Hostname: page-component-848d4c4894-75dct Total loading time: 0 Render date: 2024-05-01T06:03:41.285Z Has data issue: false hasContentIssue false
  • English
  • Français

Results of KVN Key Science Program for evolved stars

Published online by Cambridge University Press:  07 February 2024

Youngjoo Yun Open the ORCID record for Youngjoo Yun [Opens in a new window] ,
Se-Hyung Cho ,
Dong-Hwan Yoon ,
Haneul Yang ,
Richard Dodson Open the ORCID record for Richard Dodson [Opens in a new window] ,
María J. Rioja  and
Hiroshi Imai Open the ORCID record for Hiroshi Imai [Opens in a new window]
Youngjoo Yun*
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055, Republic of Korea.
Se-Hyung Cho
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055, Republic of Korea.
Dong-Hwan Yoon
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055, Republic of Korea.
Haneul Yang
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055, Republic of Korea.
Richard Dodson
Affiliation:
International Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Highway, Western Australia, Australia
María J. Rioja
Affiliation:
International Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Highway, Western Australia, Australia Observatorio Astronómico Nacional (IGN), Alfonso XII, 3 y 5, E-28014 Madrid, Spain
Hiroshi Imai
Affiliation:
Center for General Education, Institute for Comprehensive Education, Kagoshima University 1-21-30 Korimoto, Kagoshima 890-0065, Japan
*
email: yjyun@kasi.re.kr
Get access Rights & Permissions [Opens in a new window]

Abstract

We present the results of KVN Key Science Program (KSP) for evolved stars, which was launched in 2014. The first phase of KSP ended in June 2020 and the second phase started in October 2020. The goal of KSP is to study the physical characteristics of the evolved stars by observing the spatial distribution and temporal variability of the stellar masers at four frequency-bands (K, Q, W and D bands). The 22 GHz H2O maser is usually observed from the outer part of circumstellar envelopes compared to the 43, 86, 129 GHz SiO masers, thus the kinematic links between these regions can be studied by the multi-frequency simultaneous observations of KSP along the stellar pulsation cycles. This eventually enable us to study the enormous mass-loss rate of evolved stars, and the accumulated results from KSP are expected to shed light on the study of the late stage of the stellar evolution.

Keywords

masersradiative transfertechniques: interferometricstars: AGB and post-AGBstars: circumstellar matterstars: mass loss
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 324 - 327
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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

Boboltz, D. A., & Diamond, P. J. 2005, ApJ, 625, 978 10.1086/429656CrossRefGoogle Scholar
Decin, L., Richards, A. M. S., Millar, T. J., et al. 2016, A&A, 592, A76 Google Scholar
Deller, A. T., Tingay, S. J., Bailes, M., & West, C. 2007, PASP, 119, 318 10.1086/513572CrossRefGoogle Scholar
Dodson, R., Rioja, M. J., Jung, T.-H., et al. 2014, AJ, 148, 97 10.1088/0004-6256/148/5/97CrossRefGoogle Scholar
Hale, D. D. S., Bester, M., Danchi, W. C., et al. 1997, ApJ, 490, 407 10.1086/512794CrossRefGoogle Scholar
Höfner, S., & Olofsson, H. 2018, A&AR, 26, 1 Google Scholar
Khouri, T., de Koter, A., Decin, L., et al. 2014, A&A, 561, A5 Google Scholar
Khouri, T., Vlemmings, W. H. T., Paladini, C., et al. 2020, A&A, 635, A200 Google Scholar
Maercker, M., Schöier, F. L., Olofsson, H., Bergman, P., & Ramstedt, S. 2008, A&A, 479, 779 Google Scholar
Ohnaka, K., Weigelt, G., & Hofmann, K. H. 2016, A&A, 589, A9 Google Scholar
Richards, A. M. S., Impellizzeri, C. M. V., Humphreys, E. M., et al. 2014, A&A, 572, L9 Google Scholar
Richards, A. M. S., Sobolev, A., Baudry, A., et al. 2020, AdSpR, 65, 780 Google Scholar
van Leeuwen, F. 2007, A&A, 474, 653 Google Scholar
Zhang, B., Reid, M. J., Menten, K. M., & Zheng, X. W. 2012, ApJ, 744, 23 10.1088/0004-637X/744/1/23CrossRefGoogle Scholar