The double-mode nature of the HADS star GSC 00144-03031   and
the Petersen diagram of the class

Poretti, E.; Suárez, J. C.; Niarchos, P. G.; Gazeas, K.; Manimanis, V. N.; Cauteren, P. van; Lampens, P.; Wils, P.; Alonso, R.; Amado, P. J.; Belmonte, Juan Antonio; Butterworth, N.; Martignoni, M.; Mart́ın-Rúız, S.; Moskalik, P.; Robertson, C. W.

doi:10.1051/0004-6361:20053463

Cited by 62 publications

(70 citation statements)

References 14 publications

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“…found. The mass for RV Ari is then predicted between 1.75 and 2.01 M , in agreement with the results obtained by Poretti et al (2005) when considering solar metallicity.…”

Section: Petersen Diagrams For Rv Arisupporting

confidence: 88%

“…Nevertheless, Poretti et al (2005) have provided very recent evidence for the existence of pure radial double-mode pulsators within the HADS class and have stressed that they consitute a very homogeneous class of variable stars. Poretti et al (2005) and studied RV Ari from a theoretical point of view and in the framework of the Petersen Diagrams. While the former considered it within the subset of classic Pop.…”

Section: Introductionmentioning

confidence: 99%

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A comprehensive asteroseismic modelling of the high-amplitude δ Scuti star RV Arietis

Casas¹,

Suárez

Moya

et al. 2006

A&A

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We present a comprehensive asteroseismic study of the double-mode high-amplitude δ Scuti star HD 187642 (RV Ari). The modelling includes some of the most recent techniques: 1) effects of rotation on both equilibrium models and adiabatic oscillation spectrum, 2) non-adiabatic study of radial and non-radial modes, 3) relationship between the fundamental radial mode and the first overtone in the framework of Petersen diagrams. The analysis reveals that two of the observed frequencies are very probably identified as the fundamental and first overtone radial modes. Analysis of the colour index variations, together with theoretical non-adiabatic calculations, points to models in the range of [7065, 7245] K in effective temperature and of [1190, 1270] Myr in stellar age. These values were found to be compatible with those obtained using the three other asteroseismic techniques.

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“…found. The mass for RV Ari is then predicted between 1.75 and 2.01 M , in agreement with the results obtained by Poretti et al (2005) when considering solar metallicity.…”

Section: Petersen Diagrams For Rv Arisupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

A comprehensive asteroseismic modelling of the high-amplitude δ Scuti star RV Arietis

Casas¹,

Suárez

Moya

et al. 2006

A&A

Self Cite

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“…The typical uncertainties in the V and R magnitudes are ∼0.02 mag. Santolamazza et al 2001;Jeon et al 2003;Poretti et al 2005). Using the Cohen & Sarajedini (2012) P-L relation as before, we obtain M V = 2.228 ± 0.149 mag, μ 0 = 17.004 ± 0.149 mag, and a distance of ∼25.2 ± 1.8 kpc.…”

Section: Sx Phoenicis Stars and Candidatessupporting

confidence: 66%

Variable stars in the globular cluster NGC 7492

Jaimes

Ferro

Bramich

et al. 2013

A&A

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Aims. We have performed a photometric V, R, I CCD time-series analysis with a baseline of about eight years of the outer-halo globular cluster NGC 7492 with the aim of searching for new variables and using these (and the previously known variables) to determine the physical parameters of interest for the cluster (e.g. metallicity, absolute magnitude of the horizontal branch, distance, etc.). Methods. We used difference image analysis to extract precise light curves in the relatively crowded star field, especially towards the densely populated central region. Several different approaches were used for variability detection that recover the known variables and lead to new discoveries. We determined the physical parameters of the only RR0 star using a light-curve Fourier decomposition analysis. Results. We found one new long-period variable and two SX Phe stars in the blue straggler region. We also present one candidate SX Phe star that requires follow-up observations. Assuming that the SX Phe stars are cluster members and using the period-luminosity relation for these stars, we estimate their distances as ∼25.2 ± 1.8 and 26.8 ± 1.8 kpc, and identify their possible modes of oscillation. We refined the periods of the two RR Lyrae stars in our field of view. We found that the RR1 star V2 is undergoing a period change and possibly exhibits the Blazhko effect. A Fourier decomposition of the light curve of the RR0 star V1 allowed us to estimate a metallicity of [Fe/H] ZW ∼ −1.68 ± 0.10 or [Fe/H] UVES ∼ −1.64 ± 0.13, a log-luminosity log(L/L ) ∼ 1.76 ± 0.02, an absolute magnitude M V ∼ 0.38 ± 0.04 mag, and a true distance modulus of μ 0 ∼ 16.93 ± 0.04 mag, which is equivalent to a distance of ∼24.3 ± 0.5 kpc. All of these values are consistent with previous estimates in the literature.

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“…The firstovertone and second-overtone lines were positioned adopting the frequency ratios F/1O= 0.783 and F/2O = 0.571 (see Santolamazza et al 2001or Jeon et al 2003Poretti et al 2005). It seems clear from the plot that V164 is a fundamental pulsator while V160 and V170 pulsate in the first-overtone.…”

Section: Distance and Metallicity Of Mfrom Its Variable Starsmentioning

confidence: 99%

RR Lyrae stars and the horizontal branch of NGC 5904 (M5)

Ferro

Luna

Bramich

et al. 2016

Astrophys Space Sci

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We report the distance and [Fe/H] value for the globular cluster NGC 5904 (M5) derived from the Fourier decomposition of the light curves of selected RRab and RRc stars. The aim in doing this was to bring these parameters into the homogeneous scales established by our previous work on numerous other globular clusters, allowing a direct comparison of the horizontal branch luminosity in clusters with a wide range of metallicities. Our CCD photometry of the large variable star population of this cluster is used to discuss light curve peculiarities, like Blazhko modulations, on an individual basis. New Blazhko variables are reported.From the RRab stars we found [Fe/H] UVES = −1.335 ± 0.003(statistical) ± 0.110(systematic), and a distance of 7.6 ± 0.2 kpc, and from the RRc stars we found [Fe/H] UVES = −1.39 ± 0.03(statistical) ± 0.12(systematic) and a distance of 7.5 ± 0.3 kpc. The results for RRab and RRc stars should be considered independent since they come from different calibrations and zero points. Absolute magnitudes, radii and masses are also reported for individual RR Lyrae stars. The distance to the cluster was also calculated by alternative methods like the Period-Luminosity relation of SX Phe and the luminosity of the stars at the tip of the red giant branch, and we obtained the results 7.7 ± 0.4 and 7.2 − 7.5 kpc respectively.The distribution of RR Lyrae stars in the instability strip is discussed and compared with other clusters in connection with the Oosterhoff and horizontal branch type. The Oosterhoff type II clusters systematically show a RRab-RRc segregation about the instability strip first-overtone red edge, while the Oosterhoff type I clusters may or may not display this feature. A group of RR Lyrae stars is identified in an advanced evolutionary stage, and two of them are likely binaries with unseen companions.

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The double-mode nature of the HADS star GSC 00144-03031 and the Petersen diagram of the class

Cited by 62 publications

References 14 publications

A comprehensive asteroseismic modelling of the high-amplitude δ Scuti star RV Arietis

A comprehensive asteroseismic modelling of the high-amplitude δ Scuti star RV Arietis

Variable stars in the globular cluster NGC 7492

RR Lyrae stars and the horizontal branch of NGC 5904 (M5)

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