Published December 31, 1998
by Springer .
Written in English
Edition Notes
| Contributions | Claus Fröhlich (Editor), M. Huber (Editor), S.K. Solanki (Editor), Rudolf von Steiger (Editor) |
| The Physical Object | |
|---|---|
| Format | Hardcover |
| Number of Pages | 444 |
| ID Numbers | |
| Open Library | OL7808835M |
| ISBN 10 | 0792354966 |
| ISBN 10 | 9780792354963 |
Solar composition and its evolution - from core to corona. Proceedings. ISSI (International Space Science Institute) Workshop, Bern (Switzerland), 26 - 30 Jan Author: C. Fröhlich, M. C. E. Huber, S. K. Solanki, R. von Steiger. Get this from a library! Solar composition and its evolution-- from core to corona: proceedings of an ISSI Workshop January , Bern, Switzerland. [Claus Frohlich;]. Download Solar Composition and its Evolution — from Core to Corona free pdf ebook online. Solar Composition and its Evolution — from Core to Corona is a book by Claus Fröhlich,M. Huber,S.K. Solanki,Rudolf von Steiger on Enjoy reading pages by starting download or read online Solar Composition and its Evolution — from Core. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A.
The solar corona evolves on a variety of timescales closely connected with the evolution of the coronal magnetic field. (See The Sun.)The most rapid and dramatic evolution in the corona occurs in events known as coronal mass ejections or CMEs (Figure (a)).CMEs originate in closed field regions in the corona where the magnetic field normally is sufficiently strong to constrain the coronal. The corona is the outer atmosphere of the Sun. It extends many thousands of kilometers (miles) above the visible "surface" of the Sun, gradually transforming into the solar wind that flows outward through our solar material in the corona is an extremely hot but very tenuous plasma. SOHO, the Solar and Heliospheric Observatory, is a project of international cooperation between ESA and NASA to study the Sun, from its deep core to the outer corona, and the solar wind. To achieve its scientific goals it carries a complement of twelve sophisticated, state-of-the-art instruments. However, the O isotope composition of the Sun inferred from solar winds collected by Genesis (Δ 17 O = − ± ‰, McKeegan et al., ) and the composition of A-COR core minerals are far removed the highly 17 O-rich composition of the Sun required by the models proposed by Gounelle and Meibom ().
Composition of the Sun’s Atmosphere. Let’s begin by asking what the solar atmosphere is made of. As explained in Radiation and Spectra, we can use a star’s absorption line spectrum to determine what elements are present. It turns out that the Sun contains the same elements as Earth but not in the same proportions. About 73% of the Sun’s mass is hydrogen, and another 25% is helium. as the solar wind. Figure 1 shows two different views of the corona and its collection of closed and open magnetic fields. Despite almost a century of study, the physical processes responsible for heating the corona and accelerating the solar wind are not yet understood at a fundamental level. The solar wind plasma, like the SEPs, is accelerated in the solar corona, and thus its composition is expected to agree with that of the corona, not the photosphere. Element abundances in the solar wind can be determined either by the foil collection technique,asusedontheApollomissions(Geissetal)and. Rotation of the Solar Nebula We can use the concept of angular momentum to trace the evolution of the collapsing solar nebula. The angular momentum of an object is proportional to the square of its size (diameter) divided by its period of rotation (D 2 /P).If angular momentum is conserved, then any change in the size of a nebula must be compensated for by a proportional change in period, in.
