標題: Titlebook: Cores to Clusters; Star Formation with M. S. N. Kumar,M. Tafalla,P. Caselli Conference proceedings 2005 Springer-Verlag New York 2005 Astr [打印本頁] 作者: HAVEN 時間: 2025-3-21 18:02
書目名稱Cores to Clusters影響因子(影響力)
書目名稱Cores to Clusters影響因子(影響力)學(xué)科排名
書目名稱Cores to Clusters網(wǎng)絡(luò)公開度
書目名稱Cores to Clusters網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Cores to Clusters被引頻次
書目名稱Cores to Clusters被引頻次學(xué)科排名
書目名稱Cores to Clusters年度引用
書目名稱Cores to Clusters年度引用學(xué)科排名
書目名稱Cores to Clusters讀者反饋
書目名稱Cores to Clusters讀者反饋學(xué)科排名
作者: Expressly 時間: 2025-3-21 22:35 作者: 懶惰人民 時間: 2025-3-22 01:41 作者: 嚴峻考驗 時間: 2025-3-22 05:36
Studying Protostellar Jets through a Combined Infrared/Optical Spectral Analysisr jets in the star formation process (removal of excess angular momentum, dispersion of infalling enevlope, injection of turbolence for cloud support). Moreover, we investigated the abundances of refractory emitting species such as Carbon, Calcium and Iron. The depletion of these species with respec作者: 他一致 時間: 2025-3-22 10:25
Conference proceedings 2005ometimes we have chosen to organize int- national conferences of a larger size. On other occasions the choice has been for smaller and more informal discussion meetings. Or even doctoral schools with very different objectives. In common all those meetings have always had, besides the formal register作者: lymphedema 時間: 2025-3-22 14:41 作者: lymphedema 時間: 2025-3-22 17:30 作者: 肉體 時間: 2025-3-23 01:11 作者: 會犯錯誤 時間: 2025-3-23 02:36 作者: Conducive 時間: 2025-3-23 06:37
Thomas H. Murray,Arthur L. Caplanr jets in the star formation process (removal of excess angular momentum, dispersion of infalling enevlope, injection of turbolence for cloud support). Moreover, we investigated the abundances of refractory emitting species such as Carbon, Calcium and Iron. The depletion of these species with respec作者: libertine 時間: 2025-3-23 11:25
Preliminary Results on Newly Discovered Embedded Clustersnitude. To date we have observed 25 of the 346 clusters found by Bica and Dutra (2003). We constructed near-IR color-color diagrams to identify PMS stars in the clusters and examined the distribution of these stars in the cluster field. In this proceeding we show the results concerning three candidates of our survey.作者: SNEER 時間: 2025-3-23 14:10 作者: 姑姑在炫耀 時間: 2025-3-23 21:24 作者: 泥沼 時間: 2025-3-23 23:40 作者: 書法 時間: 2025-3-24 03:28 作者: opprobrious 時間: 2025-3-24 09:18
0067-0057 er and millimeter wave bands will become operationalIt was with pleasure that CAUP became for three days the core to the cloud of star formation experts all over the world. Close to the celebration of its 15th anniversary – therefore still in the early stages of institutional evolution – we are prou作者: 枯萎將要 時間: 2025-3-24 13:52 作者: 翅膀拍動 時間: 2025-3-24 16:45 作者: 整頓 時間: 2025-3-24 19:16
Controlled Singularly Perturbed Systems,ery recently, puts us in a very good position to plan rich and fruitful observative campaigns with the instruments being developed for astronomy at IR, submm amd mm wavelengths, in interferometric or single-telescope modes.作者: 無力更進 時間: 2025-3-25 00:36
Management of Radioactive Wastes,d is not affected by the problems mentioned above, which makes it a privileged target for studying not only PMS evolution and BDs but also offers a valuable opportunity to study the IMF well down into the substellar regime.作者: 草率男 時間: 2025-3-25 07:03 作者: NATTY 時間: 2025-3-25 09:42
Protostellar Jets: A High Angular Resolution Perspectiveery recently, puts us in a very good position to plan rich and fruitful observative campaigns with the instruments being developed for astronomy at IR, submm amd mm wavelengths, in interferometric or single-telescope modes.作者: 悠然 時間: 2025-3-25 11:41
Pre-Main-Sequence Evolutionand Brown Dwarfs Beyond the Solar Vicinityd is not affected by the problems mentioned above, which makes it a privileged target for studying not only PMS evolution and BDs but also offers a valuable opportunity to study the IMF well down into the substellar regime.作者: 大量殺死 時間: 2025-3-25 17:56 作者: Outmoded 時間: 2025-3-25 23:58
https://doi.org/10.1007/978-1-4612-4482-0vironments, how do individual stars form and gain mass? Can a forming star cluster be treated as an equilibrium system or is this process too rapid for equilibrium to be established? How does feedback affect the formation process?作者: 描述 時間: 2025-3-26 04:02 作者: cauda-equina 時間: 2025-3-26 04:20
The Birth of Massive Stars and Star Clustersvironments, how do individual stars form and gain mass? Can a forming star cluster be treated as an equilibrium system or is this process too rapid for equilibrium to be established? How does feedback affect the formation process?作者: 積習(xí)已深 時間: 2025-3-26 10:46
Infrared Study of the Southern Galactic Star Forming Region Associated with Iras 10049-5657ased on the MSX data (8, 12, 14, & 21 μm bands). Radiative transfer modelling has been carried out taking into account all available infrared measurements to obtain various physical parameters like nature of the exciting source, geometrical dimensions, dust distribution and composition etc.作者: QUAIL 時間: 2025-3-26 14:36 作者: Mnemonics 時間: 2025-3-26 17:28 作者: BURSA 時間: 2025-3-26 23:49 作者: 鋸齒狀 時間: 2025-3-27 01:28 作者: Paleontology 時間: 2025-3-27 06:56
Jayne Dolph,Danny Marks,George A. Kingmation of a star. In this review, I discuss the basic processes governing the physical characteristics of such cores as well as the techniques used to determine such parameters as density, temperature, and magnetic field strength.作者: Libido 時間: 2025-3-27 10:33 作者: Intersect 時間: 2025-3-27 14:38
F. J. Swanson,R. P. Neilson,G. E. Grantplic-ity and proximity, dense cores offer the clearest view of the different phases of star formation, in particular the conditions prior to the onset of gravitational col-lapse. Thanks to the combined analysis of the emission from molecular lines and the emission/absorption from dust grains, the la作者: myalgia 時間: 2025-3-27 21:28 作者: 偽造 時間: 2025-3-27 23:51 作者: Mutter 時間: 2025-3-28 03:50
https://doi.org/10.1007/978-1-4612-4482-0ntain stars drawn from an approximately universal initial mass function, so that almost all rich young star clusters contain massive stars. In this review I discuss the physical processes associated with both massive star formation and with star cluster formation. First I summarize the observed prop作者: Ingrained 時間: 2025-3-28 10:13
The Chelgraph SGML Structured Editoraracteristics of precursors of UCHII regions and their likely evolutionary properties. The second section discusses massive molecular outflows, their implications for high-mass star formation, and a possible evolutionary sequence for massive outflows.作者: AGOG 時間: 2025-3-28 10:57 作者: esculent 時間: 2025-3-28 16:02
The Chelgraph SGML Structured Editorld reverse the infall thus preventing further growth of the stellar mass. After illustrating the two models proposed to solve this problem (“accretion” and “coalescence”), we review the observational evidence pro/contra such models, focusing on rotating disk-like structures detected in association w作者: exorbitant 時間: 2025-3-28 20:29
M. Woodman,D. Ince,J. Preece,G. Daviesmarkable progress toward understanding star formation due to advances in observational technology especially at infrared and millimeter wavelengths which allow direct observation of the sites of star birth. Such observations suggest that embedded clusters may be the fundamental units of star formati作者: anthesis 時間: 2025-3-29 02:29 作者: abracadabra 時間: 2025-3-29 04:13 作者: 很是迷惑 時間: 2025-3-29 08:41 作者: 刺激 時間: 2025-3-29 11:32 作者: 后退 時間: 2025-3-29 19:36
Thomas H. Murray,Arthur L. Caplanture and to prepare for the observations with high angular resolution, we have studied the conditions of the plasma along a sample of ‘classical’ Herbig-Haro (HH) jets through a combined optical-infrared diagnostics. Here we present and discuss the results obtained for the HH 1 and HH 34 jets. We ap作者: conscience 時間: 2025-3-29 23:42
“Suffer the Little Children ...”during a systematic search of the 2MASS database. The aim of our survey was to reobserve these objects with better spatial resolution and limiting magnitude. To date we have observed 25 of the 346 clusters found by Bica and Dutra (2003). We constructed near-IR color-color diagrams to identify PMS st作者: 煩擾 時間: 2025-3-30 01:40
https://doi.org/10.1007/b137447Astrophysics; Clusters; Kumar; relativistic jet; star作者: 生來 時間: 2025-3-30 07:32
978-1-4419-2088-1Springer-Verlag New York 2005作者: Hallmark 時間: 2025-3-30 09:00 作者: 周年紀念日 時間: 2025-3-30 14:03
Brown DwarfsHundreds of brown dwarfs have been discovered since 1995. These objects are likely to populate every region of our Galaxy and possibly other galaxies in comparable number to stars. We briefly review their basic properties, mass function, spatial distribution and possible formation scenarios.作者: 繁榮中國 時間: 2025-3-30 20:02 作者: 吝嗇性 時間: 2025-3-30 22:01 作者: SLING 時間: 2025-3-31 04:56
Cores to Clusters978-0-387-26357-1Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: crucial 時間: 2025-3-31 05:25
Jayne Dolph,Danny Marks,George A. Kingmation of a star. In this review, I discuss the basic processes governing the physical characteristics of such cores as well as the techniques used to determine such parameters as density, temperature, and magnetic field strength.作者: 做事過頭 時間: 2025-3-31 12:53
The Chelgraph SGML Structured Editoraracteristics of precursors of UCHII regions and their likely evolutionary properties. The second section discusses massive molecular outflows, their implications for high-mass star formation, and a possible evolutionary sequence for massive outflows.作者: 數(shù)量 時間: 2025-3-31 14:37
M. S. N. Kumar,M. Tafalla,P. CaselliWell-known international contributors.Timely publication as shortly, several major telescope facilities operating in the infrared ubmillimeter and millimeter wave bands will become operational作者: 厚顏 時間: 2025-3-31 18:09 作者: triptans 時間: 2025-3-31 23:16
