References of "Telting, J. H"
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See detailSynthetic pulsational line profile variations
Oreiro, R.; Telting, J. H.; Østensen, R. H. et al

in Astrophysics & Space Science (2010), 329

We have produced simulated time series of high resolution spectroscopy for sdBs. We present the first results of testing classical mode identification techniques. Here, in particular, we analyse the ... [more ▼]

We have produced simulated time series of high resolution spectroscopy for sdBs. We present the first results of testing classical mode identification techniques. Here, in particular, we analyse the behaviour of individual spectral lines and discuss the results and applicability of the moment method. [less ▲]

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See detailA spectroscopic study of the β Cephei star 12 (DD) Lacertae
Desmet, M.; Briquet, Maryline ULg; De Cat, P. et al

in Communications in Asteroseismology (2007), 150

We present first results of a spectroscopic multisite campaign for 12 (DD) Lacertae (hereinafter 12 Lac). This star is one of the best observed β Cephei stars. It has a large number of known oscillation ... [more ▼]

We present first results of a spectroscopic multisite campaign for 12 (DD) Lacertae (hereinafter 12 Lac). This star is one of the best observed β Cephei stars. It has a large number of known oscillation frequencies but a lack of identified m-values for its detected modes. In our data set we find seven independent frequencies together with combination frequencies. In addition, two of these modes are identified: one radial mode and one prograde dipole mode. [less ▲]

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See detailDisentangling component spectra of κ Scorpii, a spectroscopic binary with a pulsating primary. II. Interpretation of the line-profile variability
Uytterhoeven, K.; Briquet, Maryline ULg; Aerts, C. et al

in Astronomy and Astrophysics (2005), 432

We analyse the complex short-term SiIII line-profile variability of the spectroscopic binary β Cep star κ Scorpii after orbit subtraction, before and after spectral disentangling. We refine the known ... [more ▼]

We analyse the complex short-term SiIII line-profile variability of the spectroscopic binary β Cep star κ Scorpii after orbit subtraction, before and after spectral disentangling. We refine the known oscillation frequency of the star: f[SUB]1[/SUB]=4.99922 c d[SUP]-1[/SUP] and detect 2f[SUB]1[/SUB]. Variability is also found at frequencies near f[SUB]2[/SUB]≃ 4.85 c d[SUP]-1[/SUP] and f[SUB]3[/SUB]≃ 5.69 c d[SUP]-1[/SUP] or their aliases. These frequencies are not significant if we consider the spectra alone, but they survive our selection after the consideration that they were derived previously from independent ground-based and space photometry by different teams. Moreover, we find dominant variability in the equivalent width with a frequency in the interval [0.22,0.30] c d[SUP]-1[/SUP] which we interpret as the rotational frequency f[SUB]rot[/SUB] of the star. The complex window function does not allow us to determine definite values for f[SUB]2[/SUB], f[SUB]3[/SUB], f[SUB]rot[/SUB]. The variability with f[SUB]1[/SUB] is interpreted as a prograde non-radial oscillation mode with spherical wavenumbers (ℓ,m)=(2,-1) or (1,-1). The additional frequencies are explained in terms of rotational modulation superposed to the main oscillation. We also point out that we cannot disprove the variability in κ Scorpii to originate from co-rotating structures. KOREL disentangling preserves the large-amplitude line-profile variability but its performance for complex low-amplitude variability remains to be studied in detail. Based on observations obtained with the Coudé Échelle Spectrograph on the ESO CAT telescope and with the CORALIE échelle spectrograph on the 1.2-m Euler Swiss telescope, both situated at La Silla, Chile. [less ▲]

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See detailAsteroseismology of the β Cephei star ν Eridani - III. Extended frequency analysis and mode identification
De Ridder, J.; Telting, J. H.; Balona, L. A. et al

in Monthly Notices of the Royal Astronomical Society (2004), 351

Using the large photometric and spectroscopic data sets of the ν Eridani multisite campaign given in our two recent papers (Aerts et al. and Handler et al.), we present an extended frequency analysis and ... [more ▼]

Using the large photometric and spectroscopic data sets of the ν Eridani multisite campaign given in our two recent papers (Aerts et al. and Handler et al.), we present an extended frequency analysis and a photometric mode identification. For the extended frequency analysis, we used an improved radial velocity time series, the second-moment time series and the line profiles themselves. In the radial velocity time series, we can now detect an additional pulsation frequency that was previously only found in photometric time series. We also report several new candidate pulsation frequencies. For seven frequencies, the photometric mode identification indicates that they belong to a radial mode and six dipole modes, and for three frequencies the degree l could not be unambiguously determined. We also placed ν Eri in the Hertzsprung-Russell diagram by determining T[SUB]eff[/SUB] using Geneva plus Strömgren photometric calibrations, spectral energy distribution fitting, by non-local thermodynamic equilibrium hydrogen, helium and silicon line profile fitting, and by determining log(L/L[SUB]solar[/SUB]) using the Hipparcos parallax and an Hβ calibration. [less ▲]

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