An asteroseismic study of the β Cephei star θ Ophiuchi: photometric results

We have carried out a three-site photometric campaign for the β Cephei star θ Oph from 2003 April to August. 245 h of differential photoelectric u v y photometry were obtained during 77 clear nights. The frequency analysis of our measurements has resulted in the detection of seven pulsation modes within a narrow frequency interval between 7.116 and 7.973 c d⁻¹. No combination or harmonic frequencies have been found. We have performed a mode identification of the individual pulsations from our colour photometry that shows the presence of one radial mode, one rotationally split  ℓ= 1  triplet and possibly three components of a rotationally split  ℓ= 2  quintuplet. We discuss the implications of our findings and point out the similarity of the pulsation spectrum of θ Oph to that of another β Cephei star, V836 Cen.     

Lessons for asteroseismology from white dwarf stars

The interpretation of pulsation data for sun-like stars is currently facing challenges quite similar to those faced by white dwarf modelers ten years ago. The observational requirements for uninterrupted long-term monitoring are beginning to be satisfied by successful multi-site campaigns and dedicated satellite missions. But exploration of the most important physical parameters in theoretical models has been fairly limited, making it difficult to establish a detailed best-fit model for a particular set of oscillation frequencies. I review the past development and the current state of white dwarf asteroseismology, with an emphasis on what this can tell us about the road to success for asteroseismology of other types of stars.     

Acoustic wave reflection by stellar cores: can it be seen in the autocorrelation function of p-mode measurements?

The rapid variation of density with depth in a stellar core can distort acoustic wave propagation in stellar interiors, producing a reflected wave. The reflectivity can come from a rapid density change at the boundary of a convective core, or from the steep gradients established in a radiative core during chemical evolution. We analyse this wave reflection within the framework of wave scattering theory, and address the question of the detectability of the reflected wave in the autocorrelation function of stellar p-mode measurements.     

长江下游越冬期冷暖长期变化与大型环流低频振动

本文运用上海112年月平均温度资料和1月、10月的月平均海平面气压场110年资料,分析了以上海资料为代表的长江下游地区越冬季节温度由偏冷转向偏暖的长期变化及其有关联的大型环流系统的低频振动。发现近百年中前冬11月、12月和后冬2月这三个月的冷暖长期变化相似,特点是前50年左右偏冷占优势;后50年左右偏暖占优势,相应地10月大型环流中亚洲大陆冷高压的优势是前50年偏强偏东;后50年偏弱偏西,北太平洋高压的变化趋势则是前50年偏弱;后50年偏强。1月气温的长期变化与上述11月、12月和2月的冷暖变化不同,对应的大型环流低频振动也不同。     

热带大气中30～60天低频振荡的CISK-Rossby波理论

本文根据低纬热带大气中的风压场平衡关系对CISK-Rossby波进行了研究,指出对于弱对流加热,CISK-Rossby波既可以向东西方向传播,又可以向南北方向传播,并且这种弱对流加热所激发的CISK-Rossby波是一种稳定的减幅波;对于强对流加热,这种CISK-Rossby波减速并向东和向北传播,其传播特征与30～60天低频振荡的特征比较一致,并且这种CISK-Rossby波又是一种不稳定的增幅波,在10°N和17°N地区,经向波长为6000km的CISK-Rossby波的e倍增幅时间分别为6天和8天。因此,CISK-Rossby波可能是30～60天低频振荡的触发机制。