Photometric study of a pulsating component in the eclipsing binary Y Cam

Kim, S.-L.; Lee, J. W.; Youn, Jae-Hyuck; Kwon, S. G.; Kim, C.

doi:10.1051/0004-6361:20020777

Cited by 31 publications

(24 citation statements)

References 7 publications

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“…28 And (Rodríguez et al 1998b). As mentioned in , changes in the pulsational amplitude have also been found in the hotter component of the Algol‐type eclipsing binary systems RZ Cas and Y Cam (Kim et al 2002; Rodríguez et al 2004a).…”

Section: Pulsationmentioning

confidence: 85%

“…These findings were confirmed by the parallel spectroscopic observations carried out by Lehmann & Mkrtichian (2004), who detected corresponding low‐amplitude radial velocity variations. Photometric amplitude variations have been detected in Y Cam (Kim et al 2002) too.…”

Section: Introductionmentioning

confidence: 96%

“…Thus, only data sets with very high quality lead to successful detections. Some well‐known examples have been studied recently: RZ Cas (Ohshima et al 2001; Rodríguez et al 2004a), AS Eri (Mkrtichian et al 2004) and Y Cam (Kim et al 2002; Rodríguez et al, in preparation).…”

Section: Introductionmentioning

confidence: 99%

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δ Sct-type pulsations in eclipsing binary systems: AB Cas

Rodríguez‐López¹,

García²,

Gamarova³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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This paper presents simultaneous Strömgren uvby observations carried out during the years 1998 and 1999 on the Algol-type eclipsing binary system AB Cas, where the primary component is a δ Sct-type pulsator. These observations include complete binary uvby light curves which have been analysed using the Wilson-Devinney code. The new results are compared with those from the literature. The residuals from the computed binary light curves were then analysed for their pulsational content. A single frequency was found to be sufficient to describe the out-of-eclipse pulsational behaviour. Nevertheless, some indications of the existence of secondary frequencies are also found. The main period was found to be constant during the last twenty years, making use of the classical O − C method, but an increase in its amplitude is detected during the year 1998 as compared with other epochs. Concerning the nature of the pulsations, methods based on the phase shifts and amplitude ratios between different filters were used for out-of-eclipse data and the Spatial Filtration method for observations during the primary eclipses. All methods lead to the same result: the dominant pulsation is radial, confirming previous results from earlier works. In fact, neither significant amplitude variations nor phase shifts, relative to the pulsational out-of-eclipse behaviour, are found when the primary component is hidden during primary eclipse. An iterative process was also carried out to improve both the binary and pulsation solutions, but the final results remained essentially the same.

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Section: Pulsationmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 96%

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δ Sct-type pulsations in eclipsing binary systems: AB Cas

Rodríguez‐López¹,

García²,

Gamarova³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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“…Such systems are spectacular targets for asteroseismology, because independent determination of the physical parameters (mass, radius, temperature), applying binary star astrophysics, gives strong constraints on the possible mode identification (e.g. Mkrtichian et al 2002;Kim et al 2002a). In addition, eclipses of a pulsating star give spatial resolution across the stellar surface and thereby provide the possibility for mode identification (e.g.…”

Section: V6: An Eclipsing Binary With a Pulsating Component?mentioning

confidence: 99%

The first CCD photometric study of the open cluster NGC 2126

Gáspár

Kiss

Bedding

et al. 2003

A&A

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Abstract. We present the first CCD photometric observations of the northern open cluster NGC 2126. Data were taken on eight nights in February and December 2002 with a total time span of ∼57 hours. Almost 1000 individual V-band frames were examined to find short-period variable stars. We discovered six new variable stars, of which one is a promising candidate for an eclipsing binary with a pulsating component. Two stars were classified as δ Scuti stars and one as Algol-type eclipsing binary. Two stars are slow variables with ambiguous classification. From absolute V(RI) C photometry we have estimated the main characteristics of the cluster:m 15) and d = 1.3 ± 0.6 kpc. Cluster membership is suggested for three variable stars from their positions on the colour-magnitude diagram.

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“…In addition, two new variables were recently discovered: TW Dra (Kusakin et al 2001) and GK Dra (Dallaporta et al 2002). Among these eleven variables, three stars of AB Cas Send offprint requests to: S.-L. Kim, e-mail: slkim@kao.re.kr Table 4 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/231 (Rodríguez et al1998), RZ Cas (Ohshima et al 2001) and Y Cam (Kim et al 2002a) have been studied photometrically in detail at a single observing site. From the multisite photometric campaign of AS Eri, Mkrtichian et al (2003a) detected three oscillation modes around 24 min.…”

Section: Introductionmentioning

confidence: 99%

Search for A–F Spectral type pulsating components in Algol-type eclipsing binary systems

Kim

Lee

Kwon

et al. 2003

A&A

Self Cite

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Abstract. We present the results of a systematic search for pulsating components in Algol-type eclipsing binary systems. A total number of 14 eclipsing binaries with A-F spectral type primary components were observed for 22 nights. We confirmed small-amplitude oscillating features of a recently detected pulsator TW Dra, which has a pulsating period of 0.053 day and a semi-amplitude of about 5 mmag in B-passband. We discovered new pulsating components in two eclipsing binaries of RX Hya and AB Per. The primary component of RX Hya is pulsating with a dominant period of 0.052 day and a semi-amplitude of about 7 mmag. AB Per has also a pulsating component with a period of 0.196 day and a semi-amplitude of about 10 mmag in B-passband. We suggest that these two new pulsators are members of the newly introduced group of mass-accreting pulsating stars in semi-detached Algol-type eclipsing binary systems.

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Photometric study of a pulsating component in the eclipsing binary Y Cam

Cited by 31 publications

References 7 publications

δ Sct-type pulsations in eclipsing binary systems: AB Cas

δ Sct-type pulsations in eclipsing binary systems: AB Cas

The first CCD photometric study of the open cluster NGC 2126

Search for A–F Spectral type pulsating components in Algol-type eclipsing binary systems

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