Spectral study of V565 Mon: Probable FU Ori-like or chemically peculiar star

Abstract

We present the detailed spectroscopic study of V565 Mon pre-main-sequence star, which is the illuminating star of Parsamian 17 cometary nebula. Observations were performed with 2.6 m telescope in Byurakan Astrophysical Observatory in 15 February 2018. Radial velocities and equivalent widths of the most prominent lines of V565 Mon are presented. We built the spectral energy distribution and estimated the main parameters of the star, for example obtained bolometric luminosity of V565 Mon is $L_{V565}\approx 130L_{\odot }$ . Considering all features of V565 Mon we came to conclusion that this young intermediate-mass star can belongs to some intermediate class between T Tau and HAeBe stars. Very unusual for a young star is the presence of strong absorption Ba II lines in the spectrum. Possible explanations on this issue are discussed. Hence, we think that V565 Mon is a unique example, which can help to understand some open questions in nucleosynthesis problem in young stars.

arXiv comment8 pages, 4 figures

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