Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-22T09:53:09.389Z Has data issue: false hasContentIssue false
  • English
  • Français

OH/IR stars and the Period-Luminosity Relation of Mira variables

Published online by Cambridge University Press:  06 February 2024

D. Engels Open the ORCID record for D. Engels [Opens in a new window] ,
S. Etoka Open the ORCID record for S. Etoka [Opens in a new window] ,
F. Jiménez-Esteban ,
W. Herrmann  and
B. López-Martí
D. Engels*
Affiliation:
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
S. Etoka
Affiliation:
JBCA, University of Manchester, M13 9PL, Manchester, UK
F. Jiménez-Esteban
Affiliation:
Centro de Astrobiologa (CAB), CSIC-INTA, Camino Bajo del Castillo s/n, 28692, Villanueva de la Cañada, Madrid, Spain
W. Herrmann
Affiliation:
Astropeiler Stockert e.V., Astropeiler Stockert 1-4, 53902 Bad Münstereifel, Germany
B. López-Martí
Affiliation:
Universidad San Pablo-CEU, Campus de Monteprncipe, 28668 Boadilla del Monte, Madrid, Spain
*
email: [email protected]
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.

The OH/IR stars evolving on the Asymptotic Giant Branch are large-amplitude variable stars with periods in the range of ~400 to 2500 days, significantly longer than those of the related Mira variables. We use preliminary results from a monitoring program of the 1612-MHz OH maser variations of a sample of > 70 OH/IR stars to study a possible extension of Mira Period-Luminosity Relations to longer periods. The period distribution of the sample is split around P ~ 1100 days. Using WISE W3 absolute magnitudes as proxies for the luminosity and the best available distances, we found no convincing relation between periods and absolute magnitudes. A cause could be rapid evolution of the ‘extreme OH/IR stars’ (the group with P >1100 days) close to the tip of the AGB, where no increase of luminosity is expected on the short time-scales involved.

Keywords

masersstars: AGB and post-AGBcircumstellar matter
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S376: At the crossroads of astrophysics and cosmology: Period–luminosity relations in the 2020s , December 2022 , pp. 328 - 333
Check for updates
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 (http://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), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., Demleitner, M., Andrae, R., 2021, AJ, 161, 147 CrossRefGoogle Scholar
Baud, B., Habing, H. J., Matthews, H. E., Winnberg, A., 1981, A&A, 95, 156 Google Scholar
De Beck, E., Decin, L., de Koter, A. et al., 2010, A&A, 523, A18 Google Scholar
Engels, D., Kreysa, E., Schultz, G. V., Sherwood, W. A., 1983, A&A, 124, 123 Google Scholar
Engels, D. & Jiménez-Esteban, F., 2007, A&A, 475, 941 Google Scholar
Engels, D., Etoka, S., Gérard, E., Richards, A., 2015, in Kerschbaum, F., Wing R. F. & J. Hron J., eds., Why Galaxies Care about AGB Stars III: A Closer Look in Space and Time, ASP-CS, 497, 473Google Scholar
Etoka, S. & Engels, D., 2022, European VLBI Network Mini-Symposium and Users’ Meeting 2021, 12–14 July, 2021. Online at https://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=399, id.12Google Scholar
Etoka, S., Engels, D., Ullrich, T., González, J. B., López-Martí, B., 2023, in Hirota, T., Imai, H., Menten, K. & Pihlstrom, Y., eds., Cosmic Masers: Proper Motion toward the Next-Generation Large Projects, Proceedings of the IAU Symposium 380, in pressGoogle Scholar
Goldman, S. R., Th, van Loon J. ., Zijlstra A. A. et al., 2017, MNRAS, 465, 403Google Scholar
Herman, J. & Habing, H. J., 1985, A&AS, 59, 523 Google Scholar
Iwanek, P., Soszyński, I., Kozłowski S., 2021, ApJ, 919, 99Google Scholar
Jiménez-Esteban, F. M., Engels, D., Aguado, D. S., González, J. B., García-Lario, P., 2021, MNRAS, 506, 6051 Google Scholar
Jones, T. J., Hyland, A. R., Wood, P. R., Gatley, I., 1983, ApJ, 273, 669 Google Scholar
Marini, E., Dell’Agli, F., Kamath, D. et al., 2023, A&A, 670, A97 Google Scholar
Miller Bertolami, M. M., 2016, A&A, 588, A25 Google Scholar
Nakagawa, A., Kurayama, T., Matsui, M. et al., 2016, PASJ, 68, 78 Google Scholar
Nakagawa, A., 2023, these proceedingsGoogle Scholar
Orosz, G., Imai, H., Dodson, R. et al., 2017, AJ, 153, 119 Google Scholar
Reid, M. J., Menten, K. M., Brunthaler, A. et al., 2019, ApJ, 885, 131 Google Scholar
Trabucchi, M., Wood, P. R., Mowlavi, N. et al., 2021, MNRAS, 500, 1575 Google Scholar
van Langevelde, H.J., van der Heiden, R., van Schooneveld, C., 1990, A&A, 239, 193 Google Scholar
Whitelock, P., Feast, M., Catchpole, R., 1991, MNRAS, 248, 276 Google Scholar
Wilson, W. J., Barrett, A. H., 1970, A&A, 17, 385 Google Scholar
Wolak, P., Szymczak, M., Gérard, E., 2013, MNRAS, 430, 2499 Google Scholar