Titlebook: Unsolved Problems of the Milky Way; Leo Blitz,Peter Teuben Book 1996 Springer Science+Business Media B.V. 1996 Galaxy.Spiral galaxy.astrop

尖酸好

書目名稱Unsolved Problems of the Milky Way影響因子(影響力)




書目名稱Unsolved Problems of the Milky Way影響因子(影響力)學(xué)科排名




書目名稱Unsolved Problems of the Milky Way網(wǎng)絡(luò)公開度




書目名稱Unsolved Problems of the Milky Way網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Unsolved Problems of the Milky Way被引頻次




書目名稱Unsolved Problems of the Milky Way被引頻次學(xué)科排名




書目名稱Unsolved Problems of the Milky Way年度引用




書目名稱Unsolved Problems of the Milky Way年度引用學(xué)科排名




書目名稱Unsolved Problems of the Milky Way讀者反饋




書目名稱Unsolved Problems of the Milky Way讀者反饋學(xué)科排名

deface

The Shape of the Disk: Clues from the Kinematics of Disk Starsthe existence of asymmetries has been reported and discussed in the literature from a wide variety of sources (most recently, Nakai & Nishiyana 1994). Now, in order to understand Milky Way evolutionary history, it is our job to determine the origin and intrinsic structure of these asymmetries.

cumulative

The Shapes of Dark Haloshe Milky Way (MW), the latter mean the massive, dark component providing the large dynamically inferred mass in and around galaxies. This review will focus on massive, dark halos. Despite the title of this conference, we cannot restrict our attention to the shape of the MW halo: very little would be

針葉樹

oracle

Faint Surface Photometry of the Halo of M31o of M31 down to a level of μ. ? 30 mag arcsec. (R ≈ 20 kpc). The surface brightness along the minor axis of the M31 halo is well-represented by a single de Vaucouleurs law (0.2 ? R[kpc] ? 20). Alternatively, the outer halo of M31 can also be modelled by a power-law density distribution of the form

空中

A Survey of Surveyshe status and prospects for research for 3 new ground-based surveys: the Sloan Digital Sky Survey (SDSS), the Deep Near-Infrared Survey of the Southern Sky (DENIS) and the Two Micron All Sky Survey (2MASS). These surveys will permit detailed studies of Galactic structure and stellar populations in t

Alopecia-Areata

Ellipticity of Outer Regions of Galactic Disksa ., slowly rotating, centrally concentrated dark corona (Dubinski and Carlberg, 1991; Dubinski, 1992). Binney (1978) was the first to consider the effects of triaxial coronas around disk galaxies, showing that they might explain the observed warps and apparent twists seen in many disks. In external

搬運(yùn)工

Morphology of the Galactic Bulge from COBE DIRBE Observationstic bulge at effective wavelengths of 1.25, 2.2, 3.5, and 4.9p (Hauser 1993, plate 3; Arendt et al. 1994; Weiland et al. 1994). The bulge, defined here as the spheroid within the │.│ < 20° and │.│ < 10° region around the Galactic center, and its stellar content have been subjects of considerable int

Harpoon

襲擊

Results from the Optical Gravitational Lensing Experiment (OGLE)s in the range 8.6 < to < 80 days, where t. = ../.. A complete sample of nine events gave the optical depth to gravitational microlensing larger than (3.3 ± 1.2) × 10., in excess of current theoretical estimates, indicating a much higher efficiency for microlensing by either bulge or disk lenses. Th