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Published online by Cambridge University Press: 04 August 2017
We use a three-component model of a spiral galaxy, given by (Huang et al., 1979):
1. An outer halo with a gravitational potential of the form
where R2 = x2 + y2 + z2, M1 = 1.2 × 1011M⊙ and b1 = 1.1 Kpc.
2. A nucleus, with a gravitational potential given by
where M0 = 1.1 × 107M⊙, and b0 = 0.61 × 10−2 Kpc.
3. A self-gravitating disk containing N stars. The density distribution in the z-direction is assumed to be:
where α = 2.1 Kpc−1 is the equivalent semi-thickness of the galaxy, and σ(r) is the surface density. We consider three different initial expressions for σ(r):
i. A Toomre (1963) disk.
ii. A uniform distribution.
iii. An exponential distribution.
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