Dark Matter, Magnetic Fields, and the Rotation Curve of the Milky Way

Bibcode
2012ApJ...755L..23R
DOI
10.1088/2041-8205/755/2/L23
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
Number of authors
5
IAC number of authors
1
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.
Related projects
The Invisible Scaffolding of Space
Cosmology with Large Scale Structure Probes

The Cosmic Microwave Background (CMB) contains the statistical information about the early seeds of the structure formation in our Universe. Its natural counterpart in the local universe is the distribution of galaxies that arises as a result of gravitational growth of those primordial and small density fluctuations. The characterization of the

FRANCISCO SHU
KITAURA JOYANES
In progress
Type
Refereed
Magnetic fields
Cosmology & Astroparticles (CYA, CTA)

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