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.

8 pages, 4 figures

References in corpus (5)

• Enhanced production of barium in low-mass stars: evidence from open clusters
• New insights on Ba over-abundance in open clusters. Evidence for the intermediate neutron-capture process at play?
• Infrared Nebulae Around Young Stellar Objects
• Lithium in stellar atmospheres: observations and theory
• First determination of s-process element abundances in pre-main sequence clusters: Y, Zr, La, and Ce in IC 2391, the Argus association and IC 2602

Cited by in corpus (1)

• Photometric and Spectroscopic monitoring of YSOs in nearby star forming regions. I. Eruptive YSOs