Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 755, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/755/2/L23
Keywords
Galaxy: kinematics and dynamics; magnetic fields
Categories
Funding
- Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2007-67625-C02-02, AYA2011-24728, AYA2010-21766-C03-02, CSD2010-00064, MTM2008-05271]
- Junta de Andalucia Grant [FQM-108, FQM-316]
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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 similar to 2 mu G at distances of similar to 2 R-0 (16 kpc) are able to explain the rise-up for the rotation curve in the outer disk.
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