Free Access
Issue
A&A
Volume 532, August 2011
Article Number A149
Number of page(s) 19
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201116649
Published online 09 August 2011

Online material

thumbnail Fig. 9

As in Fig. 7, model calculations for the oblate ellipsoid e = 0.7 with equatorial distribution, where the velocity in the equatorial region is twice that in the polar axis.

Open with DEXTER

thumbnail Fig. 10

As in Fig. 7, model calculations for the oblate ellipsoid (e = 0.9) with equatorial distribution,where the velocity in the equatorial region is four times higher than that in the polar axis.

Open with DEXTER

thumbnail Fig. 11

As in Fig. 7, model calculations for the prolate ellipsoid (e = 0.7) with equatorial distribution, where the velocity in the polar axis is twice than that in the equatorial plane.

Open with DEXTER

thumbnail Fig. 12

As in Fig. 7, model calculations for the prolate ellipsoid (e = 0.9) with equatorial distribution, where the velocity in the polar axis is four times higher than that in the equatorial plane.

Open with DEXTER

thumbnail Fig. 13

As in Fig. 8, model calculations for the oblate ellipsoid (e = 0.7) with biconical distribution, where the outflow velocity increases towards the equatorial plane.

Open with DEXTER

thumbnail Fig. 14

As in Fig. 8, model calculations for the oblate ellipsoid (e = 0.9) with biconical distribution, where the outflow velocity increases towards the equatorial plane.

Open with DEXTER

thumbnail Fig. 15

As in Fig. 8, model calculations for the prolate ellipsoid (e = 0.7) with biconical distribution, where the outflow velocity increases towards the polar region.

Open with DEXTER

thumbnail Fig. 16

As in Fig. 8, model calculations for the prolate ellipsoid (e = 0.9) with biconical distribution, where the outflow velocity increases towards the polar region.

Open with DEXTER


© ESO, 2011

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