Titlebook: Baryonic Dark Matter; D. Lynden-Bell,G. Gilmore Book 1990 Kluwer Academic Publishers 1990 Dark matter.Gravity.Universe.black hole.black ho

cardiovascular

Index for 2.2 (System No., References),d theoretical progress been made in understanding the nature of these objects. With the advent of more powerful instruments such as the Hubble Space Telescope, a wealth of new observational information will be forthcoming. Thus it is imperative that refinements to theoretical models keep pace with t

white-matter

Cervical-Spine

Index for 2.1 (System No., References),cal luminosity functions for both disk and halo white dwarfs, based on those diagrams, are then described. We conclude that faint, still undetected white dwarfs are unlikely to be major contributors to baryonic dark matter, neither in the disk nor in the halo of the Galaxy.

文字

Index for 2.1 (System No., References),apse of massive stars and reveal themselves as pulsars for perhaps a few million years before they fade into obscurity, unless they are given a further burst of life by accretion of external material. In this case we may see them as low-mass X-ray binary systems and then millisecond pulsars or else

avulsion

Index for 2.2 (System No., References),binary evolution is described and illustrated for simple binary star birthrate models. Owing to selection effects, the physics of the evolving distribution, and the paucity of well-selected data, I unfortunately conclude that no limits on the mass of dark objects are yet possible. Finally, I present

Enliven

condone

Index for 2.2 (System No., References),ating in the inner parts of the galaxy, while dark matter dominates beyond the optical radius. The mass-to-light ratio of the luminous material, corrected for variations in the present rate of star formation, is remarkably constant and in agreement with classical population synthesis models. Rotatio

cyanosis

Index for 2.1 (System No., References),bably massive black holes, which lurk at the . of such normal galaxies as M31, and perhaps even our own. This subject is approached historically by considering the cosmic history of the quasar population. The evidence for massive black holes in the centres of some nearby galaxies is reviewed. Some i

PRE

Index for 2.2 (System No., References), of ~ 100 . . . and greater. The cooled product is not yet observed but is proposed to be some form of low-mass star (perhaps brown dwarf or even jupiter-mass objects). Cooling flows must form baryonic dark matter. A scenario for low-mass star formation in a cooling flow is presented here. The main

VOK