论文标题
径向脉动恒星的微覆化
Microlensing of radially pulsating stars
论文作者
论文摘要
在这里，我们研究了径向脉动恒星的微透明。通过高振动微透镜观测值可以实现远处，微弱的脉动恒星的特性和表征。将恒星变异周期与微透镜相结合，可提供源距离，类型和半径，并有助于更好地确定镜头参数。考虑到其半径和表面温度的周期性变化，其微晶光曲线是由放大因子的繁殖而产生的，其有限尺寸效应通过脉冲源的固有亮度曲线而变化。由于脉动而引起的可变有限源大小对于过境和单微透镜以及苛性折射的特征可能很重要。当源半径与预计的镜头源距离的比率在[0.4,10] $中的$ρ_{\ star}/u \范围内时，这种放大因子的这种偏差很大，并且其持续时间很短，并且在交叉radius半径的时间相同。由于源强度及其面积而导致的其他偏差导致的有色和周期性偏差，这些偏差相对于脉动阶段的迹象是不对称的。正相使负相位的偏好更大。这些偏差在短波长（例如$ b-$ band）的过滤器中占主导地位。变化恒星微透明的放大峰位置各不相同，而该位移在不同的过滤器中有所不同。
Here, we study the microlensing of radially pulsating stars. Discerning and characterizing the properties of distant, faint pulsating stars is achievable through high-cadence microlensing observations. Combining stellar variability period with microlensing gives the source distance, type, and radius and helps better determine the lens parameters. Considering periodically variations in their radius and surface temperature, their microlensing light curves are resulted from multiplication of the magnification factor with variable finite size effect by the intrinsic brightness curves of pulsing source. The variable finite source size due to pulsation can be significant for transit and single microlensing and while caustic-crossing features. This kind of deviation in the magnification factor is considerable when the ratio of the source radius to the projected lens-source distance is in the range of $ρ_{\star}/u \in[0.4,10]$ and its duration is short and in the same order of the time of crossing the source radius. Other deviations due to variable source intensity and its area make colored and periodic deviations which are asymmetric with respect to the signs of pulsation phase. The positive phases makes deviations with larger amplitude that negative phase. These deviations dominate in filters with short wave lengths (e.g., $B-$band). The position of magnification peaks in microlensing of variable stars varies and this displacement differs in different filters.
