標(biāo)題: Titlebook: Dynamics and Interactions of Galaxies; Proceedings of the I Roland Wielen Conference proceedings 1990 Springer-Verlag Berlin Heidelberg 199 [打印本頁] 作者: 退縮 時間: 2025-3-21 20:05
書目名稱Dynamics and Interactions of Galaxies影響因子(影響力)
書目名稱Dynamics and Interactions of Galaxies影響因子(影響力)學(xué)科排名
書目名稱Dynamics and Interactions of Galaxies網(wǎng)絡(luò)公開度
書目名稱Dynamics and Interactions of Galaxies網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Dynamics and Interactions of Galaxies被引頻次
書目名稱Dynamics and Interactions of Galaxies被引頻次學(xué)科排名
書目名稱Dynamics and Interactions of Galaxies年度引用
書目名稱Dynamics and Interactions of Galaxies年度引用學(xué)科排名
書目名稱Dynamics and Interactions of Galaxies讀者反饋
書目名稱Dynamics and Interactions of Galaxies讀者反饋學(xué)科排名
作者: Pert敏捷 時間: 2025-3-21 20:47
Are High Redshift Galaxies Interacting?rtunately, as far as mergers at high redshifts is concerned, I cannot bring myself to do this. Instead, I propose to present you with evidence that peculiar phenomena are occurring in the most distant galaxies we can study. According to your degree of faith in the “Book of Mergers”, you can decide w作者: 衰老 時間: 2025-3-22 03:11 作者: DEFT 時間: 2025-3-22 05:20
Interactions in “Butcher-Oemler” Clusters of galaxies at redshifts near 0.4 contained a much larger population of “blue” galaxies than expected. This suggested rapid color evolution of galaxies in 1/3 of a Hubble time. In order to put this on a more quantitative level, Butcher and Oemler (1984a) undertook a photometric study of 33 clusters作者: Fantasy 時間: 2025-3-22 08:44
Are Our Globular Clusters Coeval?axy formed. A basic goal is to determine the time interval over which the Galactic halo and disk were formed, since a short time interval (< 1 Gyr) would be consistent with the picture of rapid, ordered collapse proposed by Eggen, Lynden-Bell, and Sandage (1962), whereas a much longer time interval 作者: 令人悲傷 時間: 2025-3-22 15:14
Stellar Populations and Mergerseach population being but a different stage in the process? Or have at least some of them nothing to do with the origins and evolution of the others, as expected from mergers? In the context of this meeting, we will look particularly at the latter possibility, and will discuss briefly the data suppo作者: 令人悲傷 時間: 2025-3-22 21:06
A New Model of the Magellanic Stream of the Magellanic Stream. In contrast Zaritsky et al. (1989), using the statistical procedure developed by Little and Tremaine (1987), have found this mass to be 3.6 × 10. M. from the orbits of satellites of the Galaxy.作者: ABOUT 時間: 2025-3-23 00:47 作者: animated 時間: 2025-3-23 01:59
Status of Shell Galaxiesatalogue (Arp, 1966). But only recently has special attention has been drawn to them. The improvement of photographic emulsions, and the application of new photographic techniques such as “unsharp masking” and “contrast enhancement” by Malin (1977, 1981) has led to the discovery of shells and other 作者: 值得 時間: 2025-3-23 05:46 作者: Asparagus 時間: 2025-3-23 10:14 作者: Vo2-Max 時間: 2025-3-23 15:01
Structure of the NGC 1023 Systemassume that NGC 1023A has experienced a tidal interaction with NGC 1023. The model explains some of the pecularities of NGC 1023A, but is probably unable to account for all of the HI mass about NGC 1023.作者: 要求比…更好 時間: 2025-3-23 20:06
The Detailed Velocity Field of the Ionized Gas in the Interacting Pair of Galaxies NGC 2535-36ometer and a two-dimensional photon counting system (the CIGALE equipment). Some 3200 velocity points cover the whole galaxy and its companion with a spatial resolution of 1″5 and a velocity accuracy better than 19 km s.. The redshifts are found to be 4095 km s. ± 10 km s. for NGC 2535 and 4085 km s作者: impale 時間: 2025-3-24 01:37
Kinematics of Interacting Galaxies VV 317: Motions in the Bar of One of the Components=14.8 [2], is a spiral galaxy of type SBc seen face-on. The short broad arms emerge from the ends of the bright bar. The structure of the galaxy disk is of c-d type, it contains small bright HII-regions and a lot of dust.作者: intoxicate 時間: 2025-3-24 02:32
http://image.papertrans.cn/e/image/283971.jpg作者: 加劇 時間: 2025-3-24 09:25 作者: 吹氣 時間: 2025-3-24 12:45
978-3-642-75275-9Springer-Verlag Berlin Heidelberg 1990作者: Missile 時間: 2025-3-24 15:27 作者: Allergic 時間: 2025-3-24 22:22 作者: sparse 時間: 2025-3-25 02:01
Retrograde Streaming in SBO Galaxiesg of part of a galaxy from its main body. Both phenomena indicates the existence of retrograde motions within stellar systems. They appear in galaxies of different morphological type and size, and in spite of their empirical resemblance, it is not completely clear if they represent the same physical process and/or if they have the same origin.作者: Apogee 時間: 2025-3-25 05:38
Structure of the NGC 1023 Systemassume that NGC 1023A has experienced a tidal interaction with NGC 1023. The model explains some of the pecularities of NGC 1023A, but is probably unable to account for all of the HI mass about NGC 1023.作者: 窗簾等 時間: 2025-3-25 08:36 作者: guzzle 時間: 2025-3-25 14:13 作者: 概觀 時間: 2025-3-25 18:43 作者: 妨礙議事 時間: 2025-3-25 21:29 作者: magnate 時間: 2025-3-26 02:53
Waves and Imaging through Complex Mediaassume that NGC 1023A has experienced a tidal interaction with NGC 1023. The model explains some of the pecularities of NGC 1023A, but is probably unable to account for all of the HI mass about NGC 1023.作者: 衣服 時間: 2025-3-26 08:16 作者: FLAIL 時間: 2025-3-26 10:30 作者: TIGER 時間: 2025-3-26 15:55 作者: companion 時間: 2025-3-26 19:58 作者: 袋鼠 時間: 2025-3-27 00:24
Pentti Hakkila,Gerald C. Monela of galaxies at redshifts near 0.4 contained a much larger population of “blue” galaxies than expected. This suggested rapid color evolution of galaxies in 1/3 of a Hubble time. In order to put this on a more quantitative level, Butcher and Oemler (1984a) undertook a photometric study of 33 clusters作者: Ingrained 時間: 2025-3-27 02:28 作者: HOWL 時間: 2025-3-27 08:04 作者: 一美元 時間: 2025-3-27 11:12 作者: 沉思的魚 時間: 2025-3-27 14:15
Eustáquio J. Reis,Fernando A. Blanco they are now perceived as some of the dominant processes governing galaxy formation and evolution. I shall first briefly review the early history of the subject and our recent progress in understanding the six main types of galactic collisions. Then I shall focus on three issues: (1) the fascinatin作者: Ingrained 時間: 2025-3-27 18:41 作者: 沒有貧窮 時間: 2025-3-28 02:00 作者: 鎮(zhèn)痛劑 時間: 2025-3-28 05:25 作者: Mystic 時間: 2025-3-28 06:33
Waves and Imaging through Complex Mediaassume that NGC 1023A has experienced a tidal interaction with NGC 1023. The model explains some of the pecularities of NGC 1023A, but is probably unable to account for all of the HI mass about NGC 1023.作者: 斑駁 時間: 2025-3-28 10:42
Statistical Approach to Photon Localizationometer and a two-dimensional photon counting system (the CIGALE equipment). Some 3200 velocity points cover the whole galaxy and its companion with a spatial resolution of 1″5 and a velocity accuracy better than 19 km s.. The redshifts are found to be 4095 km s. ± 10 km s. for NGC 2535 and 4085 km s作者: 故意 時間: 2025-3-28 17:32
Towards Optical Biopsy: A Brief Introduction=14.8 [2], is a spiral galaxy of type SBc seen face-on. The short broad arms emerge from the ends of the bright bar. The structure of the galaxy disk is of c-d type, it contains small bright HII-regions and a lot of dust.作者: 是限制 時間: 2025-3-28 20:23 作者: 骯臟 時間: 2025-3-29 02:25 作者: follicular-unit 時間: 2025-3-29 03:19
Are High Redshift Galaxies Interacting?hether and to what extent the processes we observe reflect interactions between galaxies and protogalaxies. Sticking to the catholic sense of the title assigned to me, I shall however show that some high-redshift galaxies are definitely interacting with themselves.作者: Ballad 時間: 2025-3-29 09:49 作者: Outspoken 時間: 2025-3-29 12:56
Conference proceedings 1990s, dynamical problems of elliptical and disk galaxies, groups and clusters, starburst and nuclear activity triggered by interactions, merger scenarios, and numerical experiments. Researchers and graduate students, specialists or not, will find here a complete overview of a rapidly growing field of astronomy.作者: aspect 時間: 2025-3-29 18:33
Gas, Dust, and Stellar Populations in the Antennae (NGC 4038/4039)ial exists from the radio to the X-ray domain, the detailed geometry and dynamics of the encounter as well as most of the physical processes induced by the violent interaction have escaped satisfactory selfconsitent explanation so far.作者: Expressly 時間: 2025-3-29 22:28
The Detailed Velocity Field of the Ionized Gas in the Interacting Pair of Galaxies NGC 2535-36spatial resolution of 1″5 and a velocity accuracy better than 19 km s.. The redshifts are found to be 4095 km s. ± 10 km s. for NGC 2535 and 4085 km s. ± 10 km s. for NGC 2536 (heliocentric radial velocities). Assuming a distance of 41 Mpc the masses are found to be around 3 10. M. for the main galaxy and 10. M. for its companion.作者: 甜得發(fā)膩 時間: 2025-3-30 01:19
Ian R. Hunter,Ian R. Calder,Tom Hattonhether and to what extent the processes we observe reflect interactions between galaxies and protogalaxies. Sticking to the catholic sense of the title assigned to me, I shall however show that some high-redshift galaxies are definitely interacting with themselves.作者: 圓木可阻礙 時間: 2025-3-30 04:24 作者: 脫水 時間: 2025-3-30 10:45 作者: 行為 時間: 2025-3-30 15:29
Eustáquio J. Reis,Fernando A. Blanconation of globular cluster ages, and has allowed at least relative ages to be derived with a new level of precision. Despite controversy over many of the details, agreement is beginning to emerge that some very significant age differences do exist among globular clusters.作者: 競選運(yùn)動 時間: 2025-3-30 16:58
Eustáquio J. Reis,Fernando A. Blancok galaxies may have formed through mergers. As we shall see, it now seems likely that the present position of a galaxy in Hubble’s morphological sequence was determined mainly by the number and severity of mergers in its past history.作者: 侵略主義 時間: 2025-3-30 22:58
Are Our Globular Clusters Coeval?nation of globular cluster ages, and has allowed at least relative ages to be derived with a new level of precision. Despite controversy over many of the details, agreement is beginning to emerge that some very significant age differences do exist among globular clusters.
