A variable star survey of the open cluster M 37

Kiss, L. L.; Szabó, Gy. M.; Sziladi, K.; Fürész, Gábor; Sárneczky, K.; Csák, B.

doi:10.1051/0004-6361:20010980

Cited by 34 publications

(68 citation statements)

References 12 publications

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“…HW Vir itself was discovered by Menzies & Marang (1986), who determined the period. Kilkenny et al (1994) observed a change in the orbital period for the first time, which motivated further studies (e.g., Çakirli & Devlen 1999;Wood & Saffer 1999;Kiss et al 2000;Kilkenny et al 2000Kilkenny et al , 2003Ibanoǧlu et al 2004). Many possible explanations have been proposed and discussed, converging towards the existence of a third object with a long period and low mass.…”

Section: Appendix A: Notes On Individual Systemsmentioning

confidence: 75%

Origin of apparent period variations in eclipsing post-common-envelope binaries

Zorotovic

Schreiber

2013

A&A

122

163

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Context. Apparent period variations detected in several eclipsing, close-compact binaries are frequently interpreted as being caused by circumbinary giant planets. This interpretation raises the question of the origin of the potential planets that must have either formed in the primordial circumbinary disk, together with the host binary star, and survived its evolution into a close-compact binary or formed in a post-common-envelope circumbinary disk that remained bound to the post-common-envelope binary (PCEB). Aims. Here we combine current knowledge of planet formation and the statistics of giant planets around primordial and evolved binary stars with the theory of close-compact binary star evolution aiming to derive new constraints on possible formation scenarios. Methods. We compiled a comprehensive list of observed eclipsing PCEBs, estimated the fraction of systems showing apparent period variations, reconstructed the evolutionary history of the PCEBs, and performed binary population models of PCEBs to characterize their main sequence binary progenitors. We reviewed the currently available constraints on the fraction of PCEB progenitors that host circumbinary giant planets. Results. We find that the progenitors of PCEBs are very unlikely to be frequent hosts of giant planets ( < ∼ 10 per cent), while the frequency of PCEBs with observed apparent period variations is very high (∼90 per cent). Conclusions. The variations in eclipse timings measured in eclipsing PCEBs are probably not caused by first-generation planets that survived common-envelope evolution. The remaining options for explaining the observed period variations are second-generation planet formation or perhaps variations in the shape of a magnetically active secondary star. We suggest observational tests for both options.

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Section: Appendix A: Notes On Individual Systemsmentioning

confidence: 75%

Origin of apparent period variations in eclipsing post-common-envelope binaries

Zorotovic

Schreiber

2013

A&A

122

163

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“…The masterlist was fed to DAOSPEC, Tsarevskii & Abakumov (1971), Dawson & Ianna (1998), and Bragaglia & Tosi (2006). (b) Averages of measurements by West (1967a), Jennens & Helfer (1975), Lyngå (1987), Mermilliod et al (1996), Twarog et al (1997), Kiss et al (2001), Kalirai et al (2001), Nilakshi & Sagar (2002), Grocholski & Sarajedini (2003), Bragaglia & Tosi (2006), and Hartman et al (2008). (c) Averages of measurements by McClure et al (1974), Barbaro & Pigatto (1984), Vandenberg (1985), Lyngå (1987), AnthonyTwarog et al (1990), Carraro & Chiosi (1994), Demarque et al (1994), Twarog et al (1997), Tadross et al (2002), and Grocholski & Sarajedini (2003).…”

Section: Linelist Atomic Data and Equivalent Widthsmentioning

confidence: 99%

“…(a) Star names and I C and R magnitudes from Dawson & Ianna (1998); coordinates and B and V magnitudes from Bragaglia & Tosi (2003); K S magnitudes from 2MASS. (b) Star names from van Zeipel & Lindgren (1921); coordinates from Kiss et al (2001); B and V magnitudes from Kalirai et al (2001); I C magnitudes from Nilakshi & Sagar (2002); K S magnitudes from 2MASS (c) Star names from Cannon & Lloyd (1970); coordinates from Stetson (2000) and Lasker et al (1990); B and V magnitudes from Anthony- Twarog et al (1990); I C and R magnitudes from Stetson (2000); K S magnitudes from 2MASS. (d) Star names from Fagerholm (1906); coordinates from Fan et al (1996); B, V and I C magnitudes from Sandquist (2004); B magnitude for star 286 and R magnitudes from Janes & Smith (1984); K S magnitudes from 2MASS.…”

Section: Introductionmentioning

confidence: 99%

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Pancino

Carrera

Rossetti

et al. 2010

A&A

196

206

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Context. The present number of Galactic Open Clusters that have high resolution abundance determinations, not only of [Fe/H], but also of other key elements, is largely insufficient to enable a clear modeling of the Galactic Disk chemical evolution. Aims. To increase the number of Galactic Open Clusters with high quality measurements. Methods. We obtained high resolution (R∼30 000), high quality (S/N∼50-100 per pixel), echelle spectra with the fiber spectrograph FOCES, at Calar Alto, Spain, for three red clump stars in each of five Open Clusters. We used the classical Equivalent Width analysis method to obtain accurate abundances of sixteen elements: Al,

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“…The colour excess E(B −V ), apparent distance modulus (m − M ) and log (age) values determined by various investigators (see Table 1) for the cluster range from 0.27 to 0.31; 11.5 to 11.8 and 8.3 to 8.7 respectively. In the cluster region, Robin (1982) provides UBV electronographic magnitudes of mostly uncrowded stars up to a limiting magnitude in V ∼ 20 with an accuracy of 0.055 mag in V , Kiss et al (2001) 0.075 mag in B and 0.10 mag in U . The first variable star survey of M 37 carried out by Kiss et al (2001) using CCD observations discovered 7 new variables in the cluster region.…”

Section: Describe It As a Loosementioning

confidence: 99%

“…In the cluster region, Robin (1982) provides UBV electronographic magnitudes of mostly uncrowded stars up to a limiting magnitude in V ∼ 20 with an accuracy of 0.055 mag in V , Kiss et al (2001) 0.075 mag in B and 0.10 mag in U . The first variable star survey of M 37 carried out by Kiss et al (2001) using CCD observations discovered 7 new variables in the cluster region. Mermilliod et al (1996) presented radial velocity measurements for 55 red giants while Glushkova & Rastorguev (1991) published such measurements for 9 red giants.…”

Section: Describe It As a Loosementioning

confidence: 99%

A comprehensive study of the rich open star cluster NGC 2099 based on deep $\vec{BVI}$ CCD observations

Nilakshi¹,

Sagar²

2002

A&A

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Abstract. The CCD observations of the rich open star cluster NGC 2099 and its surrounding field region have been carried out up to a limiting magnitude of V ∼ 22 mag in B, V and I passbands for the first time. A total of ∼12 000 stars have been observed in the area of about 24 × 34 in the cluster region, as well as ∼2180 stars in the ∼12 × 12 area of the field region located ∼45 away from the cluster center. The cluster parameters determined by fitting the convective core overshoot isochrones in the V, (B − V ) and V, (V − I) diagrams are E(B − V ) = 0.30 ± 0.04 mag, distance = 1360 ± 100 pc, age = 400 Myr and metallicity Z = 0.008. A welldefined cluster main sequence spread over about 8 mag in range is observed for the first time. Its intrinsic spread amounting to ∼0.06 mag in colour is almost the same over the entire brightness and can be understood in terms of the presence of physical/optical binaries. The core and cluster radii determined from the radial stellar density profiles are 185 and 1000 respectively. Only about 22% of cluster members are present in the core region. The effects of mass segregation, most probably due to dynamical evolution, have been observed in the cluster. The mass function slope of the entire cluster is ∼−0.67 ± 0.12. It becomes closer to the Salpeter value of −1.35, if flattening in the cluster mass function due to presence of both binaries and a much more extended corona is considered.

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A variable star survey of the open cluster M 37

Cited by 34 publications

References 12 publications

Origin of apparent period variations in eclipsing post-common-envelope binaries

Origin of apparent period variations in eclipsing post-common-envelope binaries

Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

A comprehensive study of the rich open star cluster NGC 2099 based on deep $\vec{BVI}$ CCD observations

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