Issue |
A&A
Volume 424, Number 3, September IV 2004
|
|
---|---|---|
Page(s) | 761 - 764 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20040192 | |
Published online | 06 September 2004 |
Modelling the rotational curves of spiral galaxies with a scalar field
Service d'Astrophysique, C.E. Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: mbelek@discovery.saclay.cea.fr
Received:
6
June
2003
Accepted:
26
May
2004
In a previous work (Mbelek 1998), we modelled the
rotation curves (RC) of spiral galaxies by including in the equation of motion
of the stars the dynamical terms from an external real self-interacting scalar
field, ψ, minimally coupled to gravity and which respects the equivalence
principle in the weak fields and low velocity approximation. This model
appeared to have three free parameters: the turnover radius, r0, the
maximum tangential velocity, , plus a
strictly positive integer, n. Here, we propose a new improved version where
the coupling of the ψ-field to dark matter is emphasized at the expense of
its self-interaction. This reformulation presents the very advantageous
possibility that the same potential is used for all galaxies. Using at the same time a quasi-isothermal dark matter density and the scalar
field helps to better fit the RC of spiral galaxies. In addition, new
correlations are established.
Key words: cosmology: theory / cosmology: dark matter / galaxies: kinematics and dynamics
© ESO, 2004
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