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Magnetic Coupling between the Interior and Atmosphere of the Sun pp 141–149Cite as

Probability Density Functions to Represent Magnetic Fields at the Solar Surface

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

Abstract

Numerical simulations of magneto-convection and analysis of solar magnetogram data provide empirical probability density functions (PDFs) for the line-of-sight component of the magnetic field. In this paper, we theoretically explore effects of several types of PDFs on polarized Zeeman line formation. We also propose composite PDFs to account for randomness in both field strength and orientation. Such PDFs can possibly mimic random fields at the solar surface.

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Author information

Authors and Affiliations

  1. Indian Institute of Astrophysics, Koramangala, Bangalore, 560 034, India

    M. Sampoorna

Authors
  1. M. Sampoorna
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Editor information

Editors and Affiliations

  1. Indian Institute of Astrophysics, Sarjapur Road, Bangalore, 560034, India

    S. Hasan

  2. Princetonplein 5, Utrecht, 3584 CC, Netherlands

    R. J. Rutten

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Sampoorna, M. (2010). Probability Density Functions to Represent Magnetic Fields at the Solar Surface. In: Hasan, S., Rutten, R. (eds) Magnetic Coupling between the Interior and Atmosphere of the Sun. Astrophysics and Space Science Proceedings. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-02859-5_10

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  • DOI: https://doi.org/10.1007/978-3-642-02859-5_10

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  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-642-02858-8

  • Online ISBN: 978-3-642-02859-5

  • eBook Packages: Physics and AstronomyPhysics and Astronomy (R0)

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