Relict Radiation of the Universe and Population of Rotation Levels of Interstellar Molecules
Relict radiation effect on rotational temperature of interstellar molecules
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Relict radiation effect on rotational temperature of interstellar molecules
Absorption and emission lines, continuous emission of thermal radiation, and continuous nonthermal emission of interstellar spectra
Electromagnetic radiation due to cosmic ray energy dissipation in interstellar hydrogen
Far UV extinction curve and wavelength dependence of interstellar polarization by graphite grains
Optical properties of interstellar grains, noting complex index of refraction as function of wavelength
Fusion propulsion for interstellar missions, examining requirements for detection of extra solar life
Interstellar material, emphasizing chemical characterization of dust by absorption spectroscopy
Far UV interstellar absorption lines evaluated for main-sequence B stars
Hydroxyl radical emission, hypotheses attempting to explain OH emission origin, including possible maser mechanism and interstellar communications
Nonlinear growth of interstellar gas clouds and forces in three dimensions
Interstellar gas dynamic instability caused by galactic cosmic rays and magnetic field, showing turbulent and fragmentation enhancement of ambipolar diffusion
Interstellar gas and magnetic field periodic system stability noting free-fall time
The existing theories of comet dynamics held that large numbers of comets are ejected to interstellar space and that other stellar systems would do the same; however, no comet on a hyperbolic orbit has ever been observed. Calculations developed by Duncan et al. are used to show that most comets thought to be ejected would actually be captured by the Oort Cloud.
This paper will examine candidate communications architectures for potential interstellar missions in an effort to determine feasibility for such links and to identify likely technology advances that will be needed to support such endeavors. Examination of this challenging and futuristic communications problem may serve to guide the direction and advancement of space telecommunications technologies useful for other nearer-term applications.
While molecular hydrogen is by far the most abundant gas phase molecule in interstellar dark clouds, the extreme volatility of H(sub 2) suggests that it has a relatively low abundance in grain volatile mantles, thought to be composed largely of amorphous water ice.
We discuss the effects of finite source size on the diffraction pattern produced by scattering in a thin screen, particularly as applied to radio-wave scattering, by density fluctuations in the interstellar plasma.
We analyze the properties of IRAS maps of interstellar clouds using Laplacian Pyramid.