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Modeling of Spectroscopic and Interferometric Observations of the Herbig Star VV Ser with Hybrid Models
Astronomy Reports ( IF 1 ) Pub Date : 2020-04-14 , DOI: 10.1134/s1063772920040058
L. V. Tambovtseva , A. Kreplin , V. P. Grinin , G. Weigelt

Abstract

Modeling of hydrogen emission lines is a powerful tool to study physical processes in the nearest vicinity of young stars because spectral lines carry information on the kinematics and physical conditions of the gas. One of the lines that probe emitting regions closest to the star is the Br\(\gamma \) line. We consider different types of hybrid models to reproduce both interferometric VLTI-AMBER observations and LBT-LUCIFER spectroscopic observations of the single-peak profile of the Br\(\gamma \) line of the Herbig AeBe star (HAEBE) VV Ser, a member of the UX Ori type subclass. We computed models of a magneto-centrifugal disk wind, a magnetospheric accretion region (magnetosphere), Cranmer’s polar wind, and scattered light from circumstellar polar dust. Furthermore, we calculated hybrid two-component models consisting of a disk wind and one of the aforementioned models. We computed visibilities and line profiles for all types of models and compared them with the available interferometric observations to constrain model parameters. We conclude that for the inclinations reported for this star (60°–70°), the disk wind alone cannot explain the Br\(\gamma \) line profile although it may be a dominant contributor to the hydrogen line radiation. However, magneto-centrifugal disk wind in combination with aforementioned emitting regions (magnetosphere, polar wind, or scattered light from polar dust) may be able to reproduce the observations.



中文翻译:

混合模型对Herbig Star VV Ser的光谱学和干涉测量观察建模

摘要

氢发射线的建模是研究年轻恒星附近的物理过程的有力工具,因为谱线会携带有关气体的运动学和物理条件的信息。探测最靠近恒星的发射区的线之一是Br \(\ gamma \)线。我们考虑不同类型的混合模型,以重现Br \(\ gamma \)单峰剖面的干涉式VLTI-AMBER观测和LBT-LUCIFER光谱观测UX Ori类型子类的成员Herbig AeBe星(HAEBE)VV Ser的行。我们计算了磁离心盘风,磁层吸积区(磁层),克兰默极风和星云极尘散射光的模型。此外,我们计算了由盘式风和上述模型之一组成的混合两分量模型。我们计算了所有类型的模型的可见性和线轮廓,并将它们与可用的干涉测量结果进行比较,以约束模型参数。我们得出结论,对于该恒星报告的倾角(60°–70°),仅盘风无法解释Br \(\ gamma \)线轮廓,尽管它可能是氢线辐射的主要贡献者。但是,磁离心盘风与上述发射区域(磁层,极风或来自极尘的散射光)结合可以重现观测结果。

更新日期:2020-04-23
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