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J/A+A/542/A55       Analysis of the B3IV star HD 43317      (Papics+, 2012)

Gravito-inertial and pressure modes detected in the B3 IV CoRoT target HD 43317. Papics P.I., Briquet M., Baglin A., Poretti E., Aerts C., Degroote P., Tkatchenko A., Morel T., Zima W., Niemczura E., Rainer M., Hareter M., Baudin F., Catala C., Michel E., Samadi R., Auvergne M. <Astron. Astrophys. 542, A55 (2012)> =2012A&A...542A..55P
ADC_Keywords: Stars, variable ; Stars, B-type Keywords: asteroseismology - stars: variables: general - stars: abundances - stars: oscillations - stars: individual: HD 43317 - stars: rotation Abstract: OB stars are important building blocks of the Universe, but we have only a limited sample of them well understood enough from an asteroseismological point of view to provide feedback on the current evolutionary models. Our study adds one special case to this sample, with more observational constraints than for most of these stars. Our goal is to analyse and interpret the pulsational behaviour of the B3 IV star HD 43317 using the CoRoT light curve along with the ground-based spectroscopy gathered by the Harps instrument. This way we continue our efforts to map the Beta Cep and SPB instability strips. We used different techniques to reveal the abundances and fundamental stellar parameters from the newly-obtained high-resolution spectra. We used various time-series analysis tools to explore the nature of variations present in the light curve. We calculated the moments and used the pixel-by-pixel method to look for line profile variations in the high- resolution spectra. We find that HD 43317 is a single fast rotator (vrot∼50%vcrit) and hybrid SPB/Beta Cep-type pulsator with Solar metal abundances. We interpret the variations in photometry and spectroscopy as a result of rotational modulation connected to surface inhomogeneities, combined with the presence of both g and p mode pulsations. We detect a series of ten consecutive frequencies with an almost constant period spacing of 6339s as well as a second shorter sequence consisting of seven frequencies with a spacing of 6380s. The dominant frequencies fall in the regime of gravito- inertial modes. Description: Table A.1. Fourier parameters (frequencies (fj), amplitudes (Aj), and phases (thetaj)) of peaks which are common in both halves of the data (marked with a 1 in the note column), as well as additional ones which have a S/N ratio above 4 when computed over the full periodogram. The displayed S/N values are calculated in a window of 1d-1 or 3d-1 centred on the given frequency, or from the full periodogram (from 0d-1 to 20d-1). Objects: ------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------- 06 15 47.01 +04 17 01.1 HD 43317 = HR 2232 ------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 116 424 Fourier parameters
See also: B/corot : CoRoT observation log Release 8 (CoRoT, 2012) J/A+A/482/L17 : CoRoT space mission. I. (Barge+, 2008) J/A+A/506/471 : Frequency analysis of CoRoT B stars (Degroote+, 2009) J/A+A/525/A23 : Frequency analysis of HD 49434 (Mathias+, 2011) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 10 F10.6 d-1 Freq Frequency from Fourier analysis 16- 23 F8.6 d-1 e_Freq Frequency error 27- 33 F7.1 10-6 Amp Amplitude, in ppm (part per million) 40- 43 F4.1 10-6 e_Amp Amplitude error, in ppm (part per million) 48- 54 F7.4 --- Phase [-0.5/0.5] Phase (2π/rad) 59- 65 F7.4 --- e_Phase Phase error 69- 73 F5.1 --- S/N1 Signal-to-noise in a 1d-1 wide window around Freq 77- 81 F5.1 --- S/N3 Signal-to-noise in a 3d-1 wide window around Freq 85- 89 F5.1 --- S/Nf Signal-to-noise computed over full periodogram 97-116 A20 --- Notes Notes (frot is the rotational frequency)
Acknowledgements: Peter I. Papics, Peter.Papics(at)
(End) P. Papics [Inst. Sterrenkunde, KU Leuven], P. Vannier [CDS] 26-Mar-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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