Hostname: page-component-848d4c4894-ndmmz Total loading time: 0 Render date: 2024-05-08T19:57:28.687Z Has data issue: false hasContentIssue false
  • English
  • Français

Are SiO molecules the seed of silicate dust around evolved stars?

Published online by Cambridge University Press:  12 October 2020

Biwei Jiang Open the ORCID record for Biwei Jiang [Opens in a new window]  and
Jiaming Liu
Biwei Jiang
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing 1000875, China email: bjiang@bnu.edu.cn
Jiaming Liu
Affiliation:
Department of Astronomy, Beijing Normal University, Beijing 1000875, China email: bjiang@bnu.edu.cn National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: jmliu@nao.ac.cn
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.

Silicate is the most popular dust species in the circumstellar envelope of evolved oxygen-rich stars, yet its seed particles have not been well identified. Among the candidates, corundum and SiO attract intense attention and study. SiO was suggested to be the seed particles in early 1980s and has received various supports as well as oppositions. In this work we investigate the relation of SiO maser and silicate dust emission powers. With both our own observation by using the PMO/Delingha 13.7-m telescope and the archival data, a sample is assembled of 21 SiO v=1, J=2-1 sources and 28 SiO v=1, J=1-0 sources that exhibit silicate emission features in the ISO/SWS spectrum. The analysis of their SiO maser and silicate emission power shows a moderate correlation, which agrees with the idea that SiO molecules are the seed nuclei of silicate dust.

Keywords

circumstellar matterdustmasersmass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 460 - 462
Copyright
© International Astronomical Union 2020

References

Bromley, S. T., Gómez Martn, J. C., & Plane, J. M. C. 2016, PCCP, 18, 26913 CrossRefGoogle Scholar
Bujarrabal, V. 1994, A&A, 285, 953 Google Scholar
Cho, S.-H., Chung, H.-S., Kim, H.-G., et al. 2009, ApJS, 181, 421 CrossRefGoogle Scholar
Cho, S.-H., & Kim, J. 2012, AJ, 144, 129 CrossRefGoogle Scholar
Gail, H.-P., & Sedlmayr, E. 1986, A&A, 166, 225 Google Scholar
Gail, H.-P., Wetzel, S., Pucci, A., & Tamanai, A. 2013, A&A, 555, A119 Google Scholar
Gail, H.-P., Scholz, M., & Pucci, A. 2016, A&A, 591, A17 Google Scholar
Gielen, C., et al. 2008, A&A, 490, 725 Google Scholar
Gobrecht, D., Decin, L., Cristallo, S., & Bromley, S. T. 2018, Chem. Phys. Lett., 711, 138 CrossRefGoogle Scholar
González Delgado, D., Olofsson, H., Kerschbaum, F., et al. 2003, A&A, 411, 123 Google Scholar
Jones, O. C., Kemper, F., Sargent, B. A., et al. 2012, MNRAS, 427, 3209 CrossRefGoogle Scholar
Kim, J., Cho, S.-H., Oh, C. S., & Byun, D.-Y. 2010, ApJS, 188, 209 CrossRefGoogle Scholar
Liu, J., Jiang, B. W., Li, A., & Gao, J. Liu, J., Jiang, B. W., Li, A., & Gao, J. 2017, MNRAS, 466, 1963 CrossRefGoogle Scholar
Liu, J., & Jiang, B. 2017, AJ, 153, 176 CrossRefGoogle Scholar
Nuth, J. A., & Donn, B. 1982, J. Chem. Phys., 77, 2639 CrossRefGoogle Scholar
Olofsson, J., Augereau, J.-C., van Dishoeck, E. F., et al. 2009, A&A, 507, 327 Google Scholar
Onaka, T., Yamamura, I., de Jong, T., et al. 1998, Astrophysics and Space Science, 255, 331 CrossRefGoogle Scholar