Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-12T14:27:39.521Z Has data issue: false hasContentIssue false
  • English
  • Français

Shells around Tumbling Bars: The Mass Distribution Around NGC 3923

Published online by Cambridge University Press:  04 August 2017

Ch. Dupraz ,
F. Combes  and
J.-L. Prieur
Ch. Dupraz
Affiliation:
Physikalisches Institut, Universität Köln, West Germany Observatoire de Meudon, F–92190 Meudon, France Ecole Normale Supérieure, F–75005, Paris, France
F. Combes
Affiliation:
Observatoire de Meudon, F–92190 Meudon, France Ecole Normale Supérieure, F–75005, Paris, France
J.-L. Prieur
Affiliation:
Mt. Stromlo Observatory, ACT 2606, Canberra, Australia

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In previous articles (Dupraz & Combes, 1985, 1986a), we showed that shells form with different geometries around prolate and oblate galaxies. However, theory and observations suggest that some ellipticals could be tumbling bars (Miller & Smith 1980; Müllenhoff & Marenbach 1986). Here we simulate the accretion of a small galaxy by a tumbling bar; the tumble period T& is kept free. Let Tp be the typical period of motion of a particle in the potential of the elliptical galaxy. Then we find (Dupraz & Combes, 1986b):

a) When Tt > 3TP (Figure l a), shells form with the geometry of a static prolate potential, i.e., aligned with the major axis.

When Tb < 3Tp (Figure lc), the particles feel the time-averaged potential, which is oblate: the shells display the typical oblate geometry. But there is no confusion with a static oblate shell galaxy, because the tumbling bars must be seen edge -on for the shells to appear.

c) When Tb ~ 3Tp (Figure lb), the outer shells form with the oblate geometry, the inner shells with the prolate geometry. In between, no shells form, because particles follow resonant (non-radial) motions.

Type
Posters
Information
Symposium - International Astronomical Union , Volume 127: Structure and Dynamics of Elliptical Galaxies , 1987 , pp. 469 - 470
Copyright
Copyright © Reidel 1987 

References

REFERENCES

Dupraz, C. & Combes, F., 1985. In New Aspects of Galaxy Photometry , ed. Nieto, J.-L., Lecture Notes in Physics, Springer Verlag, Berlin, p. 151.Google Scholar
Dupraz, C. & Combes, F., 1986a, b, c Astr. Astrophys., preprints.Google Scholar
Dupraz, C., Combes, F. & Gerhard, O.E., 1986. Preprint.Google Scholar
Hernquist, L. & Quinn, P.J., 1986. Astrophys. J., in press.Google Scholar
Milgrom, M., 1983. Astrophys. J., 270, 365, 371.Google Scholar
Miller, R.H. & Smith, B.F., 1980. Astrophys. J., 235, 793.Google Scholar
Möllenhoff, C. & Marenbach, G., 1986. Astr. Astrophys., 154, 219.Google Scholar
Prieur, J.-L., Fort, B., et al., 1986. Astr. Astrophys., preprint.Google Scholar
Sanders, R.H., 1984. Astr. Astrophys., 136, L21.Google Scholar
Sanders, R.H., 1986. Mon. Not. R. astr. Soc., 223. 539.Google Scholar