Titlebook: Solar Prominences; Einar Tandberg-Hanssen Book 1974 D. Reidel Publishing Company, Dordrecht, Holland 1974 Corona.Solar prominence.Sunspot.

Incise

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Observational Data,these observations pertained mainly to the easily observed shapes and overall motions of the prominences. In this chapter we shall in more detail consider these and other data and see how they can lead to physical models of different kinds of prominences.

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Models,owing parameters. electron temperature. electron density. microturbulent velocity. macroturbulent velocity. gross (organized) velocity. characteristic length. longitudinal magnetic field. filamentary structure ratio (Equation II.21).

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Formation of Prominences,scussion of stability of prominences to Chapter V. In their prominence classification Menzel and Evans (1953) realized the important distinction between objects forming from above and objects forming from below (see Section 1.3.3). We refer to the former case as condensation, and for the latter we use the term injection.

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Frequency

Introduction, Celsius (1735) edited a report of the Swedish observations which shows that other observers agreed with Vassenius’ description (see also Grant, 1852). Ulloa (1779) observed what probably was an active prominence during the eclipse of 1778, and attributed it to a hole in the Moon.

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Introduction,ty was a prominence, and Muratori’s report is one of the earliest we have of this sign of solar activity. Medieval Russian chronicles (see Vyssotsky, 1949) also mention prominences, but the first semi-scientific description of them came after the eclipse of May 2, 1733. During this event Vassenius (

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Observational Data,these observations pertained mainly to the easily observed shapes and overall motions of the prominences. In this chapter we shall in more detail consider these and other data and see how they can lead to physical models of different kinds of prominences.