Photometric activity of UX orionis stars and related objects in the near infrared and optical: CO Ori, RR Tau, UX Ori, and VV Ser
Photometric activity of UX orionis stars and related objects in the near infrared and optical: CO Ori, RR Tau, UX Ori, and VV Ser
复制标题
UX Orionis 恒星及相关天体在近红外和光学区域的光度活动：CO Ori、RR Tau、UX Ori 和 VV Ser
DOI：
--
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
S. P. Belan
中科院分区：
文献类型：
--
作者：
V. Shenavrin;A. N. Rostopchina;V. Grinin;T. Demidova;D. Shakhovskoi;S. P. Belan
本文继续了2000年开始的在光学和近红外（JHKLM波段）的UX Ori星光度活动的研究。作为比较，程序星列表包含两颗在光学上光度安静的Herbig Ae星：MWC 480和HD 179218。由于星周消光的零星增加，在光学（V波段）中的UXOri星的衰落也在红外（IR）中观察到，但幅度减小。两颗星，RR Tau和UX Ori，显示光度事件时，V -波段衰落伴随着红外通量的增加。在两颗Herbig Ae星中，MWC 480的红外光谱相当活跃，与UX Ori星不同，MWC 480的变化幅度从J波段到M波段逐渐增大。在观测过程中，没有探测到红外波段的深衰落。这表明程序星的食具有局部性质，并且是由于星周盘最内部区域的消光变化。结果证明了拱星盘相对于观测方向的排列在确定观测到的年轻恒星的红外变化中的重要作用。
This paper continues a study of the photometric activity of UX Ori stars in the optical and near-infrared (JHKLM bands) initiated in 2000. For comparison, the list of program stars contains two Herbig Ae stars that are photometrically quiet in the optical: MWC480 andHD179218. Fadings ofUXOri stars in the optical (V band) due to sporadic increases of the circumstellar extinction are also observed in the infrared (IR), but with decreasing amplitude. Two stars, RR Tau and UX Ori, displayed photometric events when V -band fadings were accompanied by an increase in IR fluxes. Among the two Herbig Ae stars that are photometrically quiet in the optical, MWC 480 proved to be fairly active in the IR. Unlike the UX Ori stars, the variation amplitude of MWC 480 increases from the J band to the M band. In the course of the observations, no deep fadings in the IR bands were detected. This indicates that eclipses of the program stars have a local nature, and are due to extinction variations in the innermost regions of the circumstellar disks. The results presented testify to an important role of the alignment of the circumstellar disks relative to the direction towards the observer in determining the observed IR variability of young stars.