Eclipse of the V773 Tau B circumbinary disc
Eclipse of the V773 Tau B circumbinary disc
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V773 Tau B 环二进制光盘的 Eclipse
DOI：
10.1051/0004-6361/202243441
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发表时间：
2022
期刊：
影响因子：
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通讯作者：
R. Oelkers
中科院分区：
文献类型：
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作者：
M. Kenworthy;D. G. Picos;E. Elizondo;R. Martin;D. M. V. Dam;J. Rodriguez;G. Kennedy;C. Ginski;M. Mugrauer;N. Vogt;C. Adam;R. Oelkers
上下文。年轻的多恒星系统既可以容纳由气体和尘埃组成的星周双星盘，也可以容纳由气体和尘埃组成的外星双星盘，外双星盘的方向可以由中心双星的取向和偏心率来塑造。研究多个双星系统及其相关的圆盘使我们能够理解随后在它们周围形成的行星系统的大小和分布。目标。2010年，年轻的多恒星系统V773Tau发生了一次深度(∼70%)和延长(∼150天)的日食。我们将其解释为，这是由于绕着B分量移动到A分量前面的外接二进制盘的结果。我们的目标是描述圆盘的方向和结构，重新确定子分量的轨道，并预测下一次日食发生的时间。方法：研究方法。我们结合了几次地面测量的光度学数据，建立了日食的光曲线模型，并使用高角度分辨率成像来重新确定系统的三个空间分辨分量：A、B和C的轨道。对光曲线的频率分析，包括来自TESS卫星的光曲线，使得能够表征AA星和AA星的自转周期。结果。外接双星圆盘的玩具模型表明，它围绕B双星延伸到大约5AU，相对于AB轨道平面的倾角为73◦，其中圆盘半径的下界由AB轨道的几何形状限制，上界由圆盘的稳定性决定。我们在光度学数据中确定了几个频率，我们将其归因于Aa和Ab恒星伴星的旋转调制。我们给出了较远的C分量围绕AB系统的轨道的fi第一次测定，并将其倾角限制在93◦。结论。圆盘的大倾角和大直径，以及理论上预期的圆盘倾斜度，表明B是一个几乎等质量、中等偏心的双星。我们确定了AA星和AB星的自转周期，以及光曲线上的第三个频率，我们将其归因于B双星中恒星的轨道周期。我们预测下一次日食将发生在2037年左右，在此期间，详细的光度和光谱监测将更详细地描述该圆盘的特征。
Context. Young multiple stellar systems can host both circumstellar and circumbinary discs composed of gas and dust, and the ori- entations of circumbinary discs can be sculpted by the orientation and eccentricity of the central binaries. Studying multiple binary systems and their associated discs enables our understanding of the size and distribution of the planetary systems that subsequently form around them. Aims. A deep ( ∼ 70%) and extended ( ∼ 150 days) eclipse was seen towards the young multiple stellar system V773 Tau in 2010. We interpret it as being due to the passage of a circumbinary disc around the B components moving in front of the A components. Our aim is to characterise the orientation and structure of the disc, to refine the orbits of the sub-components, and to predict when the next eclipse will occur. Methods. We combined the photometry from several ground-based surveys, constructed a model for the light curve of the eclipse, and used high angular resolution imaging to refine the orbits of the three spatially resolved components of the system: A, B, and C. A frequency analysis of the light curves, including from the TESS satellite, enabled the characterisation of the rotational periods of the Aa and Ab stars. Results. A toy model of the circumbinary disc shows that it extends out to approximately 5au around the B binary and has an incli- nation of 73 ◦ with respect to the orbital plane of AB, where the lower bound of the radius of the disc is constrained by the geometry of the AB orbit and the upper bound is set by the stability of the disc. We identify several frequencies in the photometric data that we attribute to rotational modulation of the Aa and Ab stellar companions. We produced the first determination of the orbit of the more distant C component around the AB system and limited its inclination to 93 ◦ . Conclusions. The high inclination and large diameter of the disc, together with the expected inclination of the disc from theory, sug- gest that B is an almost equal-mass, moderately eccentric binary. We identify the rotational periods of the Aa and Ab stars and a third frequency in the light curve that we attribute to the orbital period of the stars in the B binary. We predict that the next eclipse will occur around 2037, during which both detailed photometric and spectroscopic monitoring will characterise the disc in greater detail.