標題: Titlebook: Disks and Outflows Around Young Stars; Proceedings of a Con Steven Beckwith,Jakob Staude,Antonella Natta Conference proceedings 1996 Spring [打印本頁] 作者: CULT 時間: 2025-3-21 16:53
書目名稱Disks and Outflows Around Young Stars影響因子(影響力)
書目名稱Disks and Outflows Around Young Stars影響因子(影響力)學科排名
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書目名稱Disks and Outflows Around Young Stars網(wǎng)絡公開度學科排名
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書目名稱Disks and Outflows Around Young Stars讀者反饋
書目名稱Disks and Outflows Around Young Stars讀者反饋學科排名
作者: 壯觀的游行 時間: 2025-3-21 21:05
Circumstellar disks in the Trapezium Cluster,ts sometimes called ‘proplyds’, as revealed by ionizing radiation from the central massive OB stars of the Trapezium, and the fraction of these ionized objects that are associated with stars. Second, we look at the wider cluster population and the statistical occurrence of circumstellar disks detect作者: 憲法沒有 時間: 2025-3-22 02:44
High resolution observations of disks around protostellar sources with the Nobeyama Millimeter Arrastellar disks at 3 mm shows that the 3 mm continuum emission tends to be weaker for embedded sources than for visible T Tauri stars, which is consistent with our previous interpretation of protoplanetary disk formation. The CS gas around L1489 and IRAS 04365+2535 show disk-like structures of ～1000 A作者: Optimum 時間: 2025-3-22 07:39 作者: 格子架 時間: 2025-3-22 09:22
Physical processes in circumstellar disks,h disk accretion and secondary bodies within the disk. Next, we consider the viscous evolution of disks and the possible sources of the viscosity. We briefly consider magnetic instabilities tidal effects, and vortex motions. We also discuss the process of planet formation作者: 花束 時間: 2025-3-22 15:15
The FU orionis outburst as a thermal accretion event: Theoretical and observational implications,-averaged rate of (1–10)×10. M./yr around some fraction (≈10%) of young stellar objects. Accretion through the inner parts of these disks is self regulated by the thermal ionization instability such that long periods (≈1000 .) of low mass flux: (1–10)×10. M./yr, are punctuated by short periods (≈100作者: 花束 時間: 2025-3-22 19:50 作者: 服從 時間: 2025-3-22 22:25
Neutral gas in the vicinity of Herbig AeBe stars: What can we learn from red-shifted sodium absorptlgol-type minima. The existence of neutral sodium in the environment of relatively hot stars, such as UX Ori (spectral type A3) cannot be easily explained. We present here the preliminary results of calculations aimed at exploring under which physical conditions a sizable amount of neutral sodium ca作者: incisive 時間: 2025-3-23 05:01 作者: Flustered 時間: 2025-3-23 06:36
,A massive “core” associated with the UC H, region G31.41+0.31,egion G31.41+0.31. We also obtained a map of the continuum emission at a frequency of 110 GHz. We detect a hot molecular core in the emission both of methyl cyanide and of the 110 GHz continuum. We estimate a temperature of 200 K and a mass of 1000 M. for this compact massive region. We also detect 作者: Conserve 時間: 2025-3-23 11:42
Prediction of stellar mass in star formation: Theory and its application to the orion a cloud,tellar core mainly through an accretion disk, a significant fraction of the mass outflow and ultraviolet radiation escapes from the inner region without interacting with the infalling matter and disturbs the cloud core matter which has not yet contracted much. A highvelocity mass outflow gradually p作者: Type-1-Diabetes 時間: 2025-3-23 15:38 作者: 嬉耍 時間: 2025-3-23 20:51
Molecular entrainment by optical jets,y the most popular are those which invoke momentum-conserving collimated jets, emanating from the YSO. Two competing models describe the mechanism by which the jet sets the molecular cloud in motion: ‘prompt’ entrainment and ‘turbulent’ entrainment. We present a method for distinguishing between the作者: narcissism 時間: 2025-3-23 23:03
HH 212: The most beautiful protostellar jet known to date,not far from the famous Horsehead Nebula, and is about 0.3 pc long on either side. Each side contains an inner series of spatially resolved knots (with inter-knot emission) and an outer series of giant bow-shocks, all seen in the v=1?0 S(1) line of shock excited H. at 2.12 μm. Each pair of bow-shock作者: 激怒 時間: 2025-3-24 03:08 作者: 前兆 時間: 2025-3-24 09:40 作者: 啞巴 時間: 2025-3-24 14:36
Meldepflicht von Erbkrankheiten, even beyond. Here, techniques by which the small-scale circumstellar material can be detected are described and evidence for disks is briefly reviewed. Because of the general similarity between the disks around solar-mass stars and the nebula that surrounded the sun as the planets formed, disk prop作者: Atrium 時間: 2025-3-24 15:27
,Untersuchung mit R?ntgenstrahlen,ts sometimes called ‘proplyds’, as revealed by ionizing radiation from the central massive OB stars of the Trapezium, and the fraction of these ionized objects that are associated with stars. Second, we look at the wider cluster population and the statistical occurrence of circumstellar disks detect作者: 起草 時間: 2025-3-24 20:32 作者: Magisterial 時間: 2025-3-25 02:21 作者: 樸素 時間: 2025-3-25 05:16 作者: 緯度 時間: 2025-3-25 09:10
Parasiten und Infektionskrankheiten,-averaged rate of (1–10)×10. M./yr around some fraction (≈10%) of young stellar objects. Accretion through the inner parts of these disks is self regulated by the thermal ionization instability such that long periods (≈1000 .) of low mass flux: (1–10)×10. M./yr, are punctuated by short periods (≈100作者: 柔聲地說 時間: 2025-3-25 12:27 作者: creatine-kinase 時間: 2025-3-25 19:12 作者: Synchronism 時間: 2025-3-25 21:02
,Untersuchung mit R?ntgenstrahlen, at understanding the formation of young stellar objects (YSOs) through the use of near-infrared spectroscopy. Over the past 18 months, we have carried out an extensive survey of fundamental MK spectral standard stars in the near-infrared spanning luminosity classes I–II, III, and IV–V from spectral作者: 預感 時間: 2025-3-26 00:43
https://doi.org/10.1007/978-3-662-30056-5egion G31.41+0.31. We also obtained a map of the continuum emission at a frequency of 110 GHz. We detect a hot molecular core in the emission both of methyl cyanide and of the 110 GHz continuum. We estimate a temperature of 200 K and a mass of 1000 M. for this compact massive region. We also detect 作者: 發(fā)炎 時間: 2025-3-26 06:00
Analyse der pathologischen Konkremente,tellar core mainly through an accretion disk, a significant fraction of the mass outflow and ultraviolet radiation escapes from the inner region without interacting with the infalling matter and disturbs the cloud core matter which has not yet contracted much. A highvelocity mass outflow gradually p作者: covert 時間: 2025-3-26 12:33 作者: triptans 時間: 2025-3-26 16:42
Die Grundbegriffe der Hautkrankheiten,y the most popular are those which invoke momentum-conserving collimated jets, emanating from the YSO. Two competing models describe the mechanism by which the jet sets the molecular cloud in motion: ‘prompt’ entrainment and ‘turbulent’ entrainment. We present a method for distinguishing between the作者: coagulate 時間: 2025-3-26 20:38
https://doi.org/10.1007/978-3-662-30067-1not far from the famous Horsehead Nebula, and is about 0.3 pc long on either side. Each side contains an inner series of spatially resolved knots (with inter-knot emission) and an outer series of giant bow-shocks, all seen in the v=1?0 S(1) line of shock excited H. at 2.12 μm. Each pair of bow-shock作者: BRIDE 時間: 2025-3-26 21:40
Physical processes in circumstellar disks,h disk accretion and secondary bodies within the disk. Next, we consider the viscous evolution of disks and the possible sources of the viscosity. We briefly consider magnetic instabilities tidal effects, and vortex motions. We also discuss the process of planet formation作者: assent 時間: 2025-3-27 02:58 作者: Seminar 時間: 2025-3-27 07:04
978-3-662-15720-6Springer-Verlag Berlin Heidelberg 1996作者: 愛得痛了 時間: 2025-3-27 11:36
Lecture Notes in Physicshttp://image.papertrans.cn/e/image/281394.jpg作者: 碌碌之人 時間: 2025-3-27 15:57
The FU orionis outburst as a thermal accretion event: Theoretical and observational implications,iscosity has implications for self gravity as a possible mass transport mechanism through much of the disk. Light curves of V1515 Cyg, FU Ori, and V1057 Cyg are reproduced, and model results are compared to observations.作者: 誘惑 時間: 2025-3-27 18:00
The stellar populations of deeply embedded young clusters: Near-infrared spectral classification,sample covers a range of spectral types and disk accretion rates including classical and weak-lined T Tauri stars. Results suggest that spectral types derived from infrared spectra agree with their optically derived counterparts to within a few subclasses for late-type stars. Further, weak-lined T T作者: Exhilarate 時間: 2025-3-28 00:30 作者: Parabola 時間: 2025-3-28 05:40 作者: 人類學家 時間: 2025-3-28 09:13
Keplerian circumstellar disks in Taurus: The GG Tau Ring and the DM Tau Disk,作者: 大廳 時間: 2025-3-28 12:43 作者: 駭人 時間: 2025-3-28 17:09
Numerical simulations of the formation of binary and multiple protostellar disks, starting from dyn作者: 圓木可阻礙 時間: 2025-3-28 22:06
Multiplicity in the Opiuchus and Taurus star forming regions,作者: 關(guān)節(jié)炎 時間: 2025-3-29 00:12 作者: 航海太平洋 時間: 2025-3-29 06:40 作者: 佛刊 時間: 2025-3-29 10:13 作者: Definitive 時間: 2025-3-29 11:28 作者: BRAVE 時間: 2025-3-29 16:23 作者: Factorable 時間: 2025-3-29 20:47 作者: 鞭打 時間: 2025-3-30 01:13 作者: MEEK 時間: 2025-3-30 04:48
High resolution observations of disks around protostellar sources with the Nobeyama Millimeter Arrant with our previous interpretation of protoplanetary disk formation. The CS gas around L1489 and IRAS 04365+2535 show disk-like structures of ～1000 AU in radius. A .CO observation of HL Tau indicates direct evidence of dynamical infalling motion. We discuss the formation of a centrifugally supported viscous accretion disk around HL Tau.作者: 明確 時間: 2025-3-30 10:39
Neutral gas in the vicinity of Herbig AeBe stars: What can we learn from red-shifted sodium absorptined. We present here the preliminary results of calculations aimed at exploring under which physical conditions a sizable amount of neutral sodium can survive in the immediate vicinity of such a star. Spectral lines of circumstellar origin of other elements are also discussed.作者: jet-lag 時間: 2025-3-30 14:37
,A massive “core” associated with the UC H, region G31.41+0.31,methyl cyanide and of the 110 GHz continuum. We estimate a temperature of 200 K and a mass of 1000 M. for this compact massive region. We also detect a velocity gradient or shift across the methyl cyanide core whose origin could be due to rotation.作者: Callus 時間: 2025-3-30 19:28
Die Grundbegriffe der Hautkrankheiten, two cases by examining the velocity structure and the morphology of outflows. We also examine the effects on the observations of viewing angle and show how two well-studied outflows fit into the global picture of jet-molecular cloud interaction. Finally we show evidence for time-dependent ejection of the jet.作者: semiskilled 時間: 2025-3-30 21:00 作者: stressors 時間: 2025-3-31 02:50
Conference proceedings 1996possible connections to planetary systems and stellar astrophysics makes these topics especially broad, appealing to generalists and specialists alike. The CD not only contains papers that could not be printed in the book but allows the authors to include a fair amount of data, often displayed as color images.作者: 填料 時間: 2025-3-31 08:36 作者: Canopy 時間: 2025-3-31 10:31
,Untersuchung mit R?ntgenstrahlen,d objects that are associated with stars. Second, we look at the wider cluster population and the statistical occurrence of circumstellar disks detected through the more traditional signature of infrared excess. Both techniques reveal that a large fraction (≈50–80%) of the young stars in the Trapezium Cluster are likely surrounded by disks.作者: 財政 時間: 2025-3-31 16:44 作者: Pert敏捷 時間: 2025-3-31 17:46
https://doi.org/10.1007/978-3-662-30058-9ined. We present here the preliminary results of calculations aimed at exploring under which physical conditions a sizable amount of neutral sodium can survive in the immediate vicinity of such a star. Spectral lines of circumstellar origin of other elements are also discussed.
