Magnetic fluctuations and formation of large-scale inhomogeneous magnetic structures
... Turbulence may form inhomogeneous large-scale magnetic fields due to turbulent diamagnetic and paramagnetic effects 共see, e.g., 关3,24–28兴兲. Inhomogeneous velocity fluctuations lead to a transport of mean magnetic flux from regions with a high intensity of velocity fluctuations. Inhomogeneous magneti ...
... Turbulence may form inhomogeneous large-scale magnetic fields due to turbulent diamagnetic and paramagnetic effects 共see, e.g., 关3,24–28兴兲. Inhomogeneous velocity fluctuations lead to a transport of mean magnetic flux from regions with a high intensity of velocity fluctuations. Inhomogeneous magneti ...
The First Galaxies: Assembly under Radiative Feedback from the
... heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos with virial temperatures . 104 K, suppressing star formation in both minihalos and the first atomic cooling halos (e.g., Thoul & Weinberg 1996; Barkana & Loeb 199 ...
... heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos with virial temperatures . 104 K, suppressing star formation in both minihalos and the first atomic cooling halos (e.g., Thoul & Weinberg 1996; Barkana & Loeb 199 ...
Magnetism in Isolated and Binary White Dwarfs
... be constructed and stellar parameters deduced. Fundamental properties, such as their mass function and interior chemical composition, are now well established and have been invaluable in constraining the theory of single star evolution (Koester & Chanmugam 1990). Parallel progress in our understandi ...
... be constructed and stellar parameters deduced. Fundamental properties, such as their mass function and interior chemical composition, are now well established and have been invaluable in constraining the theory of single star evolution (Koester & Chanmugam 1990). Parallel progress in our understandi ...
