The multimode pulsation of the<i>δ</i>Scuti star V784 Cassiopeae

Kiss, L. L.; Derekas, A.; Alfaro, E. J.; Bíró, I; Csák, B.; Garrido, R.; Szatmáry, K.; Thomson, James Robertson

doi:10.1051/0004-6361:20021058

Cited by 10 publications

(13 citation statements)

References 29 publications

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“…The mean H p magnitude is 7.077 ± 0.005, which in turn yields V = 7.00 for B T − V T = 0.33 (Bessell 2000). This value and the full amplitude of 0.21 mag as well agree with those reported by Kiss et al (1999). The 2K/Δm v = 23.1/0.21 = 110 km s −1 mag −1 value supports radial pulsation.…”

Section: Cetsupporting

confidence: 83%

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Understanding the dynamical structure of pulsating stars

Nardetto

Poretti

Rainer

et al. 2014

A&A

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Context. High-resolution spectroscopy is a powerful tool to study the dynamical structure of a pulsating star's atmosphere. Aims. We aim at comparing the line asymmetry and velocity of the two δ Sct stars ρ Pup and DX Cet with previous spectroscopic data obtained on classical Cepheids and β Cep stars. Methods. We obtained, analysed and discuss HARPS high-resolution spectra of ρ Pup and DX Cet. We derived the same physical quantities as used in previous studies, which are the first-moment radial velocities and the bi-Gaussian spectral line asymmetries. Results. The identification of f = 7.098 d −1 as a fundamental radial mode and the very accurate Hipparcos parallax promote ρ Pup as the best standard candle to test the period-luminosity relations of δ Sct stars. The action of small-amplitude nonradial modes can be seen as well-defined cycle-to-cycle variations in the radial velocity measurements of ρ Pup. Using the spectral-line asymmetry method, we also found the centre-of-mass velocities of ρ Pup and DX Cet, V γ = 47.49 ± 0.07 km s −1 and V γ = 25.75 ± 0.06 km s −1 , respectively. By comparing our results with previous HARPS observations of classical Cepheids and β Cep stars, we confirm the linear relation between the atmospheric velocity gradient and the amplitude of the radial velocity curve, but only for amplitudes larger than 22.5 km s −1 . For lower values of the velocity amplitude (i.e., <22.5 km s −1 ), our data on ρ Pup seem to indicate that the velocity gradient is null, but this result needs to be confirmed with additional data. We derived the Baade-Wesselink projection factor p = 1.36 ± 0.02 for ρ Pup and p = 1.39 ± 0.02 for DX Cet. We successfully extended the period-projection factor relation from classical Cepheids to δ Scuti stars.

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Section: Cetsupporting

confidence: 83%

“…DX Cet ≡ HD 16189 is a bright high-amplitude δ Sct (HADS) star with a period P = 0.103939529 d and full amplitude of 0.20 mag in V light (Kiss et al 1999). Stellar parameters were obtained from uvbyβ photometry (Kiss et al 1999;Stetson 1991): T eff = 7250 ± 200 K, log g = 3.6 ± 0.2 dex.…”

Section: Introductionmentioning

confidence: 99%

Understanding the dynamical structure of pulsating stars

Nardetto

Poretti

Rainer

et al. 2014

A&A

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“…In some cases, this classification is incorrect or doubtful. For instance, DX Cet is actually a δ Sct star (Kiss et al 1999). This star is, in fact, of special interest as having a parallax with a small percentage error and falling on the PL relation for fundamental mode δ Sct pulsators (van Leeuwen 2007a).…”

Section: The Rr Lyrae Variablesmentioning

confidence: 99%

The luminosities and distance scales of type II Cepheid and RR Lyrae variables

Feast

Laney

Kinman

et al. 2008

Monthly Notices RAS

141

173

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Infrared and optical absolute magnitudes are derived for the type II Cepheids κ Pav and VY Pyx using revised Hipparcos parallaxes and for κ Pav, V553 Cen and SW Tau from pulsational parallaxes. Revised Hipparcos and HST parallaxes for RR Lyrae agree satisfactorily and are combined in deriving absolute magnitudes. Phase‐corrected J, H and Ks mags are given for 142 Hipparcos RR Lyraes based on Two‐Micron All‐Sky Survey observations. Pulsation and trigonometrical parallaxes for classical Cepheids are compared to establish the best value for the projection factor (p) used in pulsational analyses. The MV of RR Lyrae itself is 0.16 ± 0.12 mag brighter than predicted from an MV–[Fe/H] relation based on RR Lyrae stars in the Large Magellanic Cloud (LMC) at a modulus of 18.39 ± 0.05 as found from classical Cepheids. This is consistent with the prediction of Catelan & Cortés that it is overluminous for its metallicity. The results for the metal‐ and carbon‐rich Galactic disc stars, V553 Cen and SW Tau, each with small internal errors (±0.08 mag) have a mean deviation of only 0.02 mag from the period–luminosity (PL) relation established by Matsunaga et al. for type II Cepheids in globular clusters and with a zero‐point based on the same LMC‐scale. Comparing directly the luminosities of these two stars with published data on type II Cepheids in the LMC and in the Galactic bulge leads to an LMC modulus of 18.37 ± 0.09 and a distance to the Galactic Centre of R0= 7.64 ± 0.21 kpc. The data for VY Pyx agree with these results within the uncertainties set by its parallax. Evidence is presented that κ Pav may have a close companion and possible implications of this are discussed. If the pulsational parallax of this star is incorporated in the analyses, the distance scales just discussed will be increased by ∼0.15 ± 0.15 mag. V553 Cen and SW Tau show that at optical wavelengths PL relations are wider for field stars than for those in globular clusters. This is probably due to a narrower range of masses in the latter case.

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“…We have divided the data into three subsets, in which the changes of the dominant frequency can be neglected. Nightly mean values have been subtracted (as did, e.g., Kiss et al 2002a) and that is why we had to exclude a few nights with short light curve coverage from the analysis. The first subset covered -01-31-1997the second 1999-01-26-1999and Fig.…”

Section: Be Lyncismentioning

confidence: 99%

A photometric monitoring of bright high-amplitudeδScuti stars

Derekas

Kiss

Székely

et al. 2003

A&A

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Abstract. We present new photometric data for seven high-amplitude δ Scuti stars. The observations were acquired between 1996 and 2002, mostly in the Johnson photometric system. For one star (GW UMa), our observations are the first since the discovery of its pulsational nature from the Hipparcos data. The primary goal of this project was to update our knowledge on the period variations of the target stars. For this, we have collected all available photometric observations from the literature and constructed decades-long O−C diagrams of the stars. This traditional method is useful because of the single-periodic nature of the light variations. Text-book examples of slow period evolution (XX Cyg, DY Her, DY Peg) and cyclic period changes due to light-time effect (LITE) in a binary system (SZ Lyn) are updated with the new observations. For YZ Boo, we find a period decrease instead of increase. The previously suggested LITE-solution of BE Lyn (Kiss & Szatmáry 1995) is not supported with the new O−C diagram. Instead of that, we suspect the presence of transient light curve shape variations mimicking small period changes.

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The multimode pulsation of theδScuti star V784 Cassiopeae

Cited by 10 publications

References 29 publications

Understanding the dynamical structure of pulsating stars

Understanding the dynamical structure of pulsating stars

The luminosities and distance scales of type II Cepheid and RR Lyrae variables

A photometric monitoring of bright high-amplitudeδScuti stars

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