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The Sun: New Challenges pp 83–91Cite as

Complex Magnetic Evolution and Magnetic Helicity in the Solar Atmosphere

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Part of the book series: Astrophysics and Space Science Proceedings ((ASSSP,volume 30))

Abstract

Solar atmosphere is a single system unified by the presence of large-scale magnetic fields. Topological changes in magnetic fields that occur in one place may have consequences for coronal heating and eruptions for other, even remote locations. Coronal magnetic fields also play role in transport of magnetic helicity from Sun’s subphotosphere/upper convection zone to the interplanetary space. We discuss observational evidence pertinent to some aspects of the solar corona being a global interconnected system, i.e., large-scale coronal heating due to new flux emergence, eruption of chromospheric filament resulting from changes in magnetic topology triggered by new flux emergence, sunspots rotation as manifestation of transport of helicity through the photosphere, and potential consequences of re-distribution of energy from solar luminosity to the dynamo for solar cycle variations of solar irradiance.

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Acknowledgements

National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, AURA Inc. under cooperative agreement with the National Science Foundation.

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Authors and Affiliations

  1. National Solar Observatory, 62, Sunspot, NM, 88349, USA

    Alexei A. Pevtsov

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  1. Alexei A. Pevtsov
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Correspondence to Alexei A. Pevtsov .

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Editors and Affiliations

  1. IZMIRAN, xx, Troitsk Moscow region, 142190, Russia

    Vladimir N. Obridko

  2. SSTRI-BAS, Moskovska str. 6, Sofia, 1000, Bulgaria

    Katya Georgieva

  3. Pulkovo Observatory, Pulkovskoe shausse 65/1, Saint Petersburg, 196140, Russia

    Yury A. Nagovitsyn

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Pevtsov, A.A. (2012). Complex Magnetic Evolution and Magnetic Helicity in the Solar Atmosphere. In: Obridko, V., Georgieva, K., Nagovitsyn, Y. (eds) The Sun: New Challenges. Astrophysics and Space Science Proceedings, vol 30. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-29417-4_8

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  • DOI: https://doi.org/10.1007/978-3-642-29417-4_8

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  • Print ISBN: 978-3-642-29416-7

  • Online ISBN: 978-3-642-29417-4

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