论文标题
棉花恒星V646幼犬中的光盘灯变异性如苔丝和地面观察到
Disc light variability in the FUor star V646 Puppis as observed by TESS and from the ground
论文作者
论文摘要
我们研究了发生在不同时间尺度上的V646幼崽中的小尺度光变化，目的是研究这种变异性是否与Fu Ori中观察到的变异性相似。我们在2013年至2018年之间在SAAO和CTIO上观察到了Johnson和Sloan Filters的V646 PUP，通常使用维持一日节奏1-4周。我们还使用30分钟的节奏在2019年获得了2019年获得的1512天的公共域1512天的ASAS-SN光曲线和苔丝光度法。新的SAAO低分辨率光谱有助于更新主要的圆盘参数，而档案高分辨率Keck Spectra则用于搜索光盘旋转配置文件中的时间变化。基于地面的观察结果证实，以0.018 mag/yr的速度，V646幼崽的亮度不断降低。精确的苔丝数据表明，在这种一般趋势上施加的轻微的0.005-0.01 mag，光的光变化确实由几个明显时间交联的独立波列。假设这是典型的情况，基于对早期时代获得的颜色魔力图的分析，我们能够先推断出观察到的大部分光变化可能是由于圆盘光谱液的旋转造成的，这是由于旋转的旋转，这是在10-12 solar Radii之间引起的。我们不排除这些不均匀性也可以在盘的旋转曲线中表现出来的可能性，从高分辨率光谱中获得。假设这些不均匀性的开普勒旋转，我们对恒星质量的初步确定为0.7-0.9太阳能质量。这些初步结果与Fu Ori更好地建立的结果相似，这表明了共同的驾驶机制。
We investigate small-scale light variations in V646 Pup occurring on different timescales with the aim to investigate whether this variability is similar to that observed in FU Ori. We observed V646 Pup at the SAAO and CTIO between 2013 and 2018 with Johnson and Sloan filters, typically using a one-day cadence maintained for 1-4 weeks. We also utilised the public-domain 1512-day-long ASAS-SN light curve and TESS photometry obtained in 2019 over 24.1 days with a 30 min cadence. New SAAO low-resolution spectra assist in updating major disc parameters, while the archival high-resolution Keck spectra are used to search for temporal changes in the disc rotational profiles. The ground-based observations confirm the constantly decreasing brightness of V646 Pup at the rate of 0.018 mag/yr. Precise TESS data show that the slight, 0.005-0.01 mag, light variations imposed on this general trend do consist of a few independent wave trains of an apparently time-coherent nature. Assuming that this is typical situation, based on an analysis of colour-magnitude diagrams obtained for earlier epochs, we were able to make a preliminarily inference that the bulk of the light changes observed could be due to the rotation of disc photosphere inhomogeneities, arising between 10-12 solar radii from the star. We do not exclude the possibility that these inhomogeneities could also manifest themselves in the rotational profiles of the disc, as obtained from the high-resolution spectra. Assuming Keplerian rotation of these inhomogeneities, we give a preliminary determination of the stellar mass at 0.7-0.9 solar mass. These preliminary results are similar to those better established for FU Ori, which suggests a common driving mechanism(s).
