Hostname: page-component-745bb68f8f-5r2nc Total loading time: 0 Render date: 2025-02-11T20:05:41.385Z Has data issue: false hasContentIssue false
  • English
  • Français

Energetic processes revealed by spectrally resolved high-J COlines in low-mass star-forming regions with Herschel-HIFI

Published online by Cambridge University Press:  25 November 2011

M. Röllig ,
R. Simon ,
V. Ossenkopf ,
J. Stutzki ,
U.A. Yıldız ,
E.F. van Dishoeck ,
L.E. Kristensen ,
R. Visser ,
G. Herczeg  and
T.A. van Kempen
...Show all authors
U.A. Yıldız
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ;
E.F. van Dishoeck
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ; Max-Planck-Institut für Extraterrestrische Physik, 85748 Garching, Germany
L.E. Kristensen
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ;
R. Visser
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ;
G. Herczeg
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, 85748 Garching, Germany
T.A. van Kempen
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ;
J.K. Jørgensen
Affiliation:
Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen K., Denmark
M.R. Hogerheijde
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. e-mail: [email protected] ;
Get access

Abstract

Herschel-HIFI observations of high-J lines (up toJu = 10) of 12CO, 13CO andC18O are presented toward three deeply embedded low-mass protostars in NGC1333. The observations show several energetic components including shocked and quiescentgas. Radiative transfer models are used to quantify the C18O envelope abundancewhich require a jump in the abundance at an evaporation temperature,Tev ~ 25 K, providing new direct evidence of a COice evaporation zone around protostars. The abundance in the outermost part of theenvelope, X0, is within the canonical value of2 × 10-4; however the inner abundance, Xin, isfound around a factor of 3–5 lower than X0.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 52: Conditions and Impact of Star Formation , 2011 , pp. 313 - 314
Copyright
© EAS, EDP Sciences 2011

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Jørgensen, J.K., Schöier, F.L., & van Dishoeck, E.F., 2005, A&A, 435, 177
Kristensen, L.E., et al., 2010, A&A, 521, L30
van Dishoeck, E.F., et al., 2011, PASP, accepted [astro-ph: 1012.4570]
Yıldız, U.A., et al., 2010, A&A, 521, L40