New PDF release: Accretion Disks and Magnetic Fields in Astrophysics:

By G. Belvedere (auth.), G. Belvedere (eds.)

`It is that this element that makes this e-book specific value to excessive strength astrophysicists.'
Space technological know-how overview 56, 1991

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Read Online or Download Accretion Disks and Magnetic Fields in Astrophysics: Proceedings of the European Physical Society Study Conference, Held in Noto (Sicily), Italy, June 16–21, 1988 PDF

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Additional resources for Accretion Disks and Magnetic Fields in Astrophysics: Proceedings of the European Physical Society Study Conference, Held in Noto (Sicily), Italy, June 16–21, 1988

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1989). Thus the Sun's magnetic activity can indeed by regarded as typical of a middle-aged late-type star (Soderb10m & Baliunas 1988). On the other hand, young and rapidly rotating stars show much more irregular behaviour, which may include apparent periodicities. Starspots may cover a large fraction of their area, producing significant reductions in luminosity, while weaker magnetic fields extend over substantial patches on their surfaces (cf. Toner & Gray 1988), though both chromospheric Ca+ emission and coronal X-ray emission apparently saturate as the scaled rotation rate a increases.

Newly obtained results from helioseismology have upset our preconceptions about the internal rotation of the Sun. Solar p-modes of degree I and order m, with periods around 5 minutes, have frequencies Vl m ; in the absence of rotation Vl m is virtually independent of m but rotational splitting removes this degeneracy. The earliest results, for sectoral modes with Iml = I, supplied information about the angular velo city O(r, 'Ir /2) in the equatorial plane (Duvall & Harvey 1984; Duvall et al. 1984; Brown 1985; Libbrecht 1986).

Nature 287, 616-617. A. 1982 The overshoot layer at the base of the solar convective zone and the problem of magnetic flux storage. Astron. Astrophys. 113, 99-112. O. A. ABSTRACT. We consider two-dimensional nonlinear magnetohydrodynamic (MHD) waves of global scale for a thin magnetofluid layer on the surface of a rotating sphere. The fluid motions are assumed to be incompressible and the radial dimension is assumed to be in magnetohydrostatic balance. We are interested in a parameter regime in which horizontal spatial scales of wave motions, rotation rate of the background atmosphere, and the background zonal magnetic field strength are such that Rossby and Alfven wave speeds are comparable.

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