Search arXivSearch

arXiv · 0808.1151

VLBI Astrometry of AGB Variables with VERA -- A Semiregular Variable S Crateris --

Abstract

We present a distance measurement for the semiregular variable S Crateris (S Crt) based on its annual parallax. With the unique dual beam system of the VLBI Exploration for Radio Astrometry (VERA) telescopes, we measured the absolute proper motion of a water maser spot associated with S Crt, referred to the quasar J1147-0724 located at an angular separation of 1.23$^{\circ}$. In observations spanning nearly two years, we have detected the maser spot at the LSR velocity of 34.7 km s$^{-1}$, for which we measured the annual parallax of 2.33$\pm$0.13 mas corresponding to a distance of 430$^{+25}_{-23}$ pc. This measurement has an accuracy one order of magnitude better than the parallax measurements of HIPPARCOS. The angular distribution and three-dimensional velocity field of maser spots indicate a bipolar outflow with the flow axis along northeast-southwest direction. Using the distance and photospheric temperature, we estimate the stellar radius of S Crt and compare it with those of Mira variables.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Akiharu Nakagawa, Miyuki Tsushima, Kazuma Ando, Takeshi Bushimata, Yoon Kyung Choi, Tomoya Hirota, Mareki Honma, Hiroshi Imai, Kenzaburo Iwadate, Takaaki Jike, Seiji Kameno, Osamu Kameya, Ryuichi Kamohara, Yukitoshi Kan-Ya, Noriyuki Kawaguchi, Masachika Kijima, Mi Kyoung Kim, Hideyuki Kobayashi, Seisuke Kuji, Tomoharu Kurayama, Toshihisa Maeda, Seiji Manabe, Kenta Maruyama, Makoto Matsui, Naoko Matsumoto, Takeshi Miyaji, Takumi Nagayama, Kayoko Nakamura, Daisuke Nyu, Chung Sik Oh, Toshihiro Omodaka, Tomoaki Oyama, Nicolas Pradel, Satoshi Sakai, Tetsuo Sasao, Katsuhisa Sato, Mayumi Sato, Katsunori M. Shibata, Hiroshi Suda, Yoshiaki Tamura, Kousuke Ueda, Yuji Ueno, Kazuyoshi Yamashita. 2008-08-08. VLBI Astrometry of AGB Variables with VERA -- A Semiregular Variable S Crateris --. https://doi.org/10.1093/pasj%2F60.5.1013

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Cosmic Conundrums with Quantum Corrections

Darh energy was discovered over 25 years ago and we do not have an explanation of it. Dark matter comprises 95% of matter in the universe and we still don't know what it is. The Webb telescope has been finding fully formed galaxies with massive black holes millions of times the mass of the sun in the early universe and we don't have any explanation. A quantum density limitation will be used to solve these and other outstanding problems.

astro-ph

On binary pulsars and the force of gravity

The energy-momentum budget of the astrophysical systems can be studied by the exact local conservation equation derived by Landau and Lifshitz. We show that a similar equation is valid for the Einstein-Cartan gravity. We reanalyze a binary pulsar system using the Landau-Lifshitz conservation equation and show that the orbital period change rate can be completely understood as a curvature backreaction process. Taking into account the detailed theoretical and observational research of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude that general relativity and astrophysical observations rule out the existence of gravitational radiation. We comment upon the LIGO GW events and their alternative explanation, as well as the recent pulsar timing arrays data.

astro-ph

Oscillation frequencies and mode lifetimes in alpha Centauri A

We analyse our recently-published velocity measurements of alpha Cen A (Butler et al. 2004). After adjusting the weights on a night-by-night basis in order to optimize the window function to minimize sidelobes, we extract 42 oscillation frequencies with l=0 to 3 and measure the large and small frequency separations. We give fitted relations to these frequencies that can be compared with theoretical models and conclude that the observed scatter about these fits is due to the finite lifetimes of the oscillation modes. We estimate the mode lifetimes to be 1-2 d, substantially shorter than in the Sun.

astro-ph