Results 191 to 200 of about 4,742 (219)
V3101 Cyg: A Cataclysmic Variable Born with a Brown Dwarf Donor
Ramirez S +7 more
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Synthetic [CII] line emission maps of simulated interstellar medium [PDF]
, 2018 In this thesis I analyse the synthetic [CII] emission from a slice of interstellar medium (ISM). The [12CII] line emission is the fine structure transition in carbon ions. It is observed in several phases of the ISM, such as the molecular, warm, and ionized gas phases.
Franeck, Annika
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On the excitation mechanism of the 21 cm interstellar hydrogen emission line
Physica, 1952exaly +2 more sources
Observation of [CII] 158 μm emission from the diffuse interstellar medium
AIP Conference Proceedings, 1992 We report the first direct detection of 158 μm [CII] line emission from the diffuse interstellar medium at high galactic latitude. We measured the integrated line intensity in a 36' field-of-view along a triangular scan in a 5°×20° region in Ursa Major ...
V V Hristov, Philip Mauskopf, A E Lange
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Survey of Molecular Emission Lines in the WB 673 Interstellar Filament
Astronomy Reports, 2020We report observations of molecular line emission toward dense clumps of the WB 673 interstellar filament: WB 668, WB 673, S233–IR, and G173.57+2.43. The observations were done with the 20-m telescope at the Onsala Space Observatory (Sweden). Maps of emission, column densities, and relative abundances of CO, N2H
O. L. Ryabukhina, M. S. Kirsanova
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Measuring EUV Line Emission from the Hot Interstellar Medium
International Astronomical Union Colloquium, 1984AbstractIn the local interstellar medium, the presence of hot gas (log T ~ 5 to 6) has been inferred from measurements of oxygen VI absorption in the ultraviolet, and from diffuse emission in the extreme ultraviolet (EUV) and soft X-ray regions. Here we describe a spectrometer that is very sensitive to gas in this temperature range.
Simon Labov +2 more
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Fir continuum and line emissions from interstellar medium in galaxies
Astrophysics and Space Science, 2010A self-consistent method has been evolved to infer physical parameters like density, radiation field and abundances using line and continuum radiations as diagnostics. For that purpose, we first calculate the temperatures of graphite and silicate grains using the model of Li and Draine (Astrophys. J.
null Shafiqullah +2 more
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Anomalous Intensity Ratios of the Interstellar Lines of OH in Absorption and Emission
Nature, 1965WE have previously found1 intensity ratios of the four microwave lines of OH in disagreement with the theoretical and laboratory ratios2 of 1 : 5 : 9 : 1 for the lines at 1,612, 1,665, 1,667 and 1,720 Mc/s. For the strong OH absorption of the radio source Sagittarius A it appeared that the ratios might be attributed to high opacity3.
R. X. MCGEE +3 more
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Emission lines due to interstellar dust in the visible spectra of nebulae
Astrophysics and Space Science, 1979It is suggested that certain sharp lines in the visible and near ultraviolet spectra of nebule may be due to fluorescence from grains. Evidence is presented that some of these lines could arise from MgO or CaO grains. Some sharp diffuse interstellar bands may also appear in the spectra of nebulae.
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Interstellar Emission and Absorption Lines
2012Interstellar emission and absorption lines are discussed, including optical recombination lines, the 21cm hydrogen line, and broad lines such as the interstellar Lyman-alpha line. This chapter ends with a discussion of the curve of growth.
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