Titlebook: Jets in Young Stellar Objects; Theory and Observati A. J. L. Fernandes,P. J. V. Garcia,J. J. G. Lima Book 2003 Springer Science+Business Me

Maximizer

Respond

浪費(fèi)物質(zhì)

T.A. Gardiner,A. Frank,E.G. Blackman,S.V. Lebedev,J.P. Chittenden,D. Ampleford,S.N. Bland,A. Ciardi,

類型

K. Tsinganos,N. Vlahakis,S. Bogovalov,C. Sauty,E. Trussoni,J.J.G. Lima

簡(jiǎn)潔

The Structure of Young Stellar Jets and Winds Revealed By High Resolution [Fe Ii] λL.644μM Line Obseinig a broad line width. The HVC is located farther away from the origin and is more extended than the LVC. Our results suggest that the HVC is a well-collimated jet originating from the region close to the star, while the LVC is a widely-opened wind accelerated in the region near the inner edge of the accretion disk.

要素

Photoionization of Cool Mhd Disk Windstar. However, it is difficult to foresee how temperatures as high as ～ 5 x 10. can be reached unless a significant fraction of the X-rays radiation is produced by magnetic reconnection at the boundary between the stellar magnetosphere and the accretion disk.

值得尊敬

推延

Magnetic Star-Disk Interaction in Classical T Tauri Systemsa solar-mass central star, an accretion rate of 10..⊙/., and a viscosity parameter αss = 0.01, a field strength of 1 kG, measured at the poles on the surface of the star, was found insufficient for disk disruption.

Banister

挑剔為人

Hh 111 Stis Observations and Their Analysis Using Analytical and Numerical Modelsall bowshock within the jet beam. In this paper we present a long-slit spectrum of Herbig-Haro object HH 111 obtained with STIS and an interpretation of this observation in terms of an ejection velocity variability model.