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Radio continuum emission from M31 and M33 | | Rainer Beck
; | | Date: |
28 Sep 2000 | | Subject: | astro-ph | | Affiliation: | Max-Planck-Institut fur Radioastronomie, Bonn, Germany | | Abstract: | The radio emission from M31 (like HI, CO, FIR and Halpha) is concentrated in the ’10 kpc ring’, giving an impressive example that cosmic rays are produced in star-forming regions. M31 and M33 have similar strengths of the total magnetic field, but very different field structures: The field structure in M31 is exceptionally regular while that in M33 is rather irregular compared with other spiral galaxies. In M33 the polarized intensity is highest between the spiral arms, similar to most spiral galaxies, while in M31 total and polarized emission both emerge from the ring. Star formation in M31 is probably too weak to tangle the regular field. The high regularity of the field in the M31 ring allows fast cosmic-ray propagation. As a consequence, there is no equipartition between the energy densities of cosmic rays and total magnetic fields. Faraday rotation measures show that the regular field in the ring is uni-directional, signature of the basic axisymmetric dynamo mode with a pitch angle of only -12 degr. Faraday rotation of polarized background sources shows that the regular field and thermal gas in M31 extend to at least 25 kpc radius. The regular field in M33 forms an open spiral, a mixture of axisymmetric and higher modes, with the largest pitch angle (simeq 60 degr) observed in any spiral galaxy so far. Vertical filaments in the NW and SE indicate interaction between the thin and the thick disk of M31. The total emission in the central region of M31 follows the spiral and radial Halpha filaments, while the polarized emission is strongest on the inner edge of the southern spiral filament. | | Source: | arXiv, astro-ph/0009455 | | Services: | Forum | Review | PDF | Favorites | |
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