A comprehensive study of the open cluster NGC 6866

Bostancı, Z. F.; Ak, T.; Yontan, Talar; Bilir, S.; Güver, T.; Ak, S.; Çakırlı, Ö.; Özdarcan, O.; Paunzen, E.; Cat, P. De; Fu, Jian-Ning; Zhang, Yating; Hou, Yonghui; Lı, G.; Wang, Y.; Zhang, W.; Shi, Jianrong; Wu, Yue

doi:10.1093/mnras/stv1665

Cited by 33 publications

(23 citation statements)

References 54 publications

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“…On the other hand the distance to the KIC 8264293 as determined from the GAIA EDR3 parallax, 1526(38) pc, places the star in the background of the closer NGC 6866. The distance to this cluster is 1392(44) pc as estimated by Monteiro et al (2020) and 1189(75) pc according to Bostancı et al (2015). Thus, the star is most probably not a member of the cluster.…”

Section: Basic Stellar Parameter and Emission In H𝛼mentioning

confidence: 84%

“…KIC 8264293 is a B-type star with a brightness of 𝑉 = 11.264(1) mag (Bostancı et al 2015). From spectroscopic observations Hanes et al (2019) determined the effective temperature, 𝑇 eff = 13150(500) K, surface gravity, log 𝑔 = 4.08( 14) and the projected rotation velocity, 𝑉 sin 𝑖 = 284(13) km s −1 which The rectangles marked with blue dashed and solid lines represent 1𝜎 and 3𝜎 error boxes, respectively.…”

Section: Basic Stellar Parameter and Emission In H𝛼mentioning

confidence: 99%

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Seismic modeling of a very young SPB star -- KIC8264293

Szewczuk,

Walczak,

Daszyńska-Daszkiewicz

et al. 2022

Preprint

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KIC 8264293 is a fast rotating B-type pulsator observed by Kepler satellite. Its photometric variability is mainly due to pulsations in high-order g modes. Besides, we detected a weak H𝛼 emission. Thus, the second source of variability is the fluctuation in a disk around the star. The pulsational spectrum of KIC 8264293 reveals a frequency grouping and period spacing pattern. Here, we present the thorough seismic analysis of the star based on these features. Taking into account the position of the star in the HR diagram and fitting the 14 frequencies that form the period spacing we constrain the internal structure of the star. We conclude that the star barely left the ZAMS and the best seismic model has 𝑀 = 3.54 M , 𝑉 rot = 248 km s −1 and 𝑍 = 0.0112. We found the upper limit on the mixing at the edge of the convective core, with the overshooting parameter up to 𝑓 ov = 0.03. On the other hand, we were not able to constrain the envelope mixing for the star. To excite the modes in the observed frequency range, we had to modify the opacity data. Our best seismic model with an opacity increase by 100% at the "nickel" bump log 𝑇 = 5.46 explains the whole instability. KIC 8264293 is the unique, very young star pulsating in high-order g modes with the Be feature. However, it is not obvious whether the source of this circumstellar matter is the ejection of mass from the underlying star or whether the star has retained its protostellar disk.

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Section: Basic Stellar Parameter and Emission In H𝛼mentioning

confidence: 84%

Section: Basic Stellar Parameter and Emission In H𝛼mentioning

confidence: 99%

Seismic modeling of a very young SPB star -- KIC8264293

Szewczuk,

Walczak,

Daszyńska-Daszkiewicz

et al. 2022

Preprint

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“…To avoid degeneracies between the parameters, it is important to measure astrophysical parameters separately. Indeed, reddening and age values in particular can suffer from degeneracies, and the uncertainties of these parameters can be higher than expected (Bilir et al 2010; Bostancı et al 2015; Yontan et al 2015). In order to achieve the best fit of isochrones during the calculations, we fitted them on CMDs with an emphasis on the main‐sequence and turn‐off members of the clusters.…”

Section: Cluster Parametersmentioning

confidence: 98%

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

Yontan

Bilir

et al. 2021

Astron Nachr

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We present reddening, photometric metallicity, age, and distance estimates for the Frolov 1 and NGC 7510 open clusters based on charge-coupled device (CCD) UBV photometric and Gaia data. Photometric observations were collected using the 1-m telescope of the TÜBİTAK National Observatory. Gaia data release 2 (DR2) proper motion data in the direction of two groupings were used to identify cluster membership. We determined mean proper motion values of ( α cos δ, δ ) = (− 3.02 ± 0.10, − 1.75 ± 0.08) and (−3.66 ± 0.07, −2.17 ± 0.06) mas year −1 for Frolov 1 and NGC 7510, respectively. We used two-color diagrams to obtain E(B − V) color excesses for Frolov 1 and NGC 7510 of 0.65 ± 0.06 and 1.05 ± 0.05 mag, respectively. We derived the photometric metallicity of Frolov 1 as [Fe/H] = 0.03 ± 0.03 dex and adopted a solar metallicity for NGC 7510. Based on these reddening and metallicities, we determined the distance moduli and ages of the clusters by fitting stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (PARSEC) isochrones to the cluster color-magnitude diagrams. Isochrone-fitting distances for Frolov 1 and NGC 7510 are 2, 864 ± 254 and 2, 818 ± 247 pc, respectively, which correspond to the ages 35 ± 10 Myr and 18 ± 6 Myr. We also calculated mean Gaia distances and compared them with those given in the literature and in this study, concluding that our results are in good agreement with previous work. Finally, we calculated the mass function slopes and found them to be X = −1.21 ± 0.18 for Frolov 1 and X = −1.42 ± 0.27 for NGC 7510.

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“…In this section we summarised the techniques applied during the cluster analyses (for detailed analyses on methods used see Bilir et al (2006Bilir et al ( , 2010Bilir et al ( , 2016; Yontan et al (2015Yontan et al ( , 2019Yontan et al ( , 2021; Bostancı et al (2015Bostancı et al ( , 2018; Ak et al (2016); Banks et al (2020)). We estimated reddening and photometric metallicities from TCDs on an individual basis, then keeping these parameters as a constants we fitted theoretical isochrones on CMDs to determine distance moduli and age simultaneously.…”

Section: Astrophysical Parameters Of the Clustersmentioning

confidence: 99%

A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data

Akbulut,

Ak,

Yontan

et al. 2021

Preprint

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A comprehensive study of the open cluster NGC 6866

Cited by 33 publications

References 54 publications

Seismic modeling of a very young SPB star -- KIC8264293

Seismic modeling of a very young SPB star -- KIC8264293

A study of open clusters Frolov 1 andNGC7510 usingCCD UBVphotometry and GaiaDR2astrometry

A study of the Czernik 2 and NGC 7654 open clusters using CCD UBV photometric and Gaia EDR3 data

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