Solar and Stellar Magnetic Activity

Noyes, Robert W.

doi:10.1007/978-94-009-5255-3_4

Robert W. Noyes⁵

Part of the book series: Geophysics and Astrophysics Monographs ((GAAM,volume 26))

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Abstract

The Sun is a magnetic star, and almost all of the solar surface phenomena which attract the interest of Solar Physicists are influenced or even dominated by its magnetic fields. The list of such phenomena includes sunspots, pores, plages, the photospheric and chromospheric network, spicules, prominences, coronal loops, coronal rays and streamers, coronal holes, the solar wind, and many others. Solar magnetic variability gives rise to time-varying phenomena on scales from seconds to millennia, including flares, magneto- hydrodynamic waves, photospheric flux emergence, growth and decay of magnetic regions, the sunspot cycle, and long-term variations in cycle amplitude such as the Maunder Minimum. Even the solar luminosity appears to be controlled by the magnetic field.

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Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, 02138, USA
Robert W. Noyes

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Center for Space Science and Astrophysics, Stanford University, Stanford, California, USA
Peter A. Sturrock
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado, USA
Thomas E. Holzer & Dimitri M. Mihalas &
Astronomy Department, University of California, Los Angeles, California, USA
Roger K. Ulrich

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Noyes, R.W. (1986). Solar and Stellar Magnetic Activity. In: Sturrock, P.A., Holzer, T.E., Mihalas, D.M., Ulrich, R.K. (eds) Physics of the Sun. Geophysics and Astrophysics Monographs, vol 26. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5255-3_4

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DOI: https://doi.org/10.1007/978-94-009-5255-3_4
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