Observational consequences of baryonic gaseous dark matter

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Possible observational consequences of dark matter in the Galaxy in the form of dense molecular gas clouds - clumpuscules of masses Mc 10⁻³ and radii Rc 3× 10¹³ 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 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 30 pc and emission measure EM≃ 20 cm⁻⁶ pc, and can also be observable in Hα 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 Rc < 3.5× 10¹² cm, and their contribution to surface mass density as 50 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.