Titlebook: Disks and Outflows Around Young Stars; Proceedings of a Con Steven Beckwith,Jakob Staude,Antonella Natta Conference proceedings 1996 Spring

CULT

书目名称Disks and Outflows Around Young Stars影响因子(影响力)




书目名称Disks and Outflows Around Young Stars影响因子(影响力)学科排名




书目名称Disks and Outflows Around Young Stars网络公开度




书目名称Disks and Outflows Around Young Stars网络公开度学科排名




书目名称Disks and Outflows Around Young Stars被引频次




书目名称Disks and Outflows Around Young Stars被引频次学科排名




书目名称Disks and Outflows Around Young Stars年度引用




书目名称Disks and Outflows Around Young Stars年度引用学科排名




书目名称Disks and Outflows Around Young Stars读者反馈




书目名称Disks and Outflows Around Young Stars读者反馈学科排名

壮观的游行

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

宪法没有

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

Optimum

格子架

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

花束

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

花束

服从

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

incisive

Flustered

,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