Observational consequences of baryonic gaseous dark matter

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dc.creatorShchekinov, Yu. A.
dc.date1998-11-27
dc.date1998-12-03
dc.date.accessioned2026-07-07T02:29:19Z
dc.date.available2026-07-07T02:29:19Z
dc.descriptionPossible observational consequences of dark matter in the Galaxy in the form of dense molecular gas clouds - clumpuscules of masses $M_c\sim 10^{-3} \msun$ and radii $R_c\sim 3\times 10^{13}$ cm - are considered. Recent models of the extreme scattering events - refraction of radio-waves from quasars in dense plasma clumps in the Galactic halo - definitely show on such clouds as possible dark matter candidate. We argue that collisions of such clumpuscules are quite frequent: around $1-10 \msun$ a year can be ejected in the interstellar medium due to collisions. Optical continuum and 21 cm emissions from post-collisional gas are found to be observable. We show that clumpuscules can form around O stars HII regions of sizes $R\sim 30$ pc and emission measure $EM\simeq 20 cm^{-6}$ pc, and can also be observable in $H_α$ emission. Evaporation of clumpuscules by external ionizing radiation can be a substantial mass source. From requirement that the total mass input on the Hubble time cannot exceed the luminous mass in the Galaxy, typical radius of clouds is constrained as $R_c < 3.5\times 10^{12}$ cm, and their contribution to surface mass density as 50 $\msun pc^{-2}$. It is argued that dissipation of kinetic energy of the gas ejected by such clouds can be an efficient energy source for the Galactic halo.
dc.description21 pages, TeX, Astron. Rept., in press, revision of the paper originally submitted as 9811434, updated references
dc.identifierhttps://arxiv.org/abs/astro-ph/9811434
dc.identifierhttp://arxiv.org/abs/astro-ph/9811434
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/13428
dc.subjectAstrophysics
dc.titleObservational consequences of baryonic gaseous dark matter
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