New Whole Earth Telescope observations of CD-24 7599: steps towards   Scuti star seismology

Handler, G.; Pikall, H.; O’Donoghue, D.; Buckley, D.; Vauclair, G.; Chevreton, M.; Giovannini, O.; Kepler, S. O.; Goode, P. R.; Provençal, J. L.; Wood, M. A.; Clemens, J. C.; O'Brien, M. S.; Nather, R. E.; Winget, D. E.; Kleinman, S. J.; Kanaan, A.; Watson, T. K.; Nitta, A.; Montgomery, M. H.; Klumpe, E. W.; Bradley, P. A.; Sullivan, D. J.; Wu, K. F.; Marar, T. M. K.; Seetha, S.; Ashoka, B. N.; Mahra, H. S.; Bhat, Bratati; Babu, V. C.; Leibowitz, E. M.; Hemar, Shirley; Ibbetson, P.; Mashal, E.; Meistas, E.; Dziembowski, W. A.; Pamyatnykh, A. A.; Moskalik, P.; Zoła, S.; Pajdosz, G.; Krzesinski, J.; Solheim, J. E.; Bard, S.; Massacand, C. M.; Breger, M.; Gelbmann, M.; Paunzen, E.; North, P.

doi:10.1093/mnras/286.2.303

Cited by 65 publications

(34 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Handler et al 1997). At first, we performed the Fourier analysis of the periods listed in Table 4 and found a clear maximum at 31.4 s. This also supports the spacing derived by the linear fits and by the K-S and I-V tests.…”

Section: Tests On Period Spacingssupporting

confidence: 83%

Revealing the pulsational properties of the V777 Herculis star KUV 05134+2605 by its long-term monitoring

Bognár

Paparó

Córsico

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

Context. KUV 05134+2605 is one of the 21 pulsating DB white dwarfs (V777 Her or DBV variables) known so far. The detailed investigation of the short-period and low-amplitude pulsations of these relatively faint targets requires considerable observational efforts from the ground, long-term single-site or multi-site observations. The observed amplitudes of excited modes undergo short-term variations in many cases, which makes determining pulsation modes difficult. Aims. We aim to determine the pulsation frequencies of KUV 05134+2605, find regularities between the frequency and period components, and perform an asteroseismic investigation for the first time. Methods. We re-analysed the published data and collected new measurements. We compared the frequency content of the different datasets from the different epochs and performed various tests to check the reliability of the frequency determinations. The mean period spacings were investigated with linear fits to the observed periods, Kolmogorov-Smirnov and inverse variance significance tests, and with a Fourier analysis of different period sets, including a Monte Carlo test that simulated the effect of alias ambiguities. We employed fully evolutionary DB white dwarf models for the asteroseismic investigations. Results. We identified 22 frequencies between 1280 and 2530 μHz. These form 12 groups, which suggests at least 12 possible frequencies for the asteroseismic investigations. Thanks to the extended observations, KUV 05134+2605 joined the group of rich white dwarf pulsators. We identified one triplet and at least one doublet with a ≈9 μHz frequency separation, from which we derived a stellar rotation period of 0.6 d. We determined the mean period spacings of ≈31 s and 18 s for the modes we propose as dipole and quadrupole. We found an excellent agreement between the stellar mass derived from the = 1 period spacing and the period-to-period fits, all providing M * = 0.84−0.85 M solutions. Our study suggests that KUV 05134+2605 is the most massive amongst the known V777 Her stars.

show abstract

Section: Tests On Period Spacingssupporting

confidence: 83%

Revealing the pulsational properties of the V777 Herculis star KUV 05134+2605 by its long-term monitoring

Bognár

Paparó

Córsico

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, regular frequency spacings have been observed in at least some δ Scuti stars (eg. Handler et al 1997;Breger et al 1999), and various techniques have been proposed for identifying the patterns (García Hernández et al 2013;Paparó et al 2016). Identification of frequency patterns can be quite challenging though, as Paparó et al (2016) find that in some cases, as few as 20% of the frequencies can be located on the echelle ridges.…”

Section: Frequency Spacingsmentioning

confidence: 99%

Convection and Overshoot in Models of γ Doradus and δ Scuti Stars

Lovekin

Guzik

2017

ApJ

View full text Add to dashboard Cite

We investigate the pulsation properties of stellar models representative of δ Scuti and γ Doradus variables. We have calculated a grid of stellar models from 1.2 to 2.2 M ⊙ , including the effects of both rotation and convective overshoot using MESA, and we investigate the pulsation properties of these models using GYRE. We discuss observable patterns in the frequency spacing for p modes and the period spacings for g modes. Using the observable patterns in g mode period spacings, it may be possible to observationally constrain the convective overshoot and rotation of a model. We also calculate the pulsation constant (Q) for all models in our grid, and investigate the variation with convective overshoot and rotation. The variation in Q values of radial modes can be used to place constraints on the convective overshoot and rotation of stars in this region. As a test case, we apply this method to a sample of 22 high amplitude δ Scuti stars (HADS), and provide estimates for the convective overshoot of the sample.

show abstract

“…Following the method used by Handler et al (1997) and García Hernández et al (2009), we investigated the periodicities in the 52 independent frequencies determined in the white light CoRoT data. The input data were the frequencies in the 5.6-22.7 d −1 region.…”

Section: Regular Spacing Of Modesmentioning

confidence: 99%

CoRoT 102749568: mode identification in aδScuti star based on regular spacings

Paparó

Bognár

Benkő

et al. 2013

A&A

View full text Add to dashboard Cite

Context. The high accuracy of space data increased the number of the periodicities determined for pulsating variable stars, but the mode identification is still a critical point in the non-asymptotic regime. Aims. We use regularities in frequency spacings for identifying the pulsation modes of the recently discovered δ Sct star ID 102749568. Methods. In addition to analysing CoRoT light curves (15 252 datapoints spanning 131 days), we obtained and analysed both spectroscopic and extended multi-colour photometric data. We applied standard tools (MUFRAN, Period04, SigSpec, and FAMIAS) for time-series analysis. Results. A satisfactory light-curve fit was obtaining by means of 52 independent modes and 15 combination terms. The frequency spacing revealed distinct peaks around large (25.55-31.43 μHz), intermediate (9.80, 7.66 μHz), and low (2.35 μHz) separations. We directly identified 9 modes, and the l and n values of other three modes were extrapolated. The combined application of spectroscopy, multi-colour photometry, and modelling yielded the precise physical parameters and confirmed the observational mode identification. The large separation constrained the log g and related quantities. The dominant mode is the radial first overtone.

show abstract

New Whole Earth Telescope observations of CD-24 7599: steps towards Scuti star seismology

Cited by 65 publications

References 0 publications

Revealing the pulsational properties of the V777 Herculis star KUV 05134+2605 by its long-term monitoring

Revealing the pulsational properties of the V777 Herculis star KUV 05134+2605 by its long-term monitoring

Convection and Overshoot in Models of γ Doradus and δ Scuti Stars

CoRoT 102749568: mode identification in aδScuti star based on regular spacings

Contact Info

Product

Resources

About