Results 191 to 200 of about 3,487 (215)
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AIP Conference Proceedings, 2004
The Sun, solar and later spectral type stars show cyclical magnetic activity that manifests itself through the presence of spots on their surfaces. The characteristics of this activity show broad variations both in spot periods, which range from a few to more than 20 years, and spot surface coverages, which range from 0.002 for the Sun to more than 0.5
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The Sun, solar and later spectral type stars show cyclical magnetic activity that manifests itself through the presence of spots on their surfaces. The characteristics of this activity show broad variations both in spot periods, which range from a few to more than 20 years, and spot surface coverages, which range from 0.002 for the Sun to more than 0.5
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The tachocline and the solar dynamo
Astronomische Nachrichten, 2005AbstractThe solar tachocline contains a rich variety of physics, and contributes in many ways to the workings of the solar dynamo. It includes complex quasi‐equilibrium states supported by the near balances of gas and magnetic pressure gradients, gravity, magnetic curvature stresses, Coriolis and other forces.
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Transactions of the International Astronomical Union, 1988
Traditionally the theory of the solar dynamo has been divided into two parts. The first, more difficult part, is the derivation of equations governing the mean magnetic field; the second, easier, is the solution of this equation, and the interpretation of the result in terms of observed solar magnetism. This report follows the traditional division.
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Traditionally the theory of the solar dynamo has been divided into two parts. The first, more difficult part, is the derivation of equations governing the mean magnetic field; the second, easier, is the solution of this equation, and the interpretation of the result in terms of observed solar magnetism. This report follows the traditional division.
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2007
In this chapter we will explain the basic MHD equations which are needed to understand solar active phenomena such as spots, prominences, flares etc.
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In this chapter we will explain the basic MHD equations which are needed to understand solar active phenomena such as spots, prominences, flares etc.
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Observationally Guided Models for the Solar Dynamo and the Role of the Surface Field
Space Science Reviews, 2023R H Cameron +2 more
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Dynamo models of the solar cycle
Living Reviews in Solar Physics, 2020Paul Charbonneau, Charbonneau Paul
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Starspots, stellar cycles and stellar flares: Lessons from solar dynamo models
Science China: Physics, Mechanics and Astronomy, 2016Arnab Rai Choudhuri
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Kinematic dynamo wave in the vicinity of the solar pole
Geophysical and Astrophysical Fluid Dynamics, 1999D D Sokoloff
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