X-ray emission from dark clusters of MACHOs
| dc.creator | De Paolis, F. | |
| dc.creator | Ingrosso, G. | |
| dc.creator | Jetzer, Ph. | |
| dc.creator | Roncadelli, M. | |
| dc.date | 1997-09-05 | |
| dc.date.accessioned | 2026-07-07T06:21:17Z | |
| dc.date.available | 2026-07-07T06:21:17Z | |
| dc.description | MACHOs (Massive Astrophysical Compact Halo Objects) - as discovered by microlensing experiments towards the LMC - provide a natural explanation for the galactic halo dark matter. A realistic possibility is that MACHOs are brown dwarfs of mass $\sim 0.1 M_{\odot}$. Various arguments suggest that brown dwarfs should have a coronal X-ray emission of $\sim 10^{27}$ erg s$^{-1}$. As MACHOs are presumably clumped into dark clusters (DCs), each DC is expected to have a total X-ray luminosity of $\sim 10^{29}-10^{32}$ erg s$^{-1}$. We discuss the possibility that dark clusters contribute to the diffuse X-ray background (XRB) or show up as discrete sources in very deep field X-ray satellite observations. Moreover, from the observed diffuse XRB we infer that the amount of virialized diffuse gas present in the galactic halo can at most make up 5% of the halo dark matter. | |
| dc.description | Latex file with 2 figures. Accepted for publication in Astronomy and Astrophysics | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9709052 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9709052 | |
| dc.identifier | Astron.Astrophys. 329 (1998) 74 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/95553 | |
| dc.subject | Astrophysics | |
| dc.title | X-ray emission from dark clusters of MACHOs | |
| dc.type | text |