A new class of rapidly pulsating star .4. Oscillations in EC 20117-4014 and atmospheric analyses

被引:69
作者
ODonoghue, D
LynasGray, AE
Kilkenny, D
Stobie, RS
Koen, C
机构
[1] UNIV OXFORD,NUCL PHYS LAB,DEPT PHYS,OXFORD OX1 3RH,ENGLAND
[2] S AFRICAN ASTRON OBSERV,ZA-7935 CAPE TOWN,CAPE,SOUTH AFRICA
关键词
binaries; general; stars; individual; EC; 20117-4014; 14026-2647; 10228-0905; PB; 8783; oscillations;
D O I
10.1093/mnras/285.3.657
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
A new class of pulsating stars, the EC 14026 stars, has recently been announced. We report the discovery of rapid oscillations in EC 20117 - 4014. The oscillations are multiperiodic with three periods detected so far: 137.3, 142.1 and 158.7 s. The peak-to-peak amplitude of these oscillations is similar to 1 per cent. Along with the spectrum and UBV colours, this implies that EC 20117 - 4014 is another member of the new class. Interestingly, there is evidence for period/phase changes in the main 137.3-s period, as no linear ephemeris can be found that will fit the collection of light curves we have obtained. We interpret the oscillations as pulsations of an sdB star in a binary with an F/G companion, as indicated by the optical spectra. In order to derive atmospheric parameters of the component stars, low- (similar to 3.5 Angstrom) and intermediate- (similar to 1 Angstrom) resolution optical spectroscopy is presented for the first four EC14026 stars to be discovered: EC14026 - 2647, EC10228 - 0905, EC 20117 - 4014 and PB 8783. Their spectra are modelled as the combination of sdB and FIG stars using a grid of high-gravity model atmospheres to represent the former, and observed spectra to represent the latter. The spectral types of the late-type companions are estimated to be in the range early F to early G. Atmospheric parameters for the sdB components of the four stars are derived and found to be similar: log g similar to 6.0 and T-eff similar to 35 000 K. If the late-type companions are on or near the main sequence, their distances agree with those estimated for the sdB components, assuming that the masses of the latter are similar to 0.5 M.. The evolutionary status of the four stars strongly suggests that the sdB component has suffered substantial mass loss by Roche lobe overflow, along the lines originally proposed by Mengel et al. This hypothesis can be tested by using the orbital time delay in the pulsations to measure the binary period and separation. The discovery of pulsations in sdB stars is important: asteroseismological studies to probe their structure and evolutionary time-scale can now be contemplated.
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页码:657 / 672
页数:16
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