dc.contributor.author |
Chatterjee, S |
|
dc.date.accessioned |
2008-07-01T11:09:04Z |
|
dc.date.available |
2008-07-01T11:09:04Z |
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dc.date.issued |
1995-06 |
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dc.identifier.citation |
A&A, Vol. 298, No. 2, pp. 438 - 444 |
en |
dc.identifier.issn |
0004-6361 |
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dc.identifier.uri |
http://hdl.handle.net/2248/2567 |
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dc.description.abstract |
We present here rigourous analytical solutions of the Boltzmann-Poisson equations concerning the distribution of stars perpendicular to the galactic plane. The number density of stars at the galactic disk is assumed to follow n(m,0)~H(m-m_0_)m^-x^, where m is the mass of the star and x is an arbitrary exponent greater than 2, while H(m-m_0_) is the unit Heaviside step function. The velocity dispersion of the stars is assumed to arise from the stellar motion in a random force field - leading to <v^2^(m)>~constant for m<=m_*_, <v^2^(m)>~m^-θ^, for m>m_*_, where m_*_ is the stellar mass for which the stellar life-time equals the galactic age. It is seen that the height distribution of stars is very sensitive to the values of x and θ. Finally we have derived an expression connecting the surface density volume density and velocity dispersion of stars, and show that this relation is a sensitive function of θ and x and use them to obtain certain plausible numbers for our Galaxy in the limits of the present day data. |
en |
dc.format.extent |
1008991 bytes |
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dc.format.mimetype |
application/pdf |
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dc.language.iso |
en |
en |
dc.publisher |
EDP Sciences |
en |
dc.relation.uri |
http://adsabs.harvard.edu/abs/1995A%26A...298..438C |
en |
dc.subject |
Stars: Rotation |
en |
dc.subject |
Galaxy: Kinematics And Dynamics |
en |
dc.subject |
Galaxy: Stellar Content |
en |
dc.title |
Distribution of stars perpendicular to the plane of the Galaxy. II. |
en |
dc.type |
Article |
en |