• Published 2005

A Parsec Scale “ Superjet ” and Quasi-Periodic Structure in the HH 34 Outflow ?

@inproceedings{Rodriguez2005APS,
  title={A Parsec Scale “ Superjet ” and Quasi-Periodic Structure in the HH 34 Outflow ?},
  author={Luis Rodriguez and J. Cant{\'o} and Jose Maria Torrelles and Jose F G{\'o}mez and Guillem Anglada and Paul T.-P. Ho and Goeran Sandell and Lewis B. G. Knee and Colin A. Aspin and Ian E. Robson and A. G. Russell and Kris Sellgren and R. G. Smith and Timothy Young Brooke},
  year={2005}
}
s of recently accepted papers A Parsec Scale “Superjet” and Quasi-Periodic Structure in the HH 34 Outflow? John Bally and David Devine 1 Department of Astrophysical, Planetary, and Atmospheric Sciences and Center for Astrophysics and Space Astronomy Campus Box 389, University of Colorado, Boulder, CO 80309, USA bally@janos.colorado.edu We report the detection of a new Herbig-Haro (HH) object, HH 173, near the young stellar object HH 34∗ in the L1641 molecular cloud in Orion. The new object… CONTINUE READING

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Thesis work conducted at: Landessternwarte, Königstuhl D–69117 Heidelberg, Germany Current address: Landessternwarte Königstuhl, D–69117 Heidelberg, Germany Electronic mail: bo7@vm.urz.uni-heidelberg

  • Thesis work conducted at: Landessternwarte, Königstuhl D–69117 Heidelberg, Germany Current address: Landessternwarte Königstuhl, D–69117 Heidelberg, Germany Electronic mail: bo7@vm.urz.uni-heidelberg
  • 1994

Chile 3 Onsala Space Observatory, S-43992 Onsala, Sweden 4 Royal Observatory

  • Astronomy Joint, Centre, +5 authors Telescope
  • Chile 3 Onsala Space Observatory, S-43992 Onsala, Sweden 4 Royal Observatory
  • 1900

A correlation between the bolometric luminosity and the X–ray luminosity of the new WTTS was found. This may indicate that a mass–X–ray luminosity relation exists for low–mass PMS stars

  • A correlation between the bolometric luminosity and the X–ray luminosity of the new WTTS was found. This may indicate that a mass–X–ray luminosity relation exists for low–mass PMS stars

However, a larger ratio (up to 7) can not yet be ruled out. This ratio will be derived for the Orion complex when sufficient spectroscopic observations are complete

  • However, a larger ratio (up to 7) can not yet be ruled out. This ratio will be derived for the Orion complex when sufficient spectroscopic observations are complete

X-ray and Optical Studies of Low–Mass Star Formation

  • X-ray and Optical Studies of Low–Mass Star Formation