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Dark Matter in the Galactic Disk

Published online by Cambridge University Press:  04 August 2017

John N. Bahcall
John N. Bahcall*
Affiliation:
Institute for Advanced Study, Princeton, New Jersey 08540

Abstract

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The Poisson and Vlasov equations are solved self-consistently for realistic Galaxy models which include multiple disk components, a Population II spheroid, and an unseen massive halo. The total amount of matter in the vicinity of the Sun is determined by comparing the observed distributions of tracer stars, samples of F dwarfs and of K giants, with the predictions of the Galaxy models. Results are obtained for a number of different assumed distributions of the unseen disk mass. The major uncertainties, observational and theoretical, are estimated. For all the observed samples, typical models imply that about half of the mass in the solar vicinity must be in the form of unobserved matter. The volume density of unobserved material near the Sun is about 0.1M⊙pc−3; the corresponding column density is about 30M⊙pc−2. This so far unseen material must be in a disk with an exponential scale height of less than 0.7 kpc. If the unseen material is in the form of stars with masses less than 0.1M⊙, then the nearest such object is about 1 pc away and has a proper motion of more than 1 arcsecond per year.

Type
Review Paper
Information
Symposium - International Astronomical Union , Volume 117: Dark Matter in the Universe , 1987 , pp. 17 - 31
Copyright
Copyright © Reidel 1987 

References

Bahcall, J. N. 1984a, Ap. J. 276, 169.Google Scholar
Bahcall, J. N. 1984b, Ap. J., 287, 926.CrossRefGoogle Scholar
Bahcall, J. N. and Soneira, R. M. 1980, Ap. J. Suppl. 44, 73.CrossRefGoogle Scholar
Green, R. F. 1980, Ap. J. 238, 685.Google Scholar
Hill, E. R. 1960, Bull. Astr. Inst. Netherlands 15.Google Scholar
Hill, G., Hilditch, R.W., and Barnes, J.V. 1979, M.N.R.A.S. 186, 813.CrossRefGoogle Scholar
Lacarrieu, C.T. 1971, Astron. and Astrophys. 14, 95.Google Scholar
Liebert, J., Dahn, C. C., Gresham, M., and Strittmatter, P. A. 1979, Ap. J., 233, 226.Google Scholar
Milgrom, M. A. 1983, Ap. J. 270, 371.Google Scholar
Oort, J. H. 1932, Bull. Astr. Inst. Netherlands 6, 249.Google Scholar
Oort, J. H. 1960, Bull. Astr. Inst. Netherlands 15, 45.Google Scholar
Sanders, D. B., Solomon, P. M. and Scoville, N. Z. 1984, Ap. J. 276, 182.Google Scholar
Spitzer, L. 1978, Physical Processes in the Interstellar Medium (New York: Wiley).Google Scholar
Upgren, A. R. 1962, A. J. 67, 37.Google Scholar
Wielen, R. 1974, Highlights of Astronomy, Vol. 3, 395, ed. Contopoulos, G., (Dordrecht: D. Reidel).Google Scholar
Woolley, R. and Stewart, J. M. 1967, M.N.R.A.S. 136, 329.Google Scholar