By Jose Afonso, Nuno Santos, Andre Moitinho, Rui Agostinho
Read Online or Download 2005: Past Meets Present in Astronomy And Astrophysics: Proceedings of the 15th Portuguese National Meeting PDF
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Extra resources for 2005: Past Meets Present in Astronomy And Astrophysics: Proceedings of the 15th Portuguese National Meeting
Spectroscopy (MOS, VLT) was carried out with R = 500 in [4450-8650] A. The data were reduced according to standard procedures using IRAF. We obtained 73 galaxy spectra for CL0048-2942 and 68 spectra for both CL2245-3954 and CL22493958. Redshifts were measured according to the Tonry & Davis technique 11 . 64. 65. 56, from a total of 54 measured redshifts. 3. Stellar population synthesis We have used a population synthesis analysis to determine the stellar content (or evolutionary stage) of cluster galaxies at different radial distances from the cluster centre.
0 - „°°*' * Oo 0 ' Figure 2. Sketch of the third quadrant of the Galactic plane. Open squares: clusters from our sample. Filled triangles: BPs. Open circles: CO clouds. Starred symbols: BPs from other studies, taken as evidence for the CMa galaxy. Large filled square: position of the CMa over-density. Filled circles: Open and globular clusters suggested to be possibly associated to CMa. Sun is at (0,0). Directions of Galactic Centre and rotation are indicated by arrows. Dotted circles mark two constant heliocentric distances (5 and 10 kpc).
We find that the coronal magnetic field rapidly expands to regions of low magnetic pressure creating a relatively smooth magnetic field with no memory of the surface radial field latitudinal distribution. Thus, our results indicate that this effect does not determine a reduction in the efficiency of magnetic braking. 1. Introduction Magnetic braking by a wind is based on the principle that when gas emitted from a star is kept corotating with the star by magnetic torques, it will transport significantly more angular momentum outwards than gas that conserves its angular momentum .