JKAS - Journal of the Korean Astronomical Society

The Korean Astronomical Society

JKAS is a bimonthly publication of the Korean Astronomical Society. We aim at promoting the original work of researchers in all branches of astronomy and astrophysics. We cover all categories of work, including observation, theory, methodology, instrumentation, software, and data bases. We welcome proposals for review articles or special issues.

JKAS was launched in 1968 to provide a peer-reviewed scientific journal to the Korean community of astronomers. As there were only a few professional astronomers in Korea back then, JKAS initially published one issue per year, with each issue containing a handful of papers written either in Korean or English. The first-ever JKAS paper was written by Chou & Kitamura and discussed the photometric orbit of the eclipsing binary DI Pegasi. Over time, the Korean astronomy community grew, and so did the number of papers. In 1986, JKAS became English-only, with Korean language papers spun off to the Publications of the Korean Astronomical Society (PKAS). Around 2004/2005, the astronomical societies of Korea, Japan, China, and India discussed a merger of their national astronomy journals, including JKAS, into a unified Asian journal; eventually, this proposal was rejected In the past decade, efforts were made to make JKAS fit for the 21st century. In 2009, JKAS was added to the ISI/Thomson Reuters Science Citation Index Expanded database and received an impact factor, thus at last joining the family of globally recognized quality scientific journals. Nowadays, JKAS receives about 40 to 50 papers per year out of which 20 to 30 are accepted and published.

Journal of the Korean Astronomical Society - Vol. 53 , No. 2

53: 35 - 42, 2020 April





We analyze high dispersion emission lines of the symbiotic nova AG Pegasi, observed in 1998, 2001, and 2002. The H and H lines show three components, two narrow and one underlying broad line components, but most other lines, such as H I, He I, and He II lines, show two blue- and red-shifted components only. A recent study by Lee & Hyung (2018) suggested that the double Gaussian lines emitted from a bipolar conical shell are likely to form Raman scattering lines observed in 1998. In this study, we show that the bipolar cone with an opening angle of 74쨘 , which expands at a velocity of 70 km s닋1 along the polar axis of the white dwarf, can accommodate the observed double line profiles in 1998, 2001, and 2002. We conclude that the emission zone of the bipolar conical shell, which formed along the bipolar axis of the white dwarf due to the collimation by the accretion disk, is responsible for the double Gaussian profiles.

Key words: stars: binaries: symbiotic, stars: individual: AG Peg, ISM: dynamics and kinematics, ISM: lines and bands

Received 12 Dec 2019 Accepted 08 Feb 2020