Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-25T16:21:03.240Z Has data issue: false hasContentIssue false
  • English
  • Français

The period–luminosity relation of Mira variable stars

Published online by Cambridge University Press:  26 February 2013

Akiharu Nakagawa ,
Tomoharu Kurayama ,
Toshihiro Omodaka ,
Tatsuya Kamezaki ,
Yoshiro Nishida  and
Makoto Matsui
Akiharu Nakagawa
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan email: [email protected]
Tomoharu Kurayama
Affiliation:
Center for Fundamental Education, Teikyo University of Science, 2525 Yatsusawa, Uenohara, Yamanashi 409-0193, Japan
Toshihiro Omodaka
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan email: [email protected]
Tatsuya Kamezaki
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan email: [email protected]
Yoshiro Nishida
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan email: [email protected]
Makoto Matsui
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan 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.

We use astrometry to measure the distances to Galactic Mira variable stars. Our purpose is to determine a precise period–luminosity relation (PLR). At present, we do not have a precise PLR for Galactic Mira stars because of the large uncertainties affecting their distance estimates. To reduce the uncertainties, we adopted the Very Long Baseline Interferometry method and measured annual parallaxes of Mira variable stars with VERA. In addition to our previous results, we obtained three new distances for Mira variable stars. Based on our observations, the typical uncertainty in a given distance measurement is reduced to below 10%. At this conference, we present the current status of our project. To establish a precise Galactic PLR, we continue to observe more Mira variables. In addition, the apparent magnitudes of the target stars should be studied carefully.

Keywords

astrometrystars: AGB and post-AGBstars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 217
Copyright
Copyright © International Astronomical Union 2013