Magnetohydrodynamics in binary stars by C.G. Campbell

By C.G. Campbell

Magnetic stresses have been mentioned as a potential technique of angular momentum shipping within the improvement of accretion disc conception, within the overdue sixties and early seventies. curiosity within the function of magnetic fields in shut binary stars gradually elevated after the invention of the character of AM Herculis in 1976. The saw loss of an accretion disc and the synchronous rotation of the white dwarf advised powerful magnetic results, in line with the excessive measure of optical polarization. comparable platforms have been quickly stumbled on. facts for big magnetic fields used to be therefore present in the X-ray binary pulsars and the intermediate polar binaries, either believed to incorporate structures with in part disrupted accretion discs. A magnetically channelled wind from the most series secondary famous person has been invoked to provide an explanation for the better mass move charges saw in binaries above the interval hole, and in an evidence of the space. Magnetically encouraged winds from accretion discs were advised as contributing to the influx via removal angular momentum. Magnetism in binary stars is now a space of crucial value in stellar astrophysics. Magnetic fields are believed to playa primary function even in it sounds as if non-magnetic binaries. they supply the main possible capacity, via shear instabilities, of producing the turbulence in accretion discs essential to force the influx through the ensuing magnetic and viscous stresses.

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A near-Earth asteroid population estimate from the LINEAR survey. Science 294, 1691–1693. The nature of the near-Earth object population 21 Tedesco, E. F. 1994. Asteroid albedos and diameters. In Asteroids, Comets, Meteorites, eds. A. Milani, M. DiMartino, and A. Cellino, pp. 55–74. London, UK : Kluwer. Weissman, P. R. 1990. The cometary impactor flux at Earth. In Global Catastrophes in Earth History, eds. V. L. Sharpton and P. D. Ward, pp. 171–180. Boulder, CO: Geological Society of America. Weissman, P.

Meteor. and Planet. Sci. 33, 999–1016. Morbidelli, A. and Nesvorny, D. 1999. Numerous weak resonances drive asteroids toward terrestrial planets’ orbits. Icarus 139, 295–308. , Bottke, W. , et al. 2002a. From magnitudes to diameters: the albedo distribution of near-Earth objects and the Earth collision hazard. Icarus 158, 329–342. , Bottke, W. , et al. 2002b. Origin and evolution of near-Earth objects. In Asteroids III, eds. W. F. Bottke, A. Cellino, P. Paolicchi, and R. P. Binzel, pp. 409–422.

This last conversion is now possible thanks to the sharp correlation between bulk density and taxonomic class (for a review of asteroid bulk density measurements, see Britt et al. 2002). 3 g cm−3 . Ultimately, the coupled knowledge of the NEOs’ mass distribution and orbital distribution would allow us to compute the collision rate as a function of collision energy, on the Earth and on the other planets. This work is essential to interpreting the cratering record of planetary surfaces as well as to quantify the hazard represented by the NEO population for our civilization.

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Magnetohydrodynamics in binary stars by C.G. Campbell
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