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Accretion Disks and Magnetic Fields in Astrophysics: by G. Belvedere (auth.), G. Belvedere (eds.)

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

`It is that this point that makes this booklet specific value to excessive power astrophysicists.'
Space technology evaluate 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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The M stars include the rapidly rotating and highly active dMe (or BY Draconis) stars with chromospheric Ha emission but older, more sedate M dwarfs still show signs of magnetic activity. Since late M stars are fully convective any dynamo must operate within their convective zones. Yet there is no convincing evidence for an abrupt change in their magnetic properties (Giampapa & Liebert 1986; Giampapa 1987). Next we can attempt to identify the processes responsible for equilibration in nonlinear stellar dynamos.

B = [v(D - 1)J2 exp (it)/D , Wo = -(1 - l/D) (9) wh ich is stable for all D. Setting Wo = 0, on the other hand, yields a sixthorder system describing dynamo action limited by torsional waves. Once again there is a nonlinear periodic solution but this solution becomes unstable for v < 1; successive bifurcations lead to quasiperiodic and eventually to chaotic motion. It is possible to derive a reduced flfth-order system describing the modulation of the basic cyde (Jones, Weiss & Cattaneo 1985), which is illustrated in Figure 4 for D = 8.

1984; Brown 1985; Libbrecht 1986). 1 days: this is equal to the period derived from magnetic features (Snodgrass 1983; Howard 1984) which is ab out 2% less than the period obtained from photospheric Doppler measurements (Snodgrass 1984). The angular velocity deduced from sectoral modes remains constant through the convection zone and then drops by around 7%. 6R 0 though there is some evidence for a rapidly rotating core from modes with I :::; 2 (Duvall & Harvey 1984). Recent measurements of rotational splitting for tesseral mo des with Iml :::; I have been inverted to give the latitudinal variation of O.

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