Variable stars in the globular cluster NGC 6362

Mazur, B.; Kałużny, J.; Krzemiński, W.

doi:10.1046/j.1365-8711.1999.02588.x

Cited by 21 publications

(37 citation statements)

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“…REFERENCES.È(1) Kaluzny et al 1998b ; (2) Kaluzny et al 1997b ;(8) Kaluzny et al 1998a ;(9) Mateo et al 1990 ; (10) Yan & Reid 1996 ;(11) Drissen & Shara 1998 ;(12) Olech et al 1999 ;(13) Kaluzny et al 1999 ;(14) Kaluzny et al 1997c ;(15) Mazur et al 1999 ;(16) Rubenstein & Bailyn 1996 ;(17) Kaluzny 1997 ;(18) Layden et al 1999 ;(19) Thompson et al 1999 ;(20) 3. The color-magnitude of the core of NGC 6752 has been studied with the Hubble Space T elescope (Rubenstein & Bailyn 1997).…”

Section: èèèèèèèèèèèèèèèmentioning

confidence: 99%

W UMa-Type Binary Stars in Globular Clusters

Ruciński

2000

162

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A sample of 86 contact binary systems in 14 globular clusters with available color index data in B[V or in V [I has been analyzed. A large fraction of all systems (at least one-third) are numerous foreground Galactic disk projections over long lines of sight to the clusters. Since the selection of the cluster members has been based on the calibrations, the matter of a metallicity correction M V (log P, color) required particular attention with the result that such a correction is apparently not needed at the present level of accuracy. Analysis of the color-magnitude and period-color relations shows that globular cluster members have di †erent properties from the Galactic disk contact systems : They are underluminous mainly because of the smaller sizes and, consequently, have shorter orbital periods ; the colorindex e †ect of the diminished blanketing is relatively less important, especially for V [I. Among the class 1 members (deviations in smaller than 0.5 mag), the most common are blue straggler (BS) systems. M V The variability amplitudes for the BS systems show a signiÐcantly di †erent distribution from that for systems below the turn-o † point (TOP) : The BS systems in the sample have only small amplitudes (which may be an indication of small mass ratios), while the distribution for the systems below the TOP is peculiar in containing only large-amplitude systems. This di †erence may be linked to the relatively small number of the detected main-sequence contact systems below the TOP as resulting from an observational selection e †ect due to the rapidly increasing measurement difficulties below the TOP. As a consequence, e †orts at determining the frequency of occurrence of the contact systems below the TOP have been judged to be premature. The frequency among the BS stars could be moderately well established at about 45^10 BS stars per one contact BS binary ; thus, contact binaries are about 3 times more common among the BS stars than among the disk population dwarfs. Contact binary systems with periods longer than 0.6 days are absent in the sample, possibly because the more massive stars have left the contact binary domain.

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Section: èèèèèèèèèèèèèèèmentioning

confidence: 99%

W UMa-Type Binary Stars in Globular Clusters

Ruciński

2000

162

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“…Recently Mazur, Kaluzny & Krzemiński (1999) published results of a charge‐coupled device (CCD) search for short‐period variables in NGC 6362. They discovered 19 new candidates, of which five were cluster RR Lyr stars, four were SX Phe stars and eight were eclipsing binaries.…”

Section: Introductionmentioning

confidence: 99%

The Clusters AgeS Experiment (CASE): RR Lyrae variables in the globular cluster NGC 6362

Olech¹,

Kałużny²,

Thompson³

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We present V‐ and B‐band charge‐coupled device (CCD) photometry of 35 RR Lyr stars in the Southern hemisphere globular cluster NGC 6362. Fourier decomposition of the light curves was used to estimate the basic properties of these variables. From the analysis of the RRc stars we obtain a mean mass M=0.531±0.014 M⊙, luminosity log L/L⊙=1.656±0.006, effective temperature Teff=7429±20 and helium abundance Y=0.292±0.002. The mean values of the absolute magnitude, metallicity (on Jurcsik's scale) and effective temperature for 14 RRab stars with ‘regular’ light curves are: MV=0.86±0.01,[Fe/H]=−0.93±0.04 and Teff=6555±25, respectively. From the B−V colours, periods and metallicities of the RRab stars we estimate the colour excess for NGC 6362 to be equal to E(B−V)=0.08±0.01. Using this value we derive the colours of the blue and red edges of the instability strip in NGC 6362 to be (B−V)BE0=0.17 and (B−V)RE0=0.43. From the relations between the Fourier coefficients of RRab and RRc stars and their absolute magnitudes we estimate the apparent distance modulus to NGC 6362 to be (m−M)V=14.46±0.10. From the mean value of log L/L⊙ of the RRc stars we obtain 14.59±0.03. The V‐band light curves of three of the RRc stars exhibit changes in amplitude of over 0.1 mag on the time‐scale of around one week. Near the radial first overtone frequency we find one or two peaks, which strongly suggests that these variables belong to the newly identified group of non‐radial pulsating RR Lyr stars.

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“…The period of the system is around ∼0 d .4052 and B-V=0.66 which corresponds to G5 spectral type (Kaluzny et al 1993, Mazur et al 1999. The maxima and minima are not the same in the I passband and the difference is …”

Section: Variable V1mentioning

confidence: 97%

“…the effective temperature for star 1 is taken on the basis of un-reddened B-V values published by Mazur et al (1999) and using the Allen's table (2000). The secondary component effective temperature (T e,c ) was Since no spectroscopic observations are available for the variables, We had to constrain the most important parameter mass-ratio q=m2/m1.…”

Section: Photometric Solutionsmentioning

confidence: 99%

Photometric study of W UMa type binaries in the old open cluster Berkeley 39

Sriram

Kiron

Rao

2009

Res. Astron. Astrophys.

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The study of W UMa binary systems give a wealth of information about its nature as well as about its parent body (if any), like clusters. In this paper, we present the I passband photometric solutions of four W UMa binaries in the open cluster Berkeley 39 using the latest version of W-D program. The result shows that, two binary systems are W-subtype W UMa binary systems and another two systems are H-subtype W UMa binary systems. No third body is found in any of the four systems. We found a correlation between the period and mass-ratio as well as temperature and mass-ratio for the respective variables which is similar to the relationship between mass ratio and total mass of the contact binaries as shown by van't Veer (1996) and Li et al. (2008).

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Variable stars in the globular cluster NGC 6362

Cited by 21 publications

References 50 publications

W UMa-Type Binary Stars in Globular Clusters

W UMa-Type Binary Stars in Globular Clusters

The Clusters AgeS Experiment (CASE): RR Lyrae variables in the globular cluster NGC 6362

Photometric study of W UMa type binaries in the old open cluster Berkeley 39

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