Optical spectroscopic observations of a symbiotic star MWC 560 in the mass accumulation phase

Author:

Ando Kazuko1,Fukuda Naoya1,Sato Bunei2,Maehara Hiroyuki3ORCID,Izumiura Hideyuki3

Affiliation:

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

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

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

Abstract

Abstract There are about a dozen symbiotic stars known to produce high-velocity jets during outbursts. MWC 560 (V694 Mon) is a symbiotic star that seems to show a permanent jet. After showing an unexpected brightening in 2018 November, it has continued to brighten until 2021 and is currently in the brightest state ever. We have been conducting long-term high-dispersion spectroscopic monitoring of this object since 2016 March. An emission wing with vFWHM ≈ 700 km s−1 in the hydrogen Balmer line at an unexpected brightening event in 2018 was reported by Ando et al. (2021, PASJ, 73, L1). In subsequent continuous observations, this emission wing was no longer seen on 2019 February 6. The absorption lines seen in the hydrogen Balmer lines are gradually deepening and spreading to the slower side of the velocity, and the outflow velocity is becoming slower. The expanding component generated by the outburst was initially observed in the emission wing just after the 2018 outburst, got gradually cooler, and was observed in the absorption line after 2019.

Funder

NAOJ

Ministry of Education, Culture, Sports, Science and Technology

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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