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Figure 1 | Computational Astrophysics and Cosmology

Figure 1

From: On the origin of jets from disc-accreting magnetized stars

Figure 1

Slowly/rapidly rotating stars. Schematic profiles of the midplane angular velocity of the plasma for the case of a slowly rotating star (left-hand panel) and a rapidly rotating star (right-hand panel) which is in the propeller regime. Here, Ω is the angular rotation rate of the star, Ω K is the Keplerian rotation rate of the disc, r is the star’s radius, r m is the radius of the magnetosphere, and r cr is the co-rotation radius.

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