✦ LIBER ✦

Prominence fine structure

✍ Scribed by J. B. Zirker; S. Koutchmy

Publisher: Springer
Year: 1990
Tongue: English
Weight: 747 KB
Volume: 127
Category: Article
ISSN: 0038-0938
DOI: 10.1007/bf00158516

No coin nor oath required. For personal study only.

✦ Synopsis

The vertical fine structure in a quiescent prominence was modelled as an assembly of very narrow, optically thin threads. Random clusterings of the threads can account for the observed contrast and He line profiles of the fine structures. In this picture, each structure consists of a cluster of 7-20 elementary threads.

📜 SIMILAR VOLUMES

Prominence fine structure II: Diagnostic

Prominence fine structure II: Diagnostics

✍ J. B. Zirker; S. Koutchmy 📂 Article 📅 1991 🏛 Springer 🌐 English ⚖ 608 KB

A random-clustering model of prominence fine-structure has been applied to observations of prominence Ha spectra. The model yields an estimate of the number of unresolved elements that form an individual resolved feature, and sets limits on their velocity and Ha profile dispersions.

The fine structure of prominences

✍ Oddbjørn Engvold 📂 Article 📅 1976 🏛 Springer 🌐 English ⚖ 727 KB

The fine structure of prominences

✍ O. Engvold; J. McKim Malville 📂 Article 📅 1977 🏛 Springer 🌐 English ⚖ 354 KB

Faint, Doppler shifted, emission features are detected in high resolution spectra of limb prominences. Their average line-of-sight velocity is about 3 x 106 cm s i, their average life time is 300 s, and their angular sizes are ~<10 s cm in our spectrograms. The emission line width of the spectral fe

The fine structure of prominences

✍ J. McKim Malville 📂 Article 📅 1976 🏛 Springer 🌐 English ⚖ 207 KB

Fine structure observation in a solar pr

Fine structure observation in a solar prominence

✍ P. Lemaire; D. Samain; J.C. Vial 📂 Article 📅 1990 🏛 Elsevier Science 🌐 English ⚖ 309 KB

Dynamical fine structure of a quiescent

Dynamical fine structure of a quiescent prominence

✍ P. Mein; N. Mein 📂 Article 📅 1991 🏛 Springer 🌐 English ⚖ 931 KB

A quiescent prominence has been observed with the MSDP spectrograph at the Pic du Midi Observatory. He profiles are obtained simultaneously in a 2D field, allowing a statistical analysis. The standard deviations of Doppler shifts and line widths are investigated as functions of the line intensity. T