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Interstellar Matter and Star Formation
Astrophysics and Space Science, 2003I first met Fred Hoyle in the summer of 1967 as a visitor to the brand new Institute of Theoretical Astronomy IOTA, the precursor to the Institute of Astronomy. Fred had invited me to spend the summer in Cambridge at the suggestion of Peter Strittmatter.
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Physics of the Interstellar Matter
1988Radiation Transport Equation: Let us follow the propagation of radiation of frequency v along the line of sight towards the observer, in the region of an interstellar cloud (Fig. 5.1). Let e v denote the emission coefficient of the gas, so defined that e v dw) represents the radiation energy emitted per unit of volume, time and frequency in the solid ...
Helmut Scheffler, Hans Elsässer
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Graphite as Interstellar Matter
Nature, 1967GRAPHITE consists of hexagonal crystals. Thus the optical constants depend on the direction of the incident light. For light with an electric vector parallel to the basal planes of the crystals graphite behaves like a metal. In the perpendicular direction, for light propagation through a crystal with an electric vector along optic axis, it behaves like
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1985
Using the echelle-A grating of the GHRS, the authors have observed the C II λλ1335, 1336 emission lines of the nearby (d = 13.3 pc) star system Capella (G8 III + G1 III). Interstellar C II absorption features are detected within both stellar emission lines.
S. Böhme +9 more
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Using the echelle-A grating of the GHRS, the authors have observed the C II λλ1335, 1336 emission lines of the nearby (d = 13.3 pc) star system Capella (G8 III + G1 III). Interstellar C II absorption features are detected within both stellar emission lines.
S. Böhme +9 more
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Dynamics of Interstellar Matter
1975Three basic equations describe the flow of a fluid. They are the equation of continuity $$ \frac{{\partial \rho }}{{\partial t}} + \bar \nabla \cdot \left( {\rho \bar u} \right) = 0 $$ (1.1) , the equation of motion $$ \frac{{\partial \bar u}}{{\partial t}} + (\bar u \cdot \bar \nabla )\bar u = - \frac{{\bar \nabla P}}{\rho } $$ (1.2)
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Studies of Interstellar Matter
2012Observational evidence that the space between the stars in our Galaxy is not empty came as early as the beginning of the 20th century with the discovery of stationary Ca II lines in spectra of the binary star δ Orionis by J. Hartmann in 1904. In 1922 E. Hubble concluded that dust clouds scatter the light of nearby cool stars, which are then detected as
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Ultraviolet spectroscopy of interstellar and intergalactic matter
Applied Optics, 1980Ultraviolet radiation in absorption and emission provides diagnostics of interstellar and intergalactic matter. After reviewing some basic physical reasons for the importance of UV astronomy, the UV observations of both media, the future uses of high resolution spectrometers in the far UV, and the atomic data required for proper interpretation are ...
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Constraining axion and compact dark matter with interstellar medium heating
Physical Review D, 2023Digvijay Wadekar, Zihui Wang
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