On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer

Details On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer

2010-11-04

arxiv.org/abs/1011.1230v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

10 figures, Monthly Notices of the Royal Astronomical Society, in press

Scientific paper

Ultraviolet observations of classical T Tauri Stars (cTTSs) have shown that there is a hot (Te ~ 80,000 K) and dense (ne ~ 1e10 cm-3) component associated with the large scale jet. This hot component is formed very close to the base of the jet providing fundamental information on the jet formation mechanism. In this series, we have investigated whether this component can be formed in disc winds, either cool or warm. To conclude the series, jet launching from the interface between the magnetic rotor (the star) and the disc is studied. Synthetic profiles are calculated from numerical simulations of outflow launching by star-disc interaction. Profiles are calculated for several possible configurations of the stellar field: dipolar (with surface strengths, B of 1, 2 and 5 kG) or dynamo fed. Also two types of discs, passive or subjected to an alpha/Omega-dynamo, are considered. These profiles have been used to define the locus of the various models in the observational diagram: dispersion versus centroid, for the profiles of the SiIII] line. Bulk motions produce an increasing broadening of the profile as the lever arm launching the jet becomes more efficient; predicted profiles are however, sensitive to the disc inclination. Models are compared with observations of the SiIII] lines obtained with the Hubble Space Telescope. In addition, it is shown that the non-stationary nature of star-disc winds produce a flickering of the profile during quiescence with variations in the line flux of about 10%. At outburst, accretion signatures appear in the profiles together with an enhancement of the wind, producing the correlation between accretion and outflow as reported from RU Lup, AA Tau and RW Aur observations.

Affiliated with

Also associated with

No associations

Rating

On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On the source of dense outflows from T Tauri Stars. and III. Winds driven from the star-disc shear layer will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-146621