標(biāo)題: Titlebook: Cooling Flows in Clusters and Galaxies; A. C. Fabian Book 1988 Kluwer Academic Publishers 1988 cosmic ray.cosmology.observatory.quasar.rel [打印本頁] 作者: Assert 時間: 2025-3-21 17:23
書目名稱Cooling Flows in Clusters and Galaxies影響因子(影響力)
書目名稱Cooling Flows in Clusters and Galaxies影響因子(影響力)學(xué)科排名
書目名稱Cooling Flows in Clusters and Galaxies網(wǎng)絡(luò)公開度
書目名稱Cooling Flows in Clusters and Galaxies網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Cooling Flows in Clusters and Galaxies被引頻次
書目名稱Cooling Flows in Clusters and Galaxies被引頻次學(xué)科排名
書目名稱Cooling Flows in Clusters and Galaxies年度引用
書目名稱Cooling Flows in Clusters and Galaxies年度引用學(xué)科排名
書目名稱Cooling Flows in Clusters and Galaxies讀者反饋
書目名稱Cooling Flows in Clusters and Galaxies讀者反饋學(xué)科排名
作者: 顛簸下上 時間: 2025-3-21 20:15 作者: conformity 時間: 2025-3-22 02:58
tical and systematic error on the derived physical parameters. Of these 106 clusters, 43 have central cooling times < 2 × 10. years and hence are designated ‘cooling flows’. Mass accretion rates range from ~ 1 - 500 M. yr..作者: Introduction 時間: 2025-3-22 04:34 作者: GLEAN 時間: 2025-3-22 10:38 作者: 令人心醉 時間: 2025-3-22 14:33
th three models, 1) the addition of a cool to a hot component, 2) a power law distribution of emission measure with temperature and 3) a cooling flow model. We find strong evidence for the existence of cool components in the centers of these clusters. The derived distribution of emission measure ver作者: 令人心醉 時間: 2025-3-22 18:21 作者: 兵團(tuán) 時間: 2025-3-22 23:25 作者: 妨礙議事 時間: 2025-3-23 03:38 作者: In-Situ 時間: 2025-3-23 07:23 作者: 玉米 時間: 2025-3-23 10:12
t with the inflow rates predicted by X-ray data if the initial mass function resembles that in our Galaxy. It seems most likely that the bulk of the inflow in the clusters as well as in normal gE galaxies is deposited in the form of very low mass stars with 〈.〉 ? 0.7 M.. This efficient, low mass mod作者: Interim 時間: 2025-3-23 14:56 作者: sorbitol 時間: 2025-3-23 18:09
bjectives are to search for extended blue continuum regions indicative of star formation, to study the spatial distribution of star formation, and to make a quantitative measure of the amount of light from young stars, which can lead to a measure of the star formation rate (for an assumed intial mas作者: 體貼 時間: 2025-3-24 01:55 作者: 提名的名單 時間: 2025-3-24 03:33
Die Verbreitung von Brustkrebs,or collimated ejection in PA 160 degrees. Outside this the radio structure bends rapidly by approximately 90 degrees before merging into the 10′ radio halo. It is suggested that the relativistic gas, which is responsible for the radio emission, may have a considerable effect on any cooling inflow , 作者: 要控制 時間: 2025-3-24 07:56
Die Verbreitung von Brustkrebs,covering [OII]λ3727, H., [OIII] λ5007 and [SII]λλ6717, 6730 are presented. The line ratios are shown to be incompatible with the simplest model in which the gas is photoionized by a central active nucleus and lies at its projected distance from the nucleus.作者: 口味 時間: 2025-3-24 11:54 作者: Ballerina 時間: 2025-3-24 18:45
With the Westerbork Synthesis Radio Telescope (WSRT) we detect HI absorption at 5250 km/s in front of the nucleus of NGC 1275, with an optical depth of .003 and a dispersion of 205 km/s. We do not detect HI associated with the 30″ halo in absorption or emission.作者: 狼群 時間: 2025-3-24 22:49
Eine Entwicklungsgeschichte der Brust,We show that the excitation of the filaments observed around NGC 1275 is more probably due to photoionization by the active nucleus radiation than to local radiative shocks. The photoionized gas is in pressure equilibrium with the hot ambient gas of the cooling flow.作者: 過于平凡 時間: 2025-3-25 02:25
Characteristics of Extended Gas Around Radio Galaxies,A qualitative description is given of spectral properties, dynamical behaviour and morphology of a selection of mainly southern radio galaxies which have been observed to have extended ionized gas in their vicinity. The question of the significance of this gas in relation to cooling flows is still very much an open one.作者: 音樂會 時間: 2025-3-25 06:58 作者: 精美食品 時間: 2025-3-25 07:37 作者: 并排上下 時間: 2025-3-25 12:05
https://doi.org/10.1007/978-94-009-2953-1cosmic ray; cosmology; observatory; quasar; relativistic jet; star; star formation作者: aggravate 時間: 2025-3-25 17:21
978-94-010-7828-3Kluwer Academic Publishers 1988作者: 領(lǐng)導(dǎo)權(quán) 時間: 2025-3-25 20:03 作者: 蘆筍 時間: 2025-3-26 00:16
tical and systematic error on the derived physical parameters. Of these 106 clusters, 43 have central cooling times < 2 × 10. years and hence are designated ‘cooling flows’. Mass accretion rates range from ~ 1 - 500 M. yr..作者: CRUE 時間: 2025-3-26 08:22
ifficult or impossible to reproduce the observed temperature gradient while also reducing the net rate at which cooled gas is produced. None of the models examined lead to a viable alternative cooling flow scenario.作者: 波動 時間: 2025-3-26 09:34 作者: Outshine 時間: 2025-3-26 14:40 作者: 是剝皮 時間: 2025-3-26 19:08 作者: Angioplasty 時間: 2025-3-26 22:06
Alternative Cooling Flow Models,ifficult or impossible to reproduce the observed temperature gradient while also reducing the net rate at which cooled gas is produced. None of the models examined lead to a viable alternative cooling flow scenario.作者: judicial 時間: 2025-3-27 04:09 作者: 收藏品 時間: 2025-3-27 05:59
Cooling Flow Filaments and the Emission-Line Gas in NGC1275,covering [OII]λ3727, H., [OIII] λ5007 and [SII]λλ6717, 6730 are presented. The line ratios are shown to be incompatible with the simplest model in which the gas is photoionized by a central active nucleus and lies at its projected distance from the nucleus.作者: lipids 時間: 2025-3-27 11:57 作者: affect 時間: 2025-3-27 15:20 作者: LUT 時間: 2025-3-27 18:52 作者: CHOP 時間: 2025-3-28 01:54
he free parameters involved are totally different. We feel that the agreement between the three . experiments is good and gives weight to the the numerical values of ? for the larger sample of objects observed only with the . IPC and HRI.作者: 假裝是我 時間: 2025-3-28 05:31
l data. Although our estimates are formally only upper limits to the actual values of ? if the gas is being heated by some mechanism, this agreement is circumstantial evidence in favor of the existence of substantial cooling flows and against the dominance of conduction or other heat sources. For Pe作者: IRS 時間: 2025-3-28 08:55 作者: perpetual 時間: 2025-3-28 14:26 作者: 值得尊敬 時間: 2025-3-28 14:54
Properties of Clusters of Galaxies,hich the cooling flow environment, which appears to be ubiquitous in the early-type galactic systems which form the hosts for strong radio sources, may affect the origin and structure of the radio emitting regions.作者: 四溢 時間: 2025-3-28 21:32 作者: 臥虎藏龍 時間: 2025-3-29 02:04 作者: 錫箔紙 時間: 2025-3-29 03:31 作者: 苦笑 時間: 2025-3-29 07:33
Book 1988usters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in作者: grovel 時間: 2025-3-29 14:47 作者: Largess 時間: 2025-3-29 19:17 作者: FLAT 時間: 2025-3-29 21:22
Dynamics of Cosmic Rays in Cooling Flows,s interaction by means of steady models with spherical symmetry. It was found that the cosmic ray pressure may become comparable to the gas pressure in the halo region around a central galaxy with a cooling flow. Rayleigh Taylor instabilities might develop there and set the scale for inhomogeneities leading to filaments or star formation regions.作者: engender 時間: 2025-3-30 01:28 作者: Minuet 時間: 2025-3-30 08:08 作者: barium-study 時間: 2025-3-30 08:50
Radio Observations of NGC1275 at 90 and 20cm, halo. It is suggested that the relativistic gas, which is responsible for the radio emission, may have a considerable effect on any cooling inflow , and should be taken into account in models of such phenomena.作者: NAG 時間: 2025-3-30 15:17
s function). Four clusters with large .s and large cluster H. emission fluxes are found to have an excess of blue light concentrated to the centers of the cluster central galaxy. Assumption of a disk IMF leads to the conclusion that the starlight might play a major role in ionizing the emission line gas in these clusters.作者: insightful 時間: 2025-3-30 16:44 作者: 縮影 時間: 2025-3-30 21:10
od for deriving quantitative parameters (gas densities and cooling times) is described and the results are compared with other techniques for estimating the importance of cooling. Finally, several effects of cooling flows around galaxies in clusters are discussed.作者: Flounder 時間: 2025-3-31 01:03
nk for the cooling gas produces a gradual drop in temperature toward the cluster center in agreement with X-ray measurements. Heat conduction can suppress the accretion rate by a factor of a few to several, while larger reductions result in a nearly isothermal Intra-Cluster Medium.作者: Neolithic 時間: 2025-3-31 07:46 作者: ingrate 時間: 2025-3-31 09:45
X-ray emission is more closely related to the stellar content of Es than are the HI or infrared emission, suggesting that the hot gas originates in mass loss from stars while the cold gas is the remains of the original interstellar medium plus accretion from outside the galaxy.作者: 阻撓 時間: 2025-3-31 13:53
nflow in the clusters as well as in normal gE galaxies is deposited in the form of very low mass stars with 〈.〉 ? 0.7 M.. This efficient, low mass mode of star formation is a plausible candidate for the dark matter.作者: 支形吊燈 時間: 2025-3-31 20:35
Die Verbreitung von Brustkrebs, halo. It is suggested that the relativistic gas, which is responsible for the radio emission, may have a considerable effect on any cooling inflow , and should be taken into account in models of such phenomena.作者: floodgate 時間: 2025-4-1 01:05
Color Gradients in Cooling Flow Cluster Central Galaxies and the Ionization of Cluster Emission Lins function). Four clusters with large .s and large cluster H. emission fluxes are found to have an excess of blue light concentrated to the centers of the cluster central galaxy. Assumption of a disk IMF leads to the conclusion that the starlight might play a major role in ionizing the emission line gas in these clusters.作者: 來就得意 時間: 2025-4-1 05:49 作者: 發(fā)酵 時間: 2025-4-1 09:25 作者: DRAFT 時間: 2025-4-1 12:06
Properties of Clusters of Galaxies,gers will tend to disrupt cooling flows. I suggest that the recently observed luminous arcs in clusters may be shocks generated by a subcluster merger in a cluster with a cooling flow. The peaked galaxy distributions and radial orbits suggested by recent studies of clusters will lead to a larger num作者: 強制性 時間: 2025-4-1 14:27 作者: MIR 時間: 2025-4-1 21:36
A Catalog(UE) of Cooling Flows,tical and systematic error on the derived physical parameters. Of these 106 clusters, 43 have central cooling times < 2 × 10. years and hence are designated ‘cooling flows’. Mass accretion rates range from ~ 1 - 500 M. yr..作者: 男生戴手銬 時間: 2025-4-2 01:53
