摘要：Pulsating variables ofγDoradus type (γDor) and slowly pulsating B-type (SPB) stars are found on and near the main sequence with typical periods varying between one and several days, making them rather hard to detect from the ground. It is only with space missions such as CoRoT andKeplerthat we became truly capable of determining their oscillation frequencies with enough precision to perform in-depth analyses. Here we present an efficient and easy-to-implement seismic tool, in which the frequency (ν) and the square root of the frequency difference ($ \sqrt{\Delta \nu} $) are plotted against each other as the abscissa and the ordinate, respectively. This allows us to immediately (1) perform mode identification; (2) estimate the average rotation rate and the characteristic period of gravity modes; and (3) recognise certain physical effects, including buoyancy glitches and avoided crossings. This diagnostic tool can only be applied to prograde sectoralgmodes. To validate the tool presented here, we used stellar models and also applied it to threeγDor (KIC 12066947,KIC 5608334andKIC 4846809) and one SPB star (KIC 3459297), all observed withKepler. Furthermore, we show that the rotation rates determined using this new tool are consistent with the results of previous studies.
关键词：enasteroseismologystars: oscillationsstars: rotationmethods: data analysis
