標(biāo)題: Titlebook: Unsolved Problems of the Milky Way; Leo Blitz,Peter Teuben Book 1996 Springer Science+Business Media B.V. 1996 Galaxy.Spiral galaxy.astrop [打印本頁(yè)] 作者: 尖酸好 時(shí)間: 2025-3-21 18:18
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作者: deface 時(shí)間: 2025-3-21 23:31
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.作者: cumulative 時(shí)間: 2025-3-22 00:41
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作者: 針葉樹(shù) 時(shí)間: 2025-3-22 04:57 作者: oracle 時(shí)間: 2025-3-22 11:38
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 作者: 空中 時(shí)間: 2025-3-22 16:16
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作者: Alopecia-Areata 時(shí)間: 2025-3-22 21:07
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作者: 搬運(yùn)工 時(shí)間: 2025-3-23 00:35
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作者: Harpoon 時(shí)間: 2025-3-23 02:04 作者: 襲擊 時(shí)間: 2025-3-23 06:48
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作者: FILLY 時(shí)間: 2025-3-23 10:54 作者: 拱形面包 時(shí)間: 2025-3-23 15:44
M Giant Kinematics in Off-axis Fields between 150 and 300 PC from the Galactic Centerentric radial velocity and velocity dispersion are ?75 ± 24 km s. and 127 ± 16 km s., 2 ± 23 km s. and 127 ± 14 km s., ?14 ± 22 km s. and 126 ± 14 km s., and ?31 ± 28 km s. and 153 ± 17 km s. for fields located at 299, 288, 171, and 160 pc projected radius, respectively. The dispersions generally ma作者: CYN 時(shí)間: 2025-3-23 19:22
Results of the SiO Maser Survey of the Galactic Bulge IRAS Sources. (1991) based on IRAS point source catalogue, and more clearly by recent LOBE maps. However, no clear “dynamical” signature of the bulge bar has been found yet. At optical wavelengths, stellar radial velocities of the bulge stars were observed only at the optical windows and were not observed for t作者: 卡死偷電 時(shí)間: 2025-3-24 00:35
3D N-Body Simulations of the Milky Waygular speed etc...) still remain controversial. The large amount of photometrical and stellar kinematical data becoming now available within ～30° of the Galactic Centre should provide potentially new constraints on these parameters. Unfortunately, a detailed barred model of the Milky Way, which woul作者: 命令變成大炮 時(shí)間: 2025-3-24 04:08 作者: dictator 時(shí)間: 2025-3-24 09:08 作者: enchant 時(shí)間: 2025-3-24 12:11 作者: ELUDE 時(shí)間: 2025-3-24 15:01
A Survey of Surveysn Sky (DENIS) and the Two Micron All Sky Survey (2MASS). These surveys will permit detailed studies of Galactic structure and stellar populations in the Galaxy with unprecedented detail. Extracting the information, however, will be challenging.作者: cumulative 時(shí)間: 2025-3-24 21:41
Is There a Bulge Distinct from the Bar? the distortion pointing somewhere in the first Galactic quadrant. It is therefore tempting to reconsider our data concerning this part of the Galaxy in terms of ‘the’ Bar. But to what extent should we (or is it useful to) distinguish between the bar and the stellar bulge of old?作者: 王得到 時(shí)間: 2025-3-25 01:24 作者: FLOAT 時(shí)間: 2025-3-25 05:53
M Giant Kinematics in Off-axis Fields between 150 and 300 PC from the Galactic Centers., and ?31 ± 28 km s. and 153 ± 17 km s. for fields located at 299, 288, 171, and 160 pc projected radius, respectively. The dispersions generally match Kent’s (1992) axisymmetric mass model but may be higher than the model’s predictions at small projected radius.作者: venous-leak 時(shí)間: 2025-3-25 07:33
Results of the SiO Maser Survey of the Galactic Bulge IRAS Sources found yet. At optical wavelengths, stellar radial velocities of the bulge stars were observed only at the optical windows and were not observed for the entire region of the bulge because of the dust extinction in this direction.作者: Anecdote 時(shí)間: 2025-3-25 12:07 作者: 商店街 時(shí)間: 2025-3-25 18:36
Faint Surface Photometry of the Halo of M31[itp(.) ∝ R.. This result suggests that the globular cluster component of the halo of M31 (for which . ∝ ..) is more extended than the stellar halo of this galaxy. At μ. ≈ 28 mag arcsec. (. ≈ 10 kpc), the axial ratio of the halo of M31 is found to be ./. = 0.55 ± 0.05.作者: CHARM 時(shí)間: 2025-3-25 22:32
Book 1996hat does the answertell us about its dynamical history? Is there a black hole at thecenter of the Galaxy? How far does the Galaxy extend? How much darkmatter is there in the Milky Way system? And more.作者: 頭腦冷靜 時(shí)間: 2025-3-26 02:27 作者: Fibrillation 時(shí)間: 2025-3-26 06:56
Ellipticity of Outer Regions of Galactic Disksreference frame in which there is a common LON for orbits within the transition radius and also a differently oriented straight LON for the gas outside the transition radius, which is approximately equal to the Holmberg radius of the galaxy.作者: 沉積物 時(shí)間: 2025-3-26 09:41 作者: Palate 時(shí)間: 2025-3-26 13:38
Results from the Optical Gravitational Lensing Experiment (OGLE) OGLE events are related to dark matter . The OGLE color magnitude diagrams reveal the presence of the Galactic bar and a low density inner disk region ～ 4 kpc in radius. A catalogue of a few thousand variable stars is in preparation.作者: 放肆的你 時(shí)間: 2025-3-26 20:20
Hans-Walter Rixa about interactions between the human mind and digital entities, such as data, visual imagery, algorithms, and computer-generated predictions and recommendations. Visualization psychology is a new type of science in the making..978-3-031-34740-5978-3-031-34738-2作者: albuminuria 時(shí)間: 2025-3-26 22:19 作者: Amorous 時(shí)間: 2025-3-27 04:25 作者: MORT 時(shí)間: 2025-3-27 07:36 作者: 使熄滅 時(shí)間: 2025-3-27 09:53
he population is unknown and could be non-linear, further complicating the group-based statistical analysis. This chapter gives a perspective on performing voxel-wise morphometry of tensor data using kernel-based approach. The method is referred as Kernel-based morphometry (KBM) as it models the ten作者: Limpid 時(shí)間: 2025-3-27 14:12
E. Dweke a diffusion barrier to NO scavenging by RBCs as well as oxygen delivery from the cells to tissue in the arterioles. Thus, due to the importance of the CFL formation in the microcirculation, there have been many attempts to experimentally quantify the CFL width in microcirculatory vessels. In this 作者: 最小 時(shí)間: 2025-3-27 18:09 作者: 開(kāi)玩笑 時(shí)間: 2025-3-27 23:33 作者: 多山 時(shí)間: 2025-3-28 04:26 作者: Feckless 時(shí)間: 2025-3-28 06:48 作者: 逃避系列單詞 時(shí)間: 2025-3-28 13:59 作者: 得體 時(shí)間: 2025-3-28 18:36
S. M. Kent ideas presented in the book are appli- cable to other areas, including computer simulation, decision theory and stochastic modeling. Another book could discuss978-1-4613-6848-9978-1-4615-4121-9Series ISSN 1387-666X Series E-ISSN 2698-5489 作者: 旅行路線 時(shí)間: 2025-3-28 19:18
K. Z. Stanek,M. Mateo,A. Udalski,M. Szymański,J. Ka?u?ny,M. Kubiak,W. Krzemińskiif the contribution of this set of universal skills is to be fully exploited at all levels and in all science subjects..978-1-4020-5882-0978-1-4020-3613-2Series ISSN 1871-2983 Series E-ISSN 2213-2260 作者: Constituent 時(shí)間: 2025-3-29 01:23
Konrad Kuijkenations of information retrieval visualization for Internet traffic analysis, and Internet information searching and browsing. The author also addresses challenges such as ambiguity, metaphorical applications, a978-3-642-09442-2978-3-540-75148-9Series ISSN 1871-7500 Series E-ISSN 2730-6836 作者: jeopardize 時(shí)間: 2025-3-29 04:15
F. Combesthe substance and role of the essential representations and abstractions used by planners and designers. In the past, when 2D planar representations (drawings, usually on paper) served as the conventional means978-3-642-06783-9978-3-540-30491-3作者: magnate 時(shí)間: 2025-3-29 10:21 作者: MILL 時(shí)間: 2025-3-29 11:25
Morphology of the Galactic Bulge from COBE DIRBE Observationse. that the bulge is not rotationally symmetric in the plane of the disk (see Blitz 1993 for a review of the subject). The existence of a bar in our Galaxy would have important implications for the dynamics of the Galaxy. A bar would provide a mechanism for sweeping gas from the disk into the Galact作者: 搜集 時(shí)間: 2025-3-29 19:25
3D N-Body Simulations of the Milky Wayed so far, but will be introduced as a next step in this ongoing work. Some results presented at this meeting will be only quickly summarised here and explained in some more details elsewhere (Fux et al. 1995 and A&A paper in preparation).作者: Provenance 時(shí)間: 2025-3-29 23:08 作者: Exposition 時(shí)間: 2025-3-30 02:27
The Axisymmetric Stability of the Milky Waysis was strictly local, the stability criterion it yielded has been found to be remarkably reliable in global studies; I review earlier results and give a further example in Sellwood (1995, hereafter S95). Toomre (1974) concluded that the MW is safely stable to axisymmetric Jeans modes.作者: agenda 時(shí)間: 2025-3-30 05:52 作者: nullify 時(shí)間: 2025-3-30 10:30
Unsolved Problems of the Milky Way978-94-009-1687-6Series ISSN 1743-9213 Series E-ISSN 2352-2186 作者: 痛恨 時(shí)間: 2025-3-30 15:07
International Astronomical Union Symposiahttp://image.papertrans.cn/u/image/942499.jpg作者: Grievance 時(shí)間: 2025-3-30 18:36
https://doi.org/10.1007/978-94-009-1687-6Galaxy; Spiral galaxy; astrophysics; black hole; interstellar matter; milky way作者: SOB 時(shí)間: 2025-3-30 23:38
Near Infrared Star Counts as a Probe of Asymmetries in the Galaxy’s DiskI have recently started an observing program to study the distribution of dynamically old giant stars in the disk, looking for (.) large amplitude spiral arms and (.) small amplitude corrugations.作者: sigmoid-colon 時(shí)間: 2025-3-31 02:55
