Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-28T21:03:42.445Z Has data issue: false hasContentIssue false
  • English
  • Français

Preliminary results on SiO maser emission from the AGB binary system: R Aqr.

Published online by Cambridge University Press:  07 February 2024

J.-F. Desmurs Open the ORCID record for J.-F. Desmurs [Opens in a new window] ,
J. Alcolea Open the ORCID record for J. Alcolea [Opens in a new window] ,
V. Bujarrabal ,
M. Santander Garcia Open the ORCID record for M. Santander Garcia [Opens in a new window] ,
M. Gomez-Garrido  and
J. Mikolajewska
J.-F. Desmurs*
Affiliation:
Observatorio Astronómico Nacional (OAN/IGN), Spain.
J. Alcolea
Affiliation:
Observatorio Astronómico Nacional (OAN/IGN), Spain.
V. Bujarrabal
Affiliation:
Observatorio Astronómico Nacional (OAN/IGN), Spain.
M. Santander Garcia
Affiliation:
Observatorio Astronómico Nacional (OAN/IGN), Spain.
M. Gomez-Garrido
Affiliation:
Observatorio Astronómico Nacional (OAN/IGN), Spain.
J. Mikolajewska
Affiliation:
Nicolaus Copernicus Astronomical Center of Polish Academy of Sciences
*
email: jf.desmurs@oan.es
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.

Binary/multiple stellar systems are as abundant as single stars. They are very interesting cosmic laboratories as they are related to many astrophysical phenomena. In the case of AGB (and post-AGB) stars, binaries are the most likely explanation for the shaping of non spherical PNe, a long standing problem in stellar evolution. While many binaries are known in the PNe phase, there are few examples in the previous AGB phase. Hydrodynamical models of the binary interaction are available, but well known parameters for orbits are non-existent. We observed the AGB binary system R Aqr at 7 mm using the Global VLBI array in wide-band continuum and SiO masers. The strong SiO masers were used to self-calibrate the observations and pinpoint the location of the AGB component. We used the continuum to try to directly detect the WD companion or its close environments (non-thermal emission from accretion disks/jets). We present our preliminary results for R Aqr on the relative positions of the J=1−0 SiO masers (v=1) with respect to the white dwarf position. This opens a new way to determine orbits in binaries at the AGB phase and better study their role in late stellar evolution and PNe shaping.

Keywords

AGBSiO masers
Type
Poster 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. 365 - 367
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Boboltz, D.A, Diamond, P.J and Kembal, A. J., A.J, 1997, ApJ 487, L147 CrossRefGoogle Scholar
Bujarrabal, V., Alcolea, J., Mikolajewska, J., et al. 2018, A&A, 616, L3.Google Scholar
Bujarrabal, V., Agúndez, M., Gómez-Garrido, M. et al. 2021, A&A, 651, A4 Google Scholar
Cheulhong Min, Naoko Matsumoto, Kyoung Kim, Mi, et al. 2014, PASP, 66, Issue 2, 38 Google Scholar
Gromadzki, M., Mikolajewska, J., 2009, A&A, 495, 931 Google Scholar
Schmid, H.M., Bazzon, A., Milli, J., et al. 2017, A&A, 602, A53. Google Scholar