Optical spectroscopic monitoring of the symbiotic star MWC 560 before and after the 2018 unpredicted brightening

Author:

Ando Kazuko1,Fukuda Naoya1,Akazawa Hidehiko2,Sato Bunei3,Hasegawa Ryo3,Koizumi Yohei3,Omiya Masashi4,Harakawa Hiroki5,Kambe Eiji5,Maehara Hiroyuki6ORCID,Izumiura Hideyuki6

Affiliation:

1. Okayama University of Science, 1-1 Ridai-cyo, Kita-ku, Okayama 700-0005, Japan

2. Funao Astronomical Observatory, 107 Funao, Okayama 710-0261, Japan

3. Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan

4. Astrobiology Center / National Astronomical Observatory of Japan, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

5. Subaru Telescope, National Astronomical Observatory of Japan, NINS, 650 North A’ohoku Place, Hilo, HI 96720, USA

6. Subaru Telescope Okayama Branch, National Astronomical Observatory of Japan, NINS, 3037-5 Honjou, Kamogata, Asakuchi, Okayama 719-0232, Japan

Abstract

Abstract MWC 560 (V694 Mon) is classified as a symbiotic binary consisting of a white dwarf and an M5III red giant. In this object, a very- high-speed component, thought to be a jet, has been reported in the hydrogen Balmer line. We have been conducting long-term spectroscopic monitoring since the brightening in 2016 February. An irregular rebrightening was reported by Goranskij et al. (2018, Astronomer’s Telegram, 12227), who also showed that the high-velocity absorption component was not seen on 2018 November 16. Our low-resolution spectroscopic observations showed no high-velocity absorption component on 2018 November 14, and wide emission lines in Balmer line region (Hα, Hβ). However, high-resolution spectroscopy revealed the presence of slow, weak absorbing components and an emission wing on 2018 December 25. MWC 560 began to brighten in 2018 November, and it is gradually brightening as of 2020 April 14. For the absorption component, we propose a shell expansion of a classical symbiotic nova that occurred in 2016. During the 2018 brightening a new emission wing with vFWHM ≈ 700 km s−1 was confirmed, which could be triggered by disk instability like a dwarf nova. This paper summarizes the results of long-term monitoring observations and the recent changes in MWC 560.

Funder

Ministry of Education, Science, Culture, and Sport

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 1 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Optical spectroscopic observations of a symbiotic star MWC 560 in the mass accumulation phase;Publications of the Astronomical Society of Japan;2021-11-13

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