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Simultaneous Visible and Near-Infrared Variability of Classical T Tauri Stars

Published online by Cambridge University Press:  06 January 2014

Yukako Aimi ,
Misato Fukagawa ,
Tomonori Yasuda ,
Takuya Yamashita ,
Kouji Kawabata ,
Makoto Uemura ,
Akira Arai ,
Mahito Sasada ,
Takashi Ohsugi  and
Michitoshi Yoshida
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Yukako Aimi
Affiliation:
Dept. of Earth and Space Science, Graduate School of Science, Osaka University, 1-1, Machikaneyama, Toyonaka, Osaka 560-0043, Japan email: aimi@iral.ess.sci.osaka-u.ac.jp
Misato Fukagawa
Affiliation:
Dept. of Earth and Space Science, Graduate School of Science, Osaka University, 1-1, Machikaneyama, Toyonaka, Osaka 560-0043, Japan email: aimi@iral.ess.sci.osaka-u.ac.jp
Tomonori Yasuda
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Takuya Yamashita
Affiliation:
National Astronomical Observatory of Japan 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan
Kouji Kawabata
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Makoto Uemura
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Akira Arai
Affiliation:
Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2, Nishigaichi, Sayo-cho, Sayo, Hyogo 679-5313, Japan
Mahito Sasada
Affiliation:
Dept. of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
Takashi Ohsugi
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Michitoshi Yoshida
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
Hiroshi Shibai
Affiliation:
Dept. of Earth and Space Science, Graduate School of Science, Osaka University, 1-1, Machikaneyama, Toyonaka, Osaka 560-0043, Japan email: aimi@iral.ess.sci.osaka-u.ac.jp
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Abstract

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Temporal structural changes of protoplanetary disks surrounding T Tauri stars (TTSs) can cause magnitude variations of TTSs. On the other hand, variability is also expected due to cool spots and/or hot spots on the surface of the star, thus it is important to distinguish the causes of the observed variability. Our sample consists of 23 TTSs (22 classical T Tauri stars, 1 weak-lined T Tauri star) and 4 Herbig Ae/Be stars. The observations were performed over a period of about 3 months in the V, J, and KS band, simultaneously. We detected variability for all stars in the three bands (>0.05 mag in V, >0.09 mag in J, >0.09 mag in KS). Color-magnitude relations obtained between V, J, and KS bands suggest that stellar spots are not the only cause of variability for most of our targets. In addition, the data implies that six stellar systems contain larger grains than in the interstellar medium if the variability is only caused by extinction due to circumstellar matter.

Keywords

stars: pre-main-sequence(stars:) planetary systems: protoplanetary disksstars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 149 - 150
Copyright
Copyright © International Astronomical Union 2013 

References

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