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Introduction

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Imaging Convection and Magnetism in the Sun

Part of the book series: SpringerBriefs in Mathematics ((BRIEFSMATH))

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Abstract

The Sun was formed roughly 4.5 billion years ago from the gravitational collapse of a gaseous cloud. The core of this cloud settled in the center, gathering an overwhelming fraction of the matter of the cloud ( ∼ 99.85%) while the rest formed a disk that would eventually turn into the solar system. Owing to gravitational forcing, the central mass gained temperature and the core, reaching a critical temperature of about 15 million K, began to undergo nuclear fusion. The present Sun is primarily composed of Hydrogen ( ∼ 71%) and Helium ( ∼ 27%), the rest being metals (in astrophysical jargon, elements other than Hydrogen and Helium are termed ‘metals’).

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  1. Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai, India

    Shravan Hanasoge

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Hanasoge, S. (2015). Introduction. In: Imaging Convection and Magnetism in the Sun. SpringerBriefs in Mathematics. Springer, Cham. https://doi.org/10.1007/978-3-319-27330-3_1

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