Astronomy:Baryonic dark matter
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In astronomy and cosmology, baryonic dark matter is hypothetical dark matter composed of baryons. Only a small proportion of the dark matter in the universe is likely to be baryonic.
Characteristics
As "dark matter", baryonic dark matter is undetectable by its emitted radiation, but its presence can be inferred from gravitational effects on visible matter. This form of dark matter is composed of "baryons", heavy subatomic particles such as protons and neutrons and combinations of these, including non-emitting ordinary atoms.
Presence
Baryonic dark matter may occur in non-luminous gas or in Massive Astrophysical Compact Halo Objects (MACHOs) – condensed objects such as black holes, neutron stars, white dwarfs, very faint stars, or non-luminous objects like planets and brown dwarfs.
Estimates of quantity
The total amount of baryonic dark matter can be inferred from models of Big Bang nucleosynthesis, and observations of the cosmic microwave background. Both indicate that the amount of baryonic dark matter is much smaller than the total amount of dark matter.
Big Bang nucleosynthesis
From the perspective of Big Bang nucleosynthesis, a larger amount of ordinary (baryonic) matter implies a denser early universe, more efficient conversion of matter to helium-4, and less unburned deuterium remaining. If all of the dark matter in the universe were baryonic, then there would be much less deuterium in the universe than is observed. This could be resolved if more deuterium were somehow generated, but large efforts in the 1970s failed to identify plausible mechanisms for this to occur. For instance, MACHOs, which include, for example, brown dwarfs (bodies of hydrogen and helium with masses less than 0.08 M☉ or 1.6×1029 kg), never begin nuclear fusion of hydrogen, but they do burn deuterium. Other possibilities that were examined include "Jupiters", which are similar to brown dwarfs but have masses [math]\displaystyle{ \sim }[/math] 0.001 M☉ (2×1027 kg) and do not burn anything, and white dwarfs.[1][2][clarification needed]
See also
References
- ↑ G. Jungman; M. Kamionkowski; K. Griest (1996). "Supersymmetric dark matter". Physics Reports 267 (5–6): 195–373. doi:10.1016/0370-1573(95)00058-5. Bibcode: 1996PhR...267..195J.
- ↑ M. S. Turner (1999). "Cosmological parameters". AIP Conference Proceedings 478: 113–128. doi:10.1063/1.59381. ISBN 1563968533. Bibcode: 1999AIPC..478..113T.
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