-
Views
-
Cite
Cite
Toshihisa Maeda, Hiroshi Imai, Toshihiro Omodaka, Hideyuki Kobayashi, Katsunori M. Shibata, Takeshi Bushimata, Yoon Kyung Choi, Tomoya Hirota, Mareki Honma, Koji Horiai, Noritomo Inomata, Kenzaburo Iwadate, Takaaki Jike, Seiji Kameno, Osamu Kameya, Ryuichi Kamohara, Yukitoshi Kan-ya, Noriyuki Kawaguchi, Seisuke Kuji, Tomoharu Kurayama, Seiji Manabe, Takeshi Miyaji, Takumi Nagayama, Akiharu Nakagawa, Kouichiro Nakashima, Chung Sik Oh, Tomoaki Oyama, Satoshi Sakai, Seiichiro Sakakibara, Katsuhisa Sato, Rie Shimizu, Motonobu Shintani, Kasumi Sora, Hiroshi Suda, Yoshiaki Tamura, Kazuyoshi Yamashita, A Bipolar Outflow of the M-Type Giant IRC −10414 Traced by HO Maser Emission, Publications of the Astronomical Society of Japan, Volume 60, Issue 5, 25 October 2008, Pages 1057–1067, https://doi.org/10.1093/pasj/60.5.1057
Close - Share Icon Share
Abstract
We report on results of five-epoch VLBI observations of H|$_{2}$|O maser emission in the M-type star IRC |$-$|10414, carried out with the VLBI Exploration of Radio Astrometry (VERA). The maser distribution extends over an area of 70mas|$\times$|260mas and exhibits a bipolar structure. The relative proper motions of 17 maser features were measured during the monitoring observations spanning nine months. The distance to IRC |$-$|10414 was re-estimated on the basis of the statistical treatment of parallax and the model-fitting method, yielding |$D=$| 3.1|$\pm$|0.4kpc and |$D=$| 2.0|$\pm$|0.2kpc, respectively. The estimated distance, |$D=$| 2-3kpc, is much larger than that previously adopted. The stellar luminosity of IRC |$-$|10414 is also re-estimated to be |$L_{\ast}\sim 9\times10^{4}$|(|$D/$|2kpc)|$^{2} L_{\odot}$|, much brighter by a factor of 10-20 than previously adopted (|$L_{\ast} \sim 10000L_{\odot}$|). The maser motions exhibit not only a spherically expanding flow with a velocity of |$\sim$| 10(|$D/$|2kpc)kms|$^{-1}$|, but also a faster bipolar outflow with a major axis in the north-south direction and at a small inclination angle with respect to the celestial sphere. These characteristics of the star and the circumstellar envelope seen in IRC |$-$|10414 are very similar to those in some supergiants exhibiting bipolar stellar mass loss.
