用标准和旋转模型匹配PMS星的频谱
Matching the frequency spectrum of PMS stars by means of standard and rotating models
摘要：
我们应用ATON程序计算了标准（非旋转）和旋转主序前（PMS）模型的详细网格，计算了它们的绝热振荡谱，目的是探索年轻恒星的地震性质。我们采用了一种类似的匹配模式的方法Guenther和布朗利用，必要时，我们的旋转进化代码来计算PMS星的模型。该方法描述了一个初步的应用程序的频谱的两个PMS星（85和278）在年轻的疏散星团NGC 6530。对于星85，我们确认，与自洽旋转模型，以前的解释的数据，归因于三个接近的频率模式n=4，l=1和m=0，+1，-1。对于恒星278，我们发现了一个不同的频率拟合，对应于恒星原始误差框内的模型，并质疑这颗恒星的有效温度远低于径向不稳定带的红色边界的可能性。
英文摘要：
We applied the ATON code to the computation of detailed grids of standard (non--rotating) and rotating Pre--Main Sequence (PMS) models and computed their adiabatic oscillation spectra,with the aim of exploring the seismic properties of young stars. We adopt a method similar to the matching mode method by Guenther and Brown making use, when necessary, also of our rotating evolutionary code to compute the models for PMS stars. The method is described by a preliminary application to the frequency spectrum of two PMS stars (85 and 278) in the young open cluster NGC 6530. For the Star 85 we confirm, with self--consistent rotating models, previous interpretation of the data, attributing three close frequencies to the mode n=4, l=1 and m=0,+1,--1. For the Star 278 we find a different fit for the frequencies, corresponding to a model within the original error box of the star, and dispute the possibility thatthis star has an effective temperature much cooler that the red boundary of the radial instability strip.
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