Photoelectric photometry and period analysis of selected Delta Scuti 
stars in Praesepe

Peña, J. H.; Peniche, R.; Hobart, M. A.; Rolland, A.; Coca, P. López de; Paparó, M.; Parrao, L.; Cruz, C. de La; Olivares, J.; Costa, V.; İbanoǧlu, C.; Ertan, A. Y.; Tümer, O. T.; Evren, S.; Tunca, Z.

doi:10.1051/aas:1998170

Cited by 7 publications

(3 citation statements)

References 32 publications

(47 reference statements)

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“…How do the new frequencies compare with those found in previous, smaller studies (Breger 1973;Guerrero, Mantegazza & Scardia 1997;Breger 1980;Kim & Lee 1995;Freyhammer, Larsen & Petersen 1997;Hernandez et al 1998;Pena et al 1998)? All studies have detected the dominant frequency of 9.78 cd −1 , while the 7.02 cd −1 frequency usually was also seen.…”

Section: Frequency Analysesmentioning

confidence: 56%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

Breger,

Hareter,

Endl

et al. 2012

Preprint

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The Praesepe cluster contains a number of δ Sct and γ Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) δ Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd −1 . After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain.

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Section: Frequency Analysesmentioning

confidence: 56%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

Breger,

Hareter,

Endl

et al. 2012

Preprint

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“…Raboud & Mermilliod (1998) identified it as an SB1 on the basis of old radial velocity measurements, but Abt & Willmarth (1999) found it to have constant radial velocity. The star has been identified as photometrically variable in the older literature, but recent studies have used it as a constant photometric comparison star for δ Sct studies (Hernandez et al 1998;Pena et al 1998). HD 72942 / KW 534: HD 72942 is a known single-lined spectroscopic binary with an orbital period of 131.96 d (Abt & Willmarth 1999), indicating a lack of interaction between the stars.…”

Section: Discussionmentioning

confidence: 99%

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

Morales,

Sandquist,

Schaefer

et al. 2022

Preprint

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We observe the brightest member of the Praesepe cluster, Cnc, to precisely measure the characteristics of the stars in this binary system, en route to a new measurement of the cluster's age. We present spectroscopic radial velocity measurements and interferometric observations of the sky-projected orbit to derive the masses, which we find to be M 1 /M = 2.420 ± 0.008 and M 2 /M = 2.226 ± 0.004. We place limits on the color-magnitude positions of the stars by using spectroscopic and interferometric luminosity ratios while trying to reproduce the spectral energy distribution of Cnc. We re-examine the cluster membership of stars at the bright end of the color-magnitude diagram using Gaia data and literature radial velocity information. The binary star data are consistent with an age of 637 ± 19 Myr, as determined from MIST model isochrones. The masses and luminosities of the stars appear to select models with the most commonly used amount of convective core overshooting.

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“…The analysis of HD 200925 was carried out with Fourier analysis and least squares fitting methods. The computing packages utilizing AnaFre, PERIOD 468 Peria et al and MUFRAN have been described in Pena et al (1998). One of the first conclusions we can reach is the existence of one stable period of pulsation that corresponds to the frequency of 3.741 d _ 1 and the associated values of 2 / = 7.482 d _ 1 and 3 / = 11.223 d _ 1 .…”

Section: Discussionmentioning

confidence: 99%

Physical Parameter Determination for the δ Scuti Star HD 200925

Peña

Paparó

Peniche

et al. 2000

International Astronomical Union Colloquium

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HD 200925 is an unusual star: the period is stable on a time scale of many years, yet it shows variations which are either large and irregular, or small, suggesting a possible Blazhko effect (Poretti 1984; Joner & Johnson 1985); it has larger values of Teff and log g derived from uvbyβ than those of dwarf Cepheids of similar period; and it has a somewhat higher metal abundance, [Fe/H], than the Hyades. Furthermore, in conflict to what Joner and McNamara (1983) determined – that m1 index shows no variation with temperature – HD 200925 shows a definite variation, unlike that predicted in Crawford (1979). No explanation of this has yet been found. Johnson & Joner (1986) also derived an unusual and unexpected value of [Fe/H]. Finally, with respect to the pulsation periods of this star, Mantegazza & Poretti (1986) determined the existence of two periods: one definite, 0.26730 d and a possible second one of 0.2138 d which yield a ratio of P2/P1 = 0.800, the theoretical ratio expected between the first and the second overtones, found in other pulsating variables. All of these facts make HD 200925 an interesting star, motivating the present study.

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Photoelectric photometry and period analysis of selected Delta Scuti stars in Praesepe

Cited by 7 publications

References 32 publications

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

Physical Parameter Determination for the δ Scuti Star HD 200925

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