演講資訊

摘要：

As the main-sequence objects, Be stars are unique in two ways: their rotating velocity approach a critical value in the equatorial region, and they have or have had line-emitting region surrounded. Because the surrounding disks are dissipated outward, the Be stars often show photometric, spectroscopic and polarimetric variability, known as Be phenomenon. This is why we keep our attention on Be stars with the high cadence strategy surveys, such as ZTF project. In the very beginning of ZTF survey, a Be star, HO Puppis, was observed with two highly unusual 2.5-magnitude dips within 30 days. Along with these significant dips in the light curve, HO Pup also shows usual semi-regular periodic variation. Here we report our results of periodic analysis, photometric and spectroscopic simultaneous followup with public surveys, CFHT/EsPADOnS and our Lulin Observatory.