Synthetic RR Lyrae velocity curves

Liu, Tianxing

doi:10.1086/132809

Cited by 53 publications

(78 citation statements)

References 7 publications

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“…M5-V8, on the other hand, shows only very weak traces of such a dip, although a similar bump is present in the visual light curve for this star. These findings are in good agreement with those of Liu (1991) for field RR Lyr and three M4 RR Lyr. M92-V1, unfor- 0.6 0.8 1.0 0.8 0.9 0.7 0.7 0.6 0.7 0.5 0.5 0.6 1.0 0.9 0.9 0.7 0.8 0.8 0.7 0.6 0.6 0.6 0.6 0.8 0.9 0.8 0.6 0.9 1.6 0.7 0.9 0.9 1.1 1.1 0.8 0.9 0.9 1.1 1.3 0.8 1.0 0.9 0.7 0.8 0.9 0.6 0.8 1.1 tunately, lacks coverage of this interesting phase region.…”

Section: Resultssupporting

confidence: 91%

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Storm

Carney

Latham

et al. 1992

PASP

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ABSTRACT. Radial-velocity curves are presented for the RR Lyrae stars VI and V3 in the lowmetallicity globular cluster M92 (NGC 6341) and V8 and V28 in the intermediate-metallicity globular cluster M5 (NGC 5904) based on between 50 and 90 observations per star. The radial velocities were derived by cross-correlating spectra obtained with the Multiple Mirror Telescope echelle spectrograph with synthetic templates calculated using Kurucz's model atmospheres (ATLAS8) and synthetic spectrum (SYNTHE) codes. The synthetic templates provide a better match to the observed spectra than the available observed templates, especially for the metal-poor stars, resulting in high-precision radialvelocities good to a few km s -1 in most cases. We find systemic velocities of -125.4, -122.6, +48.7, and +53.6 km s -1 for M92-V1, M92-V3, M5-V8, and M5-V28, respectively, in good agreement with previous determinations of cluster mean velocities.

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Section: Resultssupporting

confidence: 91%

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Storm

Carney

Latham

et al. 1992

PASP

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“…In this paper we reexamine the light change variations of Blazhko stars utilizing the A V -A v rad relation, compare the measured and calculated [Fe/H] values (Jurcsik & Kovács 1996) at different Blazhko phases, and measure the compatibility of the light curves with that of normal RRab stars using the interrelations between the Fourier parameters (Kovács & Kanbur 1998) Liu (1991) provides the opportunity and also makes it necessary to refine the positions of Blazhko variables on this diagram. In order to do so, the literature was searched for radial velocity measurements of known Blazhko variables.…”

Section: Introductionmentioning

confidence: 99%

Blazhko stars: Always distorted?

Jurcsik¹,

Benkő²,

Szeidl³

2002

A&A

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Abstract.A reexamination of the amplitude ratios of the photometric and radial velocity changes of Blazhko RRab stars in their different Blazhko phases shows that a normal amplitude ratio occurs near the phase of maximum amplitude. Checking the Fourier parameters of maximum amplitude light curves with different methods proved, however, that none of these light curves can be regarded as a normal RR Lyrae type light curve.

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“…The A puls − AV relation determined by Liu (1991) in comparison with the M3 results is shown in Fig. 11.…”

Section: A Puls − Av Relation Of Rrl Starsmentioning

confidence: 99%

“…Liu (1991) has found that, in contrast with the large diversity of the shapes of the light curves, the shapes of the available sample of RRL RV curves is relatively stable; actually only their amplitudes are scaled according to the amplitude of the light curve. The Fourier parameters of the V light-curves and the RV curves of stable RRab stars in M3 are compared in Fig.…”

Section: Fourier Parameters Of the V Light Curve And The Radial-velocmentioning

confidence: 99%

“…Based on photometric and spectroscopic data, Liu (1991) derived a linear relation between the pulsation amplitude (ARV puls = pARV; p:projection factor) and the V amplitude of stable-light-curve RRab stars. The ARV − AV relation of a Blazhko star in different phases of the modulation seems, however, to be star by star different and steeper than that of stable RRab stars (Jurcsik et al 2002).…”

Section: A Puls − Av Relation Of Rrl Starsmentioning

confidence: 99%

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Photometric and radial-velocity time series of RR Lyrae stars in M3: analysis of single-mode variables

Jurcsik

Smitola

Hajdu

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first simultaneous photometric and spectroscopic investigation of a large set of RR Lyrae variables in a globular cluster. The radial-velocity data presented comprise the largest sample of RVs of RR Lyrae stars ever obtained. The target is M3; BV I C time-series of 111 and b flux data of further 64 RRab stars, and RV data of 79 RR Lyrae stars are published. Blazhko modulation of the light curves of 47 percent of the RRab stars are detected. The mean value of the center-of-mass velocities of RR Lyrae stars is −146.8 km s −1 with 4.52 km s −1 standard deviation, which is in good agreement with the results obtained for the red giants of the cluster. The Φ 21 RV phase difference of the RV curves of RRab stars is found to be uniformly constant both for the M3 and for Galactic field RRab stars; no period or metallicity dependence of the Φ 21 RV is detected. The Baade-Wesselink distances of 26 non-Blazhko variables with the best phase-coverage radial-velocity curves are determined; the corresponding distance of the cluster, 10480 ± 210 pc, agrees with the previous literature information. A quadratic formula for the A puls −A V relation of RRab stars is given, which is valid for both OoI and OoII variables. We also show that the (V − I) 0 of RRab stars measured at light minimum is period dependent, there is at least 0.1 mag difference between the colours at minimum light of the shortest-and longest-period variables.

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Synthetic RR Lyrae velocity curves

Cited by 53 publications

References 7 publications

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Blazhko stars: Always distorted?

Photometric and radial-velocity time series of RR Lyrae stars in M3: analysis of single-mode variables

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