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Monitoring of dynamical processes in outer atmospheres of cool protoplanetary nebulae

Published online by Cambridge University Press:  06 October 2025

Kārlis Puķītis Open the ORCID record for Kārlis Puķītis [Opens in a new window] ,
Laimons Začs ,
Julius Sperauskas  and
Aija Grankina
Kārlis Puķītis*
Affiliation:
Laser Center, Faculty of Physics, Mathematics, and Optometry, University of Latvia, Raiņa bulvāris 19, LV-1586 Rīga, Latvia
Laimons Začs
Affiliation:
Laser Center, Faculty of Physics, Mathematics, and Optometry, University of Latvia, Raiņa bulvāris 19, LV-1586 Rīga, Latvia
Julius Sperauskas
Affiliation:
Vilnius University Observatory, Saulėtekio al. 3, 10257 Vilnius, Lithuania
Aija Grankina
Affiliation:
Laser Center, Faculty of Physics, Mathematics, and Optometry, University of Latvia, Raiņa bulvāris 19, LV-1586 Rīga, Latvia
*
email: karlis.pukitis@lu.lv
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Abstract

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Dynamics in the atmospheres of central stars of cool protoplanetary nebulae can contribute to shaping of the subsequent planetary nebulae by giving rise to stellar wind. We have investigated variation in high-resolution spectra of three relatively cool post-asymptotic giant branch stars that are surrounded by non-spherical nebulae. Spectra of HD 161796 show variability in blue wings of weak and medium strength absorption lines while red wings remain unchanged. This could be caused by warm variable outflow. An episode of infall of matter is revealed in spectra of IRAS 22272+5435. Also, episodes of molecular lines in emission are detected for this star. The emissions appear to be related to the star’s brightness changes. Qualitatively the same molecular line variability is observed in the spectrum of IRAS Z02229+6208. Possibly, the observed spectral variations are a consequence of similar dynamics as in the atmospheres of asymptotic giant branch stars.

Keywords

stars: AGB and post-AGBstars: atmospheresstars: windsoutflowsstars: individual (HD 161796, IRAS 22272+5435, IRAS Z02229+6208)

Information

Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S384: Planetary Nebulae: A Universal Toolbox in the Era of Precision Astrophysics , December 2023 , pp. 315 - 319
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2025. Published by Cambridge University Press on behalf of International Astronomical Union

References

Hrivnak, B. J., Van de Steene, G., Van Winckel, H., et al. 2017, ApJ, 846, 96. doi: 10.3847/1538-4357/aa84ae CrossRefGoogle Scholar
Parthasarathy, M. 2022, RNAAS, 6, 33. doi: 10.3847/2515-5172/ac54bb CrossRefGoogle Scholar
Sánchez Contreras, C., Sahai, R., Gil de Paz, A., et al. 2008, ApJS, 179, 166. doi: 10.1086/591273 CrossRefGoogle Scholar
Začs, L., Musaev, F., Kaminsky, B., et al. 2016, ApJ, 816, 3. doi: 10.3847/0004-637X/816/1/3 CrossRefGoogle Scholar
Hrivnak, B. J., Lu, W., Bakke, W. C., et al. 2022, ApJ, 939, 32. doi: 10.3847/1538-4357/ac938a CrossRefGoogle Scholar
Höfner, S. & Olofsson, H. 2018, A&ARv, 26, 1. doi: 10.1007/s00159-017-0106-5 Google Scholar
Krtička, J., Kubát, J., & Krtičková, I. 2020, A&A, 635, A173. doi: 10.1051/0004-6361/201937150 CrossRefGoogle Scholar
Gezer, I., Van Winckel, H., Bozkurt, Z., et al. 2015, MNRAS, 453, 133. doi: 10.1093/mnras/stv1627 CrossRefGoogle Scholar
Schönberner, D. & Steffen, M. 2007, Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes, 378, 343 Google Scholar
Miller Bertolami, M. M. 2016, A&A, 588, A25. doi: 10.1051/0004-6361/201526577 CrossRefGoogle Scholar
Začs, L. & Puķītis, K. 2021, ApJ, 920, 17. doi: 10.3847/1538-4357/ac1671 CrossRefGoogle Scholar
Puķītis, K., Začs, L., & Grankina, A. 2022, ApJ, 928, 29. doi: 10.3847/1538-4357/ac4bc8 CrossRefGoogle Scholar
Puķītis, K., Začs, L., & Sperauskas, J. 2023, ApJ, 948, 70. doi: 10.3847/1538-4357/acc52b CrossRefGoogle Scholar
Začs, L. & Puķītis, K. 2023, ApJ, 952, 49. doi: 10.3847/1538-4357/acdcfe CrossRefGoogle Scholar
Ueta, T., Meixner, M., & Bobrowsky, M. 2000, ApJ, 528, 861. doi: 10.1086/308208 CrossRefGoogle Scholar
Takeda, Y., Taguchi, H., Yoshioka, K., et al. 2007, PASJ, 59, 1127. doi: 10.1093/pasj/59.6.1127 CrossRefGoogle Scholar
Hrivnak, B. J., Lu, W., & Nault, K. A. 2015, AJ, 149, 184. doi: 10.1088/0004-6256/149/6/184 CrossRefGoogle Scholar
Reddy, B. E., Bakker, E. J., & Hrivnak, B. J. 1999, ApJ, 524, 831. doi: 10.1086/307858 CrossRefGoogle Scholar