><identifier>EISSN: 1573-093X</identifier><identifier>DOI: 10.1007/s11207-013-0341-5</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Astrophysics and Astroparticles ; Atmospheric Sciences ; Cosmic rays ; Fluctuations ; Magnetic fields ; Physics ; Physics and Astronomy ; Satellite communications ; Solar physics ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Sun</subject><ispartof>Solar physics, 2014, Vol.289 (1), p.407-421</ispartof><rights>Springer Science+Business Media Dordrecht 2013</rights><rights>Springer Science+Business Media Dordrecht 2014</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c349t-20122615c6d1b69c7c9a927937f3b841afad75bbd56314f45b7b3f9df561168d3</citedby><cites>FETCH-LOGICAL-c349t-20122615c6d1b69c7c9a927937f3b841afad75bbd56314f45b7b3f9df561168d3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s11207-013-0341-5$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s11207-013-0341-5$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Thomas, S. R.</creatorcontrib><creatorcontrib>Owens, M. J.</creatorcontrib><creatorcontrib>Lockwood, M.</creatorcontrib><title>The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation</title><title>Solar physics</title><addtitle>Sol Phys</addtitle><description>The ability to predict times of greater galactic cosmic ray (GCR) fluxes is important for reducing the hazards caused by these particles to satellite communications, aviation, or astronauts. The 11-year solar-cycle variation in cosmic rays is highly correlated with the strength of the heliospheric magnetic field. Differences in GCR flux during alternate solar cycles yield a 22-year cycle, known as the Hale Cycle, which is thought to be due to different particle drift patterns when the northern solar pole has predominantly positive (denoted as
qA
>0 cycle) or negative (
qA
<0) polarities. This results in the onset of the peak cosmic-ray flux at Earth occurring earlier during
qA
>0 cycles than for
qA
<0 cycles, which in turn causes the peak to be more dome-shaped for
qA
>0 and more sharply peaked for
qA
<0. In this study, we demonstrate that properties of the large-scale heliospheric magnetic field are different during the declining phase of the
qA
<0 and
qA
>0 solar cycles, when the difference in GCR flux is most apparent. This suggests that particle drifts may not be the sole mechanism responsible for the Hale Cycle in GCR flux at Earth. However, we also demonstrate that these polarity-dependent heliospheric differences are evident during the space-age but are much less clear in earlier data: using geomagnetic reconstructions, we show that for the period of 1905 – 1965, alternate polarities do not give as significant a difference during the declining phase of the solar cycle. Thus we suggest that the 22-year cycle in cosmic-ray flux is at least partly the result of direct modulation by the heliospheric magnetic field and that this effect may be primarily limited to the grand solar maximum of the space-age.</description><subject>Astrophysics and Astroparticles</subject><subject>Atmospheric Sciences</subject><subject>Cosmic rays</subject><subject>Fluctuations</subject><subject>Magnetic fields</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Satellite communications</subject><subject>Solar physics</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Sun</subject><issn>0038-0938</issn><issn>1573-093X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNp1kN9KwzAUh4MoOKcP4F3AG2-qOUmTtpdSnRMmgkxwVyFNU9fRNTNpxd35Dr6hT2LKvBDBm_MHvu9w-CF0CuQCCEkuPQAlSUSARYTFEPE9NAKehC1jz_toRAhLhzk9REferwgZLD5Ci_nSYEqjhVEOT1VjcL7VodYtzq1f1xo_qi2eNP07_vr4xDdvdWlabXBlHb6undEdnpqmtn6zNC7Q97bsG9XVtj1GB5VqvDn56WP0NLmZ59No9nB7l1_NIs3irIsoAUoFcC1KKESmE52pjCYZSypWpDGoSpUJL4qSCwZxFfMiKViVlRUXACIt2Rid7-5unH3tje_kuvbaNI1qje29hFjEnHDOREDP_qAr27s2fBcoTkDQFOJAwY7SznrvTCU3rl4rt5VA5BCb3IUtQ9hyCFvy4NCd4wPbvhj36_K_0jeU-H-t</recordid><startdate>2014</startdate><enddate>2014</enddate><creator>Thomas, S. 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J. ; Lockwood, M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c349t-20122615c6d1b69c7c9a927937f3b841afad75bbd56314f45b7b3f9df561168d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Astrophysics and Astroparticles</topic><topic>Atmospheric Sciences</topic><topic>Cosmic rays</topic><topic>Fluctuations</topic><topic>Magnetic fields</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Satellite communications</topic><topic>Solar physics</topic><topic>Space Exploration and Astronautics</topic><topic>Space Sciences (including Extraterrestrial Physics</topic><topic>Sun</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Thomas, S. R.</creatorcontrib><creatorcontrib>Owens, M. J.</creatorcontrib><creatorcontrib>Lockwood, M.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Solar physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Thomas, S. R.</au><au>Owens, M. J.</au><au>Lockwood, M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation</atitle><jtitle>Solar physics</jtitle><stitle>Sol Phys</stitle><date>2014</date><risdate>2014</risdate><volume>289</volume><issue>1</issue><spage>407</spage><epage>421</epage><pages>407-421</pages><issn>0038-0938</issn><eissn>1573-093X</eissn><abstract>The ability to predict times of greater galactic cosmic ray (GCR) fluxes is important for reducing the hazards caused by these particles to satellite communications, aviation, or astronauts. The 11-year solar-cycle variation in cosmic rays is highly correlated with the strength of the heliospheric magnetic field. Differences in GCR flux during alternate solar cycles yield a 22-year cycle, known as the Hale Cycle, which is thought to be due to different particle drift patterns when the northern solar pole has predominantly positive (denoted as
qA
>0 cycle) or negative (
qA
<0) polarities. This results in the onset of the peak cosmic-ray flux at Earth occurring earlier during
qA
>0 cycles than for
qA
<0 cycles, which in turn causes the peak to be more dome-shaped for
qA
>0 and more sharply peaked for
qA
<0. In this study, we demonstrate that properties of the large-scale heliospheric magnetic field are different during the declining phase of the
qA
<0 and
qA
>0 solar cycles, when the difference in GCR flux is most apparent. This suggests that particle drifts may not be the sole mechanism responsible for the Hale Cycle in GCR flux at Earth. However, we also demonstrate that these polarity-dependent heliospheric differences are evident during the space-age but are much less clear in earlier data: using geomagnetic reconstructions, we show that for the period of 1905 – 1965, alternate polarities do not give as significant a difference during the declining phase of the solar cycle. Thus we suggest that the 22-year cycle in cosmic-ray flux is at least partly the result of direct modulation by the heliospheric magnetic field and that this effect may be primarily limited to the grand solar maximum of the space-age.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s11207-013-0341-5</doi><tpages>15</tpages></addata></record> |
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| subjects | Astrophysics and Astroparticles Atmospheric Sciences Cosmic rays Fluctuations Magnetic fields Physics Physics and Astronomy Satellite communications Solar physics Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Sun |
| title | The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation |
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