On the nature of the δ Scuti star HD 115520

Peña, J. H.; Fox, Lance; Cervantes-Sodi, B.; Peña, Ricardo de la; Muñoz, G. M.; Vargas, Baudilio Acosta; Sareyan, J. P.; Álvarez, M.; Cano, Mariana; Sorcia, M.

doi:10.1088/1742-6596/118/1/012067

Cited by 15 publications

(36 citation statements)

References 9 publications

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“…If the photometric system is well-defined and calibrated, it provides an efficient way to investigate physical conditions such as effective temperature and surface gravity via a direct comparison of the unreddened indexes with those obtained from the theoretical models. These calibrations have already been described and used in previous analyses (Peña & Peniche;1994;Peña & Sareyan, 2006). The reduction was done considering the accuracy of the standard stars.…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

“…As was stated in Peña et al (2016) reporting on BO Lyn, the observational pattern, as well as the reduction procedure, have been employed at the SPM Observatory since 1986 and hence, have been described many times. A detailed description of the methodology can be found in Peña et al (2007). Over the seven nights of observation, the following procedure was used: for each measurement at least five ten-second integrations of each star and one ten-second integration of the sky for the uvby filters and the narrow and wide filters that define Hβ were taken.…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

“…In all but HD190849 the standard deviations are on the order of hundredths of magnitude. The large dispersion of this star could be due to variability, as in the case of HD 115520 (Peña et al, 2007) The file 6260-t7.txt lists the photometric values of HD 220735. In this Table column 1 reports the time of the observation in HJD, columns 2 to 5 list the Strömgren values V , (b − y), m 1 and c 1 , respectively; column 6, Hβ; the remaining columns list the unreddened indexes…”

Section: Data Acquisition and Reductionmentioning

confidence: 99%

“…Position of the HD220735 star in the [m 1 ] − [c 1 ] diagram of alpha Per (Peña & Sareyan, 2006) Position of the HD30110 star in the [m 1 ] − [c 1 ] diagram of alpha Per(Peña & Sareyan, 2006) …”

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confidence: 99%

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HD220735 and HD30110, new short period variable stars

Peña¹,

Soni²,

Rentería³

et al. 2019

IBVS

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Section: Data Acquisition and Reductionmentioning

confidence: 99%

Section: Data Acquisition and Reductionmentioning

confidence: 99%

Section: Data Acquisition and Reductionmentioning

confidence: 99%

mentioning

confidence: 99%

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HD220735 and HD30110, new short period variable stars

Peña¹,

Soni²,

Rentería³

et al. 2019

IBVS

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“…Trullols et al (1989) provide E ( b − y ) for 12 F star members: the mean E ( b − y ) is 0.065 ± 0.012, where the standard error again indicates little if no variation from star to star. Peña & Sareyan (2006) provided Strömgren photometry for cluster stars from a combination of their own measurements and published values and obtained a mean reddening from 169 stars of E ( b − y ) = 0.073 ± 0.038. However, for the 15 F stars in common, their reddening [ E ( b − y ) = 0.086 ± 0.029] differs from that of Crawford & Barnes, suggesting calibration differences.…”

Section: Stellar Parametersmentioning

confidence: 99%

Lithium abundances in the α Per cluster

Balachandran

Mallik

Lambert

2010

Monthly Notices of the Royal Astronomical Society

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Lithium (Li) abundances are presented and discussed for 70 members of the 50‐Myr‐old open cluster α Per. More than half of the abundances are from new high‐resolution spectra. The Li abundance in the F‐type stars is equal to its presumed initial abundance, confirming previous suggestions that pre‐main‐sequence depletion is ineffective for these stars. Intrinsic star‐to‐star scatter in Li abundance among these stars is comparable to the measurement uncertainties. There is marginal evidence that the stars of high projected rotational velocity (v sin i) follow a different abundance versus temperature trend from the slow rotators. For stars cooler than about 5500 K, the Li abundance declines steeply with decreasing temperature and there develops a star‐to‐star scatter in the Li abundance. This scatter is shown to resemble the well‐documented scatter seen in the 70‐Myr‐old Pleiades cluster. The scatter appears to be far less pronounced in the 30‐Myr clusters, which have been studied for Li abundance.

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Physical parameter determination of seven RR Lyrae stars in Bootes

Peña¹

2007

cia

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uvby β photoelectric photometry of the RR Lyrae stars AE, RS, ST, TV, TW, UU, and XX Bootis has been acquired in order to determine the physical parameters of the stars. We used the correlation between the Fourier parameters derived from the light curves and the physical parameters such as the absolute magnitude Mv , intrinsic colour (B − V ) 0 and metal abundance [Fe/H]. Once reddening has been determined, unreddened indices are obtained and T eff and log g followed along the cycle, using a comparison with the theoretical models given for our determined metallicity. AnalysisOur knowledge on stellar evolution comes from a direct comparison between the observational determination of the star's basic physical parameters (i.e. T eff , g , luminosity, metallicity and eventual pulsation periods) and models. In the case of the RR Lyrae variables, some of the goals can be attained from the relationships that have been developed by Kovács & Jurcsik in several papers , 1997, Jurcsik 1998. As Kovács & Walker (2001) state in their review paper, this method is empirical and based on the assumption that the period and the shape of the light curve are directly correlated with the physical parameters. Since we have obtained simultaneous uvby β photoelectric photometry, the precise variation of these parameters along the cycle can be determined for each star.The observations were all taken at the Observatorio Astronómico Nacional, Mexico. The 1.5m telescope, to which a spectrophotometer was attached, was used in all seasons. The physical parameters can be determined with the ad-hoc models. From the data of several photometric campaigns we obtained uvby β photometry, which was used to calculate the physical parameters of each star. The fit with our observations has been considered as reasonable when the rms error is the same order of magnitude as the detected amplitude. Reddening has been estimated by considering different objects in the same direction. Once reddening has been fixed, the unreddened Strömgren indices give the variation along the cycle of the effective temperature and surface gravity. These results are summarized in Table 1 which reports the physical parameters. The last two columns list the number of data points and the standard deviation of the residuals.Acknowledgments. This paper was partially supported by Papiit IN108106. This article has made use of the SIMBAD database operated at CDS, Strasbourg, France and ADS, NASA Astrophysics Data Systems hosted by Harvard-Smithsonian Center for Astrophysics.

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On the nature of the δ Scuti star HD 115520

Cited by 15 publications

References 9 publications

HD220735 and HD30110, new short period variable stars

HD220735 and HD30110, new short period variable stars

Lithium abundances in the α Per cluster

Physical parameter determination of seven RR Lyrae stars in Bootes

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