H2 Velocity Structure in HH 211

Details H2 Velocity Structure in HH 211 H2 Velocity Structure in HH 211

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxaa..39...77s&link_type=abstract

Revista Mexicana de Astronomía y Astrofísica Vol. 39, pp. 77-88 (2003) (http://www.astroscu.unam.mx/~rmaa/)

Astronomy and Astrophysics

Astronomy

3

Ism: Individual (Hh 211), Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Ism: Molecules, Stars: Formation

Scientific paper

We describe the velocity structure of the molecular outflow HH 211 in the 2.12 μ m line of H2. Observations were obtained using an IR Fabry-Pérot interferometer with a spectral resolution of 24 km s-1. It is observed that the eastern lobe of the outflow is blue-shifted while the western side is red-shifted. Most of the emission originates at low velocities, in agreement with the flux-velocity relation of Salas & Cruz-González (2002), but these velocities are in general higher than the low velocities observed in CO . There is also evidence of the high velocities that trace the molecular jet, in both CO and SiO, and these high velocities in H2 occur closer to the central axis of the outflow. These arguments lead us to the conclusion that H2 coexists with CO in the molecular outflow, as opposed to the view that H2 emission arises in the shocked quiescent medium. The jet and X-wind driven outflow dynamical models are tested to fit the observed morphology and kinematics of H2.

Affiliated with

Also associated with

No associations

Rating

H2 Velocity Structure in HH 211 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 H2 Velocity Structure in HH 211, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and H2 Velocity Structure in HH 211 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1326090