THEORETICAL p-MODE OSCILLATION FREQUENCIES FOR THE RAPIDLY ROTATING δ SCUTI STAR α OPHIUCHI
THEORETICAL p-MODE OSCILLATION FREQUENCIES FOR THE RAPIDLY ROTATING δ SCUTI STAR α OPHIUCHI
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快速旋转 δ SCUTI 星 α OPHIUCHI 的理论 p 模振荡频率
DOI：
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
R. Deupree
中科院分区：
文献类型：
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作者：
R. Deupree
演化出一个旋转的二维恒星模型来匹配 α Oph 的近似条件。轴对称和非轴对称振荡频率都是针对二维旋转模型计算的，该模型近似 α Oph 的属性。将这些计算出的频率与观察到的频率进行比较。振荡计算是假设本征函数可以用六个勒让德多项式拟合进行的，但与八个勒让德多项式的比较计算表明，频率平均一致在约 0.26% 以内。两组假定数量的勒让德多项式的特征函数的表面水平形状不太一致，但所有计算都显示与单个勒让德多项式的特征函数有显着偏差。尽管小间距的估计比较复杂，但仍然可以确定大间距。添加非轴对称模式 |m| ≤ 4，频率空间变得足够密集，以至于很难评论计算的频率与观测到的频率的拟合是否充分。虽然非轴对称频率模式分裂不再均匀，但相同 m 的正值和负值的频率之间的频率差仍然是旋转速率的 2m 倍。
A rotating, two-dimensional stellar model is evolved to match the approximate conditions of α Oph. Both axisymmetric and nonaxisymmetric oscillation frequencies are computed for two-dimensional rotating models which approximate the properties of α Oph. These computed frequencies are compared to the observed frequencies. Oscillation calculations are made assuming the eigenfunction can be fitted with six Legendre polynomials, but comparison calculations with eight Legendre polynomials show the frequencies agree to within about 0.26% on average. The surface horizontal shape of the eigenfunctions for the two sets of assumed number of Legendre polynomials agrees less well, but all calculations show significant departures from that of a single Legendre polynomial. It is still possible to determine the large separation, although the small separation is more complicated to estimate. With the addition of the nonaxisymmetric modes with |m| ⩽ 4, the frequency space becomes sufficiently dense that it is difficult to comment on the adequacy of the fit of the computed to the observed frequencies. While the nonaxisymmetric frequency mode splitting is no longer uniform, the frequency difference between the frequencies for positive and negative values of the same m remains 2m times the rotation rate.