標題: Titlebook: Galactic Bulges; Proceedings of the 1 Herwig Dejonghe,Harm J. Habing Conference proceedings 1993 Kluwer Academic Publishers 1993 Bulge.Gala [打印本頁] 作者: notable 時間: 2025-3-21 19:40
書目名稱Galactic Bulges影響因子(影響力)
書目名稱Galactic Bulges影響因子(影響力)學科排名
書目名稱Galactic Bulges網(wǎng)絡公開度
書目名稱Galactic Bulges網(wǎng)絡公開度學科排名
書目名稱Galactic Bulges被引頻次
書目名稱Galactic Bulges被引頻次學科排名
書目名稱Galactic Bulges年度引用
書目名稱Galactic Bulges年度引用學科排名
書目名稱Galactic Bulges讀者反饋
書目名稱Galactic Bulges讀者反饋學科排名
作者: Custodian 時間: 2025-3-21 21:36
Dynamics of the Galactic Bulgeng fairly rapidly. To date, there is little evidence for triaxiality in the stellar kinematics: the available stellar velocities are consistent with Kent’s (1992) oblate model. This unsatisfactory situation is expected to improve rapidly.作者: 驚奇 時間: 2025-3-22 02:10
1743-9213 to hold a more properly organised symposium on "Galactic Bulges" in a few years time. After some discussion a Scientific Organising Committee was founded and after some manoeuvring a chairman was chosen, a local organiser was assigned and two editors were given instructions. A good thing about the l作者: 保守黨 時間: 2025-3-22 07:02
Object-Oriented Transaction-Level Modellingike Rich, Don Terndrup, and Jay Frogel. But any errors, and especially any prejudices, are purely my own. And in my reading I have undoubtedly missed some important papers, but I hope that their authors will forgive me.作者: Commodious 時間: 2025-3-22 09:05 作者: Folklore 時間: 2025-3-22 16:10 作者: Folklore 時間: 2025-3-22 20:17 作者: 殘忍 時間: 2025-3-22 23:34
Olga Barrera,Alan Cocks,Alan Ponterity function in the central 200 pc resembles that recently found in M32 and M31 bulge fields. Depending on how one interprets the extended giant branch, the population may be intermediate age with some ongoing star formation, or mostly old and metal rich, with star formation confined to the nucleus.作者: 高原 時間: 2025-3-23 03:14 作者: ALT 時間: 2025-3-23 07:28
The Stellar Population of the Inner 200 Parsecsity function in the central 200 pc resembles that recently found in M32 and M31 bulge fields. Depending on how one interprets the extended giant branch, the population may be intermediate age with some ongoing star formation, or mostly old and metal rich, with star formation confined to the nucleus.作者: 騙子 時間: 2025-3-23 09:49
Ilan Fridental,Yaron Finkelsteinterized by different galactic orbits. (1) OH/IR stars in the galactic disk on almost circular orbits; (2) OH/IR stars in the galactic bulge on orbits of lower angular momentum; (3) OH/IR stars within 150 pc from the galactic center forming a rapidly rotating system.作者: Conserve 時間: 2025-3-23 16:40 作者: craving 時間: 2025-3-23 20:20 作者: ingenue 時間: 2025-3-23 23:16
Trends in Digital Image Processing Researche dwarf ellipticals of the similar mass (the biased wind). Unfortunately, the observational data available at present of stellar populations of the bulges are not yet sufficient to get a firm conclusion on the origin of the bulges.作者: 滑稽 時間: 2025-3-24 04:53
N. D. Gunn,J. Byrne,E. B. Holubthan halo properties alone. This is clearest for systems with low B/D ratio, where bulge velocity dispersions are similar to disk velocity dispersions. Constraints on the stellar formation scenarios are discussed.作者: 異常 時間: 2025-3-24 10:25 作者: 單調性 時間: 2025-3-24 11:56
Stellar Population Synthesise dwarf ellipticals of the similar mass (the biased wind). Unfortunately, the observational data available at present of stellar populations of the bulges are not yet sufficient to get a firm conclusion on the origin of the bulges.作者: Tincture 時間: 2025-3-24 15:36
What is the Connection between Ellipticals and Bulges ?than halo properties alone. This is clearest for systems with low B/D ratio, where bulge velocity dispersions are similar to disk velocity dispersions. Constraints on the stellar formation scenarios are discussed.作者: 事先無準備 時間: 2025-3-24 19:26 作者: obsolete 時間: 2025-3-25 00:53 作者: Foreshadow 時間: 2025-3-25 06:06
Advances in Discrete Differential Geometry.-law central brightness profiles belong not to bulges but to disks. That is, some galaxy disks have central brightness profiles that are much steeper than the inward extrapolation of an exponential fit to the outer parts. These observations and .-body simulations of gas flow in nonaxisymmetric gala作者: Decibel 時間: 2025-3-25 11:16
Advances in Earthquake Predictionfollowing situations: 1) slow or fast pattern speed Ω., 2) direct or retrograde gas motion with respect to the stars, and 3) warm or hot gas temperature .. Initial parameters and final characteristics of each runs are reported in Table I.作者: 重畫只能放棄 時間: 2025-3-25 15:32
Conference proceedings 1993 This feeling of togeth- erness made up for the small shortcomings of the lecture room, which is normally used as a sports hall. The weather was fair, except on the day of the barbecue when pouring rain forced us to go inside.作者: Colonoscopy 時間: 2025-3-25 18:58
1743-9213 situation. This feeling of togeth- erness made up for the small shortcomings of the lecture room, which is normally used as a sports hall. The weather was fair, except on the day of the barbecue when pouring rain forced us to go inside.978-0-7923-2425-6978-94-011-0922-2Series ISSN 1743-9213 Series E-ISSN 2352-2186 作者: 有害 時間: 2025-3-25 21:12
The Globular Cluster and Horizontal Branch Content of the Bulge and HaloB that traces the density of its parent population (Preston, Shectman, and Beers 1991a) and the RHB component must be inferred by indirect methods. Furthermore, well above the Galactic plane, where nearly all searches have been conducted (see Preston . 1991a for references), these two species occur 作者: collateral 時間: 2025-3-26 03:04 作者: ALB 時間: 2025-3-26 05:22
Kinematics of Extragalactic Bulges: Evidence that some Bulges are Really Disks.-law central brightness profiles belong not to bulges but to disks. That is, some galaxy disks have central brightness profiles that are much steeper than the inward extrapolation of an exponential fit to the outer parts. These observations and .-body simulations of gas flow in nonaxisymmetric gala作者: 漂浮 時間: 2025-3-26 10:49
3D Gas Dynamics in Triaxial Systemsfollowing situations: 1) slow or fast pattern speed Ω., 2) direct or retrograde gas motion with respect to the stars, and 3) warm or hot gas temperature .. Initial parameters and final characteristics of each runs are reported in Table I.作者: FORGO 時間: 2025-3-26 16:16
Object-Oriented Transaction-Level Modellingn very close in recent years, so that I have been able to approach it with a fairly open mind, though I must acknowledge a lot of generous help from Mike Rich, Don Terndrup, and Jay Frogel. But any errors, and especially any prejudices, are purely my own. And in my reading I have undoubtedly missed 作者: 尖 時間: 2025-3-26 17:20 作者: 鎮(zhèn)壓 時間: 2025-3-26 21:48
Diabetes and Neurological Disorder,ira evolutionary phase. There is evidence that Miras in the LMC and the Bulge occupy different parts of the instability strip but obey the same PLC relation. The Bulge contains at least 2 x 10. Miras of which 100 or so have luminosities in excess of M. = -5 mag. The Mira phase lasts more than 10. yr作者: genesis 時間: 2025-3-27 01:34 作者: FLEET 時間: 2025-3-27 08:13
Monica Levine MD,R. Wendel Naumann MDs global properties. The mean metal abundance is [M/H] ≈ +0.3 at . = 0.5 kpc, and declines by about 1.2 dex out to . = 2 kpc. The line-of-sight velocity dispersion at . = 0.5 kpc is σ. ≈ 115 km sec. for all population tracers, and declines by . logσr/. log . = -0.4. It now seems fairly clear that on作者: 消極詞匯 時間: 2025-3-27 11:15
https://doi.org/10.1007/88-470-0458-6 Bulge place modest constraints on the early history of these regions and possible interactions between them. The extant data are fragmentary, and the conclusions correspondingly uncertain. The observables are HB morphology, heavy element abundance, and space density. The data base is constrained by作者: 單片眼鏡 時間: 2025-3-27 16:32
Trends in Digital Image Processing Researcho that of the giant ellipticals. There seems to be no conspicuous colour-magnitude relation intrinsic to the bulges. This can be explained if the bulges formed by the dissipative collapse of central regions of proto-galaxies followed by the supernova-driven bulge wind which was induced later than th作者: Leisureliness 時間: 2025-3-27 18:11 作者: 冒號 時間: 2025-3-27 22:23 作者: 可行 時間: 2025-3-28 06:00 作者: cardiovascular 時間: 2025-3-28 08:54 作者: BUDGE 時間: 2025-3-28 12:15
N. D. Gunn,J. Byrne,E. B. Holubdistinction between bulges and ellipticals is more accurately described as a quantitative variation in Bulge/Dis& ratio. The exception may be the brightest ellipticals, which are usually Bright(est) Cluster Members. The available evidence suggests that the spheroid properties are determined by more 作者: 免除責任 時間: 2025-3-28 17:40 作者: 新奇 時間: 2025-3-28 22:27
Monte Carlo Simulation Using VHDL-AMSevealed by each type of survey is discussed. Particular attention is given to surveys of the Sgr I clear field, its content of long-period variables and their implications for distance determination and the high end of the Bulge luminosity function.作者: 征服 時間: 2025-3-29 01:44 作者: overrule 時間: 2025-3-29 05:18
https://doi.org/10.1007/978-94-011-0922-2Bulge; Galaxy; Variation; galaxies; milky way作者: Vldl379 時間: 2025-3-29 10:05
978-0-7923-2425-6Kluwer Academic Publishers 1993作者: 靈敏 時間: 2025-3-29 13:32
Galactic Bulges978-94-011-0922-2Series ISSN 1743-9213 Series E-ISSN 2352-2186 作者: 來這真柔軟 時間: 2025-3-29 18:15
Tim Mould MD, FRCOG, MBBS, MA, DM, FRCOGThe available kinematical data on OH/IR stars is discussed, and dynamical models for the OH/IR stars are presented.作者: foliage 時間: 2025-3-29 20:13
J. Struyven,G. Kuhn,C. C. SchulmanAfter a discussion of the methods used to derive the physical parameters of planetary nebulae and their central stars, the global properties of planetary nebulae in the Galactic bulge are reviewed, and compared to those of planetary nebulae in different contexts.作者: 角斗士 時間: 2025-3-30 00:40
Moonyong Lee,Nguyen Van Duc LongThe “unresolved nuclear region” as Hubble (1926) indicated the bulge of spiral galaxies, became a physically distinct component with the introduction by Baade (1944) of the concept of stellar populations.作者: 一再煩擾 時間: 2025-3-30 05:54
Introduction to the Time Scales Calculus,Without attempting to cover all of the topics discussed at this meeting, I plan to talk briefly about some of the major achievements and ideas that came up here, and then mention a few of the important open questions and some work that might be done to answer them.作者: 口訣法 時間: 2025-3-30 11:16 作者: 狗舍 時間: 2025-3-30 14:35
The Global Properties of Planetary Nebulae in the Galactic BulgeAfter a discussion of the methods used to derive the physical parameters of planetary nebulae and their central stars, the global properties of planetary nebulae in the Galactic bulge are reviewed, and compared to those of planetary nebulae in different contexts.作者: Firefly 時間: 2025-3-30 17:18
Photometric Properties of Extragalactic BulgesThe “unresolved nuclear region” as Hubble (1926) indicated the bulge of spiral galaxies, became a physically distinct component with the introduction by Baade (1944) of the concept of stellar populations.作者: fulcrum 時間: 2025-3-30 23:37
Summary: Achievements and Open QuestionsWithout attempting to cover all of the topics discussed at this meeting, I plan to talk briefly about some of the major achievements and ideas that came up here, and then mention a few of the important open questions and some work that might be done to answer them.作者: NAIVE 時間: 2025-3-31 01:41 作者: FANG 時間: 2025-3-31 08:28 作者: 固執(zhí)點好 時間: 2025-3-31 11:24
Long-Period Variables and Carbon Stars in the Galactic Bulgeira evolutionary phase. There is evidence that Miras in the LMC and the Bulge occupy different parts of the instability strip but obey the same PLC relation. The Bulge contains at least 2 x 10. Miras of which 100 or so have luminosities in excess of M. = -5 mag. The Mira phase lasts more than 10. yr作者: Foregery 時間: 2025-3-31 14:39 作者: 短程旅游 時間: 2025-3-31 18:29 作者: 嫻熟 時間: 2025-3-31 22:20
The Globular Cluster and Horizontal Branch Content of the Bulge and Halo Bulge place modest constraints on the early history of these regions and possible interactions between them. The extant data are fragmentary, and the conclusions correspondingly uncertain. The observables are HB morphology, heavy element abundance, and space density. The data base is constrained by
