Bibcode
Ruiz-Granados, B.; Battaner, E.; Calvo, J.; Florido, E.; Rubiño-Martín, J. A.
Bibliographical reference
The Astrophysical Journal Letters, Volume 755, Issue 2, article id. L23 (2012).
Advertised on:
8
2012
Citations
12
Refereed citations
10
Description
The study of the disk rotation curve of our Galaxy at large distances
provides an interesting scenario for us to test whether magnetic fields
should be considered as a non-negligible dynamical ingredient. By
assuming a bulge, an exponential disk for the stellar and gaseous
distributions, and a dark halo and disk magnetic fields, we fit the
rotation velocity of the Milky Way. In general, when the magnetic
contribution is added to the dynamics, a better description of the
rotation curve is obtained. Our main conclusion is that magnetic fields
should be taken into account for the Milky Way dynamics. Azimuthal
magnetic field strengths of B phi ~ 2 μG at distances of
~2 R 0(16 kpc) are able to explain the rise-up for the
rotation curve in the outer disk.
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