期刊文献+

仙王座β型变星νEri的测光和高分辨率分光观测和脉动模示分析

The Photometry and High-resolution Spectroscopy and The pulsational Mode of the β Cephei variable Star v Eridani
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摘要 β Cephei stars are pulsational stars with short periods. So far, their pulsational me-chanicses, the separating of the multiple periods and the pulsational mode are still outstanding issues. In the recent years, it is very active to study pulsational modes and shock wave phenomena with line profile variations.In this paper, based on the photometric data (observed in Nov., 1991) and high resolution, high S / N spectra (observed in Dec., 1991) of v Eri, we have obtained its pulsational periods and modes, we have also confirmed that there are shock wave activities on it.We applied a Fourier analysis method in the separating multiple pulsational periods snd have gotten the following results: P1=0.d2150, P2 = 0.d1766, P3 = 0d.1508. Using Stamford and Watson’s continuum flux examination method, we have determined the pulsational mode of every period: P1 and P3 are nonradial pulsational modes with 1= 1, and 1 = 2 respectively, P2 corresponds to a radial pulsational mode.A series of spectra-handling programs named SPYD have been worked out to handle the spectra of v Eri near Si Ⅲ (4567A) region, and we have obtained the equivalent widths, full width at half maximum, radial velocities of Si Ⅲ (4567A), SiⅢ(4574A) lines with these programs. Most of their variations have shown to be related to the shock wave activities for v Eri. β Cephei stars are pulsational stars with short periods. So far, their pulsational me-chanicses, the separating of the multiple periods and the pulsational mode are still outstanding issues. In the recent years, it is very active to study pulsational modes and shock wave phenomena with line profile variations. In this paper, based on the photometric data (observed in Nov., 1991) and high resolution, high S / N spectra (observed in Dec., 1991) of v Eri, we have obtained its pulsational periods and modes, we have also confirmed that there are shock wave activities on it. We applied a Fourier analysis method in the separating multiple pulsational periods snd have gotten the following results: P1=0.d2150, P2 = 0.d1766, P3 = 0d.1508. Using Stamford and Watson's continuum flux examination method, we have determined the pulsational mode of every period: P1 and P3 are nonradial pulsational modes with 1= 1, and 1 = 2 respectively, P2 corresponds to a radial pulsational mode. A series of spectra-handling programs named SPYD have been worked out to handle the spectra of v Eri near Si Ⅲ (4567A) region, and we have obtained the equivalent widths, full width at half maximum, radial velocities of Si Ⅲ (4567A), SiⅢ(4574A) lines with these programs. Most of their variations have shown to be related to the shock wave activities for v Eri.
出处 《紫金山天文台台刊》 北大核心 1994年第1期75-75,共1页
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