Death of Stellar Baryonic Dark Matter Candidates

Simple item page
dc.creatorFreese, Katherine
dc.creatorFields, Brian
dc.creatorGraff, David
dc.date2000-07-28
dc.date.accessioned2026-07-07T01:54:36Z
dc.date.available2026-07-07T01:54:36Z
dc.descriptionThe nature of the dark matter in the Universe is one of the outstanding questions in astrophysics. In this talk, I address possible stellar baryonic contributions to the 50-90% of our Galaxy that is made of unknown dark matter. First I show that faint stars and brown dwarfs constitute only a few percent of the mass of the Galaxy. Next, I show that stellar remnants, including white dwarfs and neutron stars, are also insufficient in abundance to explain all the dark matter of the Galaxy. High energy gamma-rays observed in HEGRA data place the most robust constraints, $Ω_{WD} < 3 \times 10^{-3} h^{-1}$, where $h$ is the Hubble constant in units of 100 km s$^{-1}$ Mpc$^{-1}$. Overproduction of chemical abundances (carbon, nitrogen, and helium) provide the most stringent constraints, $Ω_{WD} < 2 \times 10^{-4} h^{-1}$. Comparison with recent updates of microlensing data are also made. According to the gamma-ray limit, all Massive Compact Halo Objects seen by the experiments (Machos) can be white dwarfs if one takes the extreme numbers; however, from chemical overproduction limits, NOT all Machos can be white dwarfs. Comments on recent observations of the infrared background and of white dwarfs are also made. In conclusion, a nonbaryonic component in the Halo seems to be required.
dc.descriptioncontribution to: Sources and Detection of Dark Matter in the Universe, Marina del Rey, CA, February 2000
dc.identifierhttps://arxiv.org/abs/astro-ph/0007444
dc.identifierhttp://arxiv.org/abs/astro-ph/0007444
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/1411
dc.subjectAstrophysics
dc.titleDeath of Stellar Baryonic Dark Matter Candidates
dc.typetext

Files

Collections

arXiv