Titlebook: Internal Kinematics and Dynamics of Galaxies; E. Athanassoula Book 1983 International Astronomical Union 1983 Bulge.Galaxy.Hubble sequence

MAUVE

W. Wamsteker,J. J. Lorre,H. E. Schusterion, where the definition of self is affirmed through differentiation from the other. The chapter investigates how correctional officers’ identities are daily constructed and affirmed through their juxtaposition with inmates and the dominant gendered narratives. It also examines how stigma and preco

思考而得

P. Notni,W. BronkallaArbeiten von Gale Miller (1992) und James Holstein (1992) (siehe auch Holstein/Miller 1993). Im Unterschied zu einer Vielzahl weiterer Ansätze im Forschungsbereich sozialer Probleme beschäftigen sie sich nicht mit gesellschaftlichen Definitionsprozessen, sondern mit „der Konstruktion konkreter Probl

悦耳

P. C. van der Kruit,G. S. ShostakArbeiten von Gale Miller (1992) und James Holstein (1992) (siehe auch Holstein/Miller 1993). Im Unterschied zu einer Vielzahl weiterer Ansätze im Forschungsbereich sozialer Probleme beschäftigen sie sich nicht mit gesellschaftlichen Definitionsprozessen, sondern mit „der Konstruktion konkreter Probl

Debate

清澈

Fulsome

enterprise

不适

HI Observations of the Irregular Galaxy IC 10De Vaucouleurs and Freeman (1972) have classified it as a Magellanic barred irregular. With a heliocentric radial velocity of -350 km/sec, its distance is uncertain, and various investigators have placed it as far away as 3, and as near as 1 Mpc (Bottinelli et al., 1972; Roberts, 1962). For the latt

搏斗

The Distribution of Molecular Clouds in Spiral GalaxiesI is concentrated in the inner part of the Galaxy in a “ring” between 4–8 kpc and in the inner 1 kpc. Subsequent surveys (Gordon and Burton 1976, Cohen and Thaddeus 1977, Solomon .. {dy1979}) confirmed this picture with more extensive data. The molecular interstellar medium was shown to be dominated

Gossamer

The CO Rotation Curve of the Milky Way : Accuracy and Implications= 18 kpc. Recently, Blitz and Fich (1983) have examined the uncertainties in the rotation curve at large R and have concluded that : 1) Of all the uncertainties, small changes in R. and θ. have the most serious effect on the rise at large R. However, unless ω. < 20 km s. kpc., a value smaller than t