Hostname: page-component-8448b6f56d-t5pn6 Total loading time: 0 Render date: 2024-04-18T04:43:36.664Z Has data issue: false hasContentIssue false
  • English
  • Français

A documentary of high-mass star formation: Probing the dynamical evolution of Orion Source I on 10–100 AU scales using SiO masers

Published online by Cambridge University Press:  01 March 2007

L. D. Matthews ,
C. Goddi ,
L. J. Greenhill ,
C. J. Chandler ,
M. J. Reid  and
E. M. L. Humphreys
L. D. Matthews
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
C. Goddi
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
L. J. Greenhill
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
C. J. Chandler
Affiliation:
National Radio Astronomy Observatory, Socorro, NM, USA
M. J. Reid
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
E. M. L. Humphreys
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A comprehensive picture of high-mass star formation has remained elusive, in part because examples of high-mass young stellar objects (YSOs) tend to be relatively distant, deeply embedded, and confused with other emission sources. These factors have impeded dynamical investigations within tens of AU of high-mass YSOs—scales that are critical for probing the interfaces where outflows from accretion disks are launched and collimated. Using observations of SiO masers obtained with the Very Large Array (VLA) and the Very Long Baseline Array (VLBA), the KaLYPSO project is overcoming these limitations by mapping the structure and dynamical/temporal evolution of the material 10-1000 AU from the nearest high-mass YSO: Radio Source I in the Orion BN/KL region. Our data include ~40 epochs of VLBA observations over a several-year period, allowing us to track the proper motions of individual SiO maser spots and to monitor changes in the physical conditions of the emitting material with time. Ultimately these data will provide 3-D maps of the outflow structure over approximately 30% of the outflow crossing time. Here we summarize recent results from the KaLYPSO project, including evidence that high-mass star formation occurs via disk-mediated accretion.

Keywords

masersstars: pre-main sequencetechniques: high angular resolutioncircumstellar matterstars: formationstars: windsoutflowsstars: individual (Source I)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 130 - 134
Copyright
Copyright © International Astronomical Union 2008

References

Beltrán, M. T., Cesaroni, R., Codella, C., Testi, L., Furuya, R. S., & Olmi, L. 2006, Nature, 443, 427CrossRefGoogle Scholar
Beuther, H., Kerp, J., Preibisch, T., Stanke, T., & Schilke, P. 2002, A&A, 395, 169Google Scholar
Bonnell, I. A. & Bate, M. R. 2005, MNRAS, 362CrossRefGoogle Scholar
Cesaroni, R. 2002, Highlights of Astronomy, Vol. 12, ed. Rickman, H., (ASP:San Francisco), p. 156Google Scholar
Cunningham, A., Frank, A., & Hartmann, L. 2005, ApJ, 631, 1010CrossRefGoogle Scholar
Doeleman, S. S., Lonsdale, C. J., & Pelkey, S. 1999, ApJ, 510, L55CrossRefGoogle Scholar
Greenhill, L. J., Gwinn, C. R., Schwartz, C., Moran, J. M., & Diamond, P. J. 1998, Nature, 396, 650CrossRefGoogle Scholar
Krumholz, M. R., McKee, C. F., & Klein, R. I. 2005, Nature, 438, 332CrossRefGoogle Scholar
McKee, C. F. & Tan, J. C. 2002, Nature, 416, 59CrossRefGoogle Scholar
Patel, N. A. et al. 2005, Nature, 437, 109Google Scholar
Reid, M. J., Menten, K. M., Greenhill, L. J., & Chandler, C. J. 2007, ApJ, submittedGoogle Scholar
Wright, M. C. H., Plambeck, R. L., Mundy, L. G., & Looney, L. W¿ 1995, ApJ, 455, L185CrossRefGoogle Scholar
Zhang, Q., Hunter, T. R., & Sridharan, T. K. 1998, ApJ, 505, L151CrossRefGoogle Scholar