The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints?
In 1844 Schwabe discovered that the number of sunspots increased and decreased over a period of about 11 years, that variation became known as the sunspot cycle. Almost eighty years later, Hale described the nature of the Sun's magnetic field, identifying that it takes about 22 years for the Su...
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Frontiers Media S.A.
2018-11-01
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| Series: | Frontiers in Astronomy and Space Sciences |
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| Online Access: | https://www.frontiersin.org/article/10.3389/fspas.2018.00038/full |
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| author | Abhishek K. Srivastava Scott W. McIntosh N. Arge Dipankar Banerjee Mausumi Dikpati Bhola N. Dwivedi Madhulika Guhathakurta B.B. Karak B.B. Karak Robert J. Leamon Robert J. Leamon Shibu K. Matthew Andres Munoz-Jaramillo D. Nandy Aimee Norton L. Upton S. Chatterjee Rakesh Mazumder Yamini K. Rao Rahul Yadav |
| author_facet | Abhishek K. Srivastava Scott W. McIntosh N. Arge Dipankar Banerjee Mausumi Dikpati Bhola N. Dwivedi Madhulika Guhathakurta B.B. Karak B.B. Karak Robert J. Leamon Robert J. Leamon Shibu K. Matthew Andres Munoz-Jaramillo D. Nandy Aimee Norton L. Upton S. Chatterjee Rakesh Mazumder Yamini K. Rao Rahul Yadav |
| author_sort | Abhishek K. Srivastava |
| collection | DOAJ |
| description | In 1844 Schwabe discovered that the number of sunspots increased and decreased over a period of about 11 years, that variation became known as the sunspot cycle. Almost eighty years later, Hale described the nature of the Sun's magnetic field, identifying that it takes about 22 years for the Sun's magnetic polarity to cycle. It was also identified that the latitudinal distribution of sunspots resembles the wings of a butterfly—showing migration of sunspots in each hemisphere that abruptly start at mid-latitudes (about ±35o) toward the Sun's equator over the next 11 years. These sunspot patterns were shown to be asymmetric across the equator. In intervening years, it was deduced that the Sun (and sun-like stars) possess magnetic activity cycles that are assumed to be the physical manifestation of a dynamo process that results from complex circulatory transport processes in the star's interior. Understanding the Sun's magnetism, its origin and its variation, has become a fundamental scientific objective—the distribution of magnetism, and its interaction with convective processes, drives various plasma processes in the outer atmosphere that generate particulate, radiative, eruptive phenomena, and shape the heliosphere. In the past few decades, a range of diagnostic techniques have been employed to systematically study finer scale magnetized objects, and associated phenomena. The patterns discerned became known as the “Extended Solar Cycle” (ESC). The patterns of the ESC appeared to extend the wings of the activity butterfly back in time, nearly a decade before the formation of the sunspot pattern, and to much higher solar latitudes. In this short review, we describe their observational patterns of the ESC and discuss possible connections to the solar dynamo as we depart on a multi-national collaboration to investigate the origins of solar magnetism through a blend of archived and contemporary data analysis with the goal of improving solar dynamo understanding and modeling. |
| first_indexed | 2024-12-10T11:52:25Z |
| format | Article |
| id | doaj.art-65cbb81bdb034ac1a604775b78363008 |
| institution | Directory Open Access Journal |
| issn | 2296-987X |
| language | English |
| last_indexed | 2024-12-10T11:52:25Z |
| publishDate | 2018-11-01 |
| publisher | Frontiers Media S.A. |
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| series | Frontiers in Astronomy and Space Sciences |
| spelling | doaj.art-65cbb81bdb034ac1a604775b783630082022-12-22T01:49:52ZengFrontiers Media S.A.Frontiers in Astronomy and Space Sciences2296-987X2018-11-01510.3389/fspas.2018.00038414817The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints?Abhishek K. Srivastava0Scott W. McIntosh1N. Arge2Dipankar Banerjee3Mausumi Dikpati4Bhola N. Dwivedi5Madhulika Guhathakurta6B.B. Karak7B.B. Karak8Robert J. Leamon9Robert J. Leamon10Shibu K. Matthew11Andres Munoz-Jaramillo12D. Nandy13Aimee Norton14L. Upton15S. Chatterjee16Rakesh Mazumder17Yamini K. Rao18Rahul Yadav19Department of Physics, Indian Institute of Technology (BHU), Varanasi, IndiaHigh Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, United StatesHeliophysics Division, NASA Goddard Space Flight Center, Greenbelt, MD, United StatesIndian Institute of Astrophysics, Bangalore, IndiaHigh Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, United StatesDepartment of Physics, Indian Institute of Technology (BHU), Varanasi, IndiaNASA Headquarters, Washington, DC, United StatesDepartment of Physics, Indian Institute of Technology (BHU), Varanasi, IndiaHigh Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, United StatesHeliophysics Division, NASA Goddard Space Flight Center, Greenbelt, MD, United StatesDepartment of Astronomy, University of Maryland, College Park, MD, United StatesUdaipur Solar Observatory, Physical Research Laboratory, Udaipur, IndiaSouthwest Research Institute, Boulder, CO, United StatesCenter of Excellence in Space Sciences India, IISER, Kolkata, India0Hansen Experimental Physics Laboratory (HEPL), Stanford University, Stanford, CA, United StatesHigh Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, United StatesIndian Institute of Astrophysics, Bangalore, IndiaCenter of Excellence in Space Sciences India, IISER, Kolkata, IndiaDepartment of Physics, Indian Institute of Technology (BHU), Varanasi, IndiaUdaipur Solar Observatory, Physical Research Laboratory, Udaipur, IndiaIn 1844 Schwabe discovered that the number of sunspots increased and decreased over a period of about 11 years, that variation became known as the sunspot cycle. Almost eighty years later, Hale described the nature of the Sun's magnetic field, identifying that it takes about 22 years for the Sun's magnetic polarity to cycle. It was also identified that the latitudinal distribution of sunspots resembles the wings of a butterfly—showing migration of sunspots in each hemisphere that abruptly start at mid-latitudes (about ±35o) toward the Sun's equator over the next 11 years. These sunspot patterns were shown to be asymmetric across the equator. In intervening years, it was deduced that the Sun (and sun-like stars) possess magnetic activity cycles that are assumed to be the physical manifestation of a dynamo process that results from complex circulatory transport processes in the star's interior. Understanding the Sun's magnetism, its origin and its variation, has become a fundamental scientific objective—the distribution of magnetism, and its interaction with convective processes, drives various plasma processes in the outer atmosphere that generate particulate, radiative, eruptive phenomena, and shape the heliosphere. In the past few decades, a range of diagnostic techniques have been employed to systematically study finer scale magnetized objects, and associated phenomena. The patterns discerned became known as the “Extended Solar Cycle” (ESC). The patterns of the ESC appeared to extend the wings of the activity butterfly back in time, nearly a decade before the formation of the sunspot pattern, and to much higher solar latitudes. In this short review, we describe their observational patterns of the ESC and discuss possible connections to the solar dynamo as we depart on a multi-national collaboration to investigate the origins of solar magnetism through a blend of archived and contemporary data analysis with the goal of improving solar dynamo understanding and modeling.https://www.frontiersin.org/article/10.3389/fspas.2018.00038/fullSun: magnetismSun: interiorSun: rotationsolar cyclesunspots |
| spellingShingle | Abhishek K. Srivastava Scott W. McIntosh N. Arge Dipankar Banerjee Mausumi Dikpati Bhola N. Dwivedi Madhulika Guhathakurta B.B. Karak B.B. Karak Robert J. Leamon Robert J. Leamon Shibu K. Matthew Andres Munoz-Jaramillo D. Nandy Aimee Norton L. Upton S. Chatterjee Rakesh Mazumder Yamini K. Rao Rahul Yadav The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? Frontiers in Astronomy and Space Sciences Sun: magnetism Sun: interior Sun: rotation solar cycle sunspots |
| title | The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? |
| title_full | The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? |
| title_fullStr | The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? |
| title_full_unstemmed | The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? |
| title_short | The Extended Solar Cycle: Muddying the Waters of Solar/Stellar Dynamo Modeling or Providing Crucial Observational Constraints? |
| title_sort | extended solar cycle muddying the waters of solar stellar dynamo modeling or providing crucial observational constraints |
| topic | Sun: magnetism Sun: interior Sun: rotation solar cycle sunspots |
| url | https://www.frontiersin.org/article/10.3389/fspas.2018.00038/full |
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