We present a detailed spectroscopic study of pre-main sequence star V565 Mon, which is the illuminating star of the Parsamian 17 cometary nebula. Observations were performed with the 2.6 m telescope in Byurakan Astrophysical Observatory on 2018 February 15. Radial velocities and equivalent widths of the most prominent lines of V565 Mon are presented. We build the spectral energy distribution and estimate the main parameters of the star, for example the obtained bolometric luminosity of V565 Mon is L _V565 ≈ 130 L _⊙. Considering all features of V565 Mon, we come to the conclusion that this young intermediate-mass star 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 involved in the problem of nucleosynthesis in young stars.

我们对前主序星 V565 Mon 进行了详细的光谱研究，它是 Parsamian 17 彗星星云的发光星。于 2018 年 2 月 15 日在 Byurakan 天体物理天文台使用 2.6 m 望远镜进行了观测。提供了 V565 Mon 最突出线的径向速度和等效宽度。我们建立光谱能量分布并估计恒星的主要参数，例如获得的 V565 Mon 的热光度为L _{V 565} ≈ 130 L _⊙ . 考虑到 V565 Mon 的所有特征，我们得出的结论是，这颗年轻的中等质量恒星属于 T Tau 和 HAeBe 星之间的中间类。对于年轻的恒星来说，非常不寻常的是在光谱中存在强吸收 Ba II 谱线。讨论了关于这个问题的可能解释。因此，我们认为 V565 Mon 是一个独特的例子，它可以帮助理解一些涉及年轻恒星核合成问题的开放性问题。