8. The Milky Way and Interstellar Matter: Stars and the Space Between

2019 ◽  
pp. 100-114
Keyword(s):  
Milky Way ◽  
Interstellar Matter

scholarly journals The galactic structure and the appearance of the Milky Way

1970 ◽  
Vol 38 ◽  
pp. 222-224
Author(s):  
E. D. Pavlovskaya ◽  
A. S. Sharov
Keyword(s):  
Spatial Distribution ◽  
Surface Brightness ◽  
Milky Way ◽  
Spiral Structure ◽  
Galactic Structure ◽  
Interstellar Matter

The appearance of the Milky Way for an observer situated within our Galaxy is determined by the spatial distribution of stars and absorbing interstellar matter. Hence it may be hoped that the study of the surface brightness of the Milky Way permits to derive the spiral structure of our Galaxy.

scholarly journals Fluctuations of the Diffuse Galactic Background

1990 ◽  
Vol 139 ◽  
pp. 99-99
Author(s):  
K. Mattila
Keyword(s):  
Milky Way ◽  
Interstellar Matter ◽  
Observational Material ◽  
The Galaxy ◽  
The Mean ◽  
Dust Distribution ◽  
Galactic Background

An analysis of fluctuations in the brightness of the Milky Way using the concept that interstellar matter occurs in the form of discrete clouds was first applied by Ambarzumian (1940, 1944). This theory was formulated in a general way and discussed in great detail in a series of papers by Chandrasekhar and Münch (1950a, 1950b, 1951, 1952), by Münch and Chandrasekhar (1952), and by Limber (1953). More recently Peters (1970) presented an analysis of this kind based on extensive photographic observational material. Although the influence of clumpiness of the dust distribution on the mean integrated starlight was thoroughly discussed in these papers, it has not been properly included in most of the photometric models of the Galaxy. Only the models of Caplan and Grec (1979) and Mattila (1980a, 1980b) incorporate these effects.

scholarly journals DIVISION VI: INTERSTELLAR MATTER

2008 ◽  
Vol 4 (T27A) ◽  
pp. 267-272
Author(s):  
Thomas J. Millar ◽  
You Hua Chu ◽  
John E. Dyson ◽  
Dieter Breitschwerdt ◽  
Michael G. Burton ◽  
...  
Keyword(s):  
Milky Way ◽  
Chemical Properties ◽  
Interstellar Matter ◽  
Physical And Chemical Properties ◽  
Wide Range ◽  
Physical And Chemical ◽  
And Chemical Properties

Division VI provides a focus for astronomers studying a wide range of problems related to the physical and chemical properties of interstellar matter in the Milky Way and other galaxies.

scholarly journals A Study of the Distribution of Interstellar Matter

1973 ◽  
Vol 52 ◽  
pp. 219-225
Author(s):  
Lars Olof Lodén
Keyword(s):  
Interstellar Dust ◽  
Milky Way ◽  
Angular Separation ◽  
Minimum Size ◽  
Interstellar Matter ◽  
Lateral Separation ◽  
Empirical Estimation ◽  
Colour Excess ◽  
The Difference ◽  
Selection Of

As a first step towards an empirical estimation of the minimum size of interstellar dust formation units (clouds etc.) the correlation between angular separation and difference in colour excess has been studied for a selection of close star couples with coinciding magnitude and spectral type. Principally, the result indicates that there is no palpable correlation between the difference in colour excess and the lateral separation of the stars. This and other properties speak in favour of the conception that obscuring matter in the Milky Way is concentrated in extremely small units of high density.

Variation of the amount of hydrogen along the galactic ridge

1967 ◽  
Vol 31 ◽  
pp. 171-172
Author(s):  
Th. Schmidt-Kaler
Keyword(s):  
Surface Brightness ◽  
Milky Way ◽  
Neutral Hydrogen ◽  
Line Of Sight ◽  
Optical Surface ◽  
Hydrogen Density ◽  
Continuous Radiation ◽  
Galactic Longitude

The integralNHof neutral-hydrogen density along the line of sight is determined from the Kootwijk and Sydney surveys. The run ofNHwith galactic longitude agrees well with that of thermal continuous radiation and that of the optical surface brightness of the Milky Way.

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