Searching for Planets with White Dwarf Pulsations: Spurious Detections

β Pictoris b 希尔球凌星观测计划。论文 II：通过 δ Scuti 脉动的时间延迟分析搜寻 β Pictoris 系外行星的信号

The $β$ Pictoris b Hill sphere transit campaign. Paper II: Searching for the signatures of the $β$ Pictoris exoplanets through time delay analysis of the $δ$ Scuti pulsations

本文通过多年测光数据与 maelstrom 分析 β Pictoris 的 δ Scuti 脉动时间延迟，试图间接探测其行星 b 和 c，但未探测到预期信号，并发现脉动模式本身年际漂移从根本上限制了该方法。

EXOTIME: searching for planets and measuring Pdot in sdB pulsators

We review the status of the EXOTIME project (EXOplanet search with the TIming MEthod). The two main goals of EXOTIME are to search for sub-stellar companions to sdB stars in wide orbits, and to measure the secular variation of the pulsation periods, which are related to the evolutionary change of the stellar structure. Now, after four years of dense monitoring, we start to see some results and present the brown dwarf and exoplanet candidates V1636 Ori b and DW Lyn b.

EXOTIME: searching for planets around pulsating subdwarf B stars

In 2007, a companion with planetary mass was found around the pulsating subdwarf B star V391 Pegasi with the timing method, indicating that a previously undiscovered population of substellar companions to apparently single subdwarf B stars might exist. Following this serendipitous discovery, the EXOTIME (http://www.na.astro.it/~silvotti/exotime/) monitoring program has been set up to follow the pulsations of a number of selected rapidly pulsating subdwarf B stars on time-scales of several years with two immediate observational goals: 1) determine Pdot of the pulsational periods P 2) search for…

Spectroscopic Transit Search: a self-calibrating method for detecting planets around bright stars

We search for transiting exoplanets around the star $β$ Pictoris using high resolution spectroscopy and Doppler imaging that removes the need for standard star observations. These data were obtained on the VLT with UVES during the course of an observing campaign throughout 2017 that monitored the Hill sphere transit of the exoplanet $β$ Pictoris b. We utilize line profile tomography as a method for the discovery of transiting exoplanets. By measuring the exoplanet distortion of the stellar line profile, we remove the need for reference star measurements. We demonstrate the method with white no…