New PDF release: Advances in Geophysics, Vol. 8

By H.E. Landsberg (ed.), J. Van Mieghem (ed.)

ISBN-10: 0120188082

ISBN-13: 9780120188086

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The fainter lines, however, where there is little self-absorption, are intrinsically narrow, testimony t,o their relatively low kinetic temperatures -10,000”K. A part,icularly characteristic form of quiescent prominence is the “hedgerow” prominence (see Fig. 13) which stretches out ribbon-like, somet’imes for hundreds of t,housands of kilometers. The internal structure of prominences consists of a fine network of filamentation, generally radial in orientation. Motion within prominences is generally sunward along the filamentary structure.

First recognized on interferometer records, these long-lived emissions come from a source of large extent that moves in the solar corona to heights of the order of a solar radius [45]. Radiation occurs over a broad band of frequencies at each height [43]. The identification of these events with the long-lasting continuum that sometimes follows a type I1 burst and with high intensity, long duration bursts in the centimeter range seems quite certain [46]. Probably the noise sources at low frequencies are also related to type IV events.

Lifetimes may run for as long as a few months. The quiescent prominences, when observed a t the limb, appear to be of great optical depth in their stronger spectral lines. The fainter lines, however, where there is little self-absorption, are intrinsically narrow, testimony t,o their relatively low kinetic temperatures -10,000”K. A part,icularly characteristic form of quiescent prominence is the “hedgerow” prominence (see Fig. 13) which stretches out ribbon-like, somet’imes for hundreds of t,housands of kilometers.

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Advances in Geophysics, Vol. 8 by H.E. Landsberg (ed.), J. Van Mieghem (ed.)


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