Search for variable stars in the open cluster NGC 2509

Dar, Ahsana; Parihar, Padmakar; Saleh, Parvej Reja; Malik, Manzoor Ahmad

doi:10.1016/j.newast.2018.04.002

Cited by 5 publications

(2 citation statements)

References 17 publications

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“…It also provides opportunity to verify stellar evolution theory and offer constraints for understanding the structure and the evolution of the Galaxy (Dias et al 2002;Piskunov et al 2006). The study of variable stars in large number of open clusters have been carried out in the past; some of the recent work can be found in Zejda et al (2012); Balona et al (2013); Venuti et al (2015); Dar et al (2018); Lata et al (2019); Michalska (2019) where large number of δ-Scuti stars, γ Doradus variables, slow pulsating B stars and other kind of variable stars are reported. However, cluster NGC 1960 has not been studied for variability aspect so far.…”

Section: Introductionmentioning

confidence: 99%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a comprehensive photometric analysis of a young open cluster NGC 1960 (= M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86±0.05 mas and mean proper motions of µ RA = -0.143±0.008 mas yr −1 , µ Dec = -3.395±0.008 mas yr −1 . We obtain basic parameters of the cluster such as E(B − V) = 0.24±0.02 mag, log(Age/yr)=7.44±0.02, and d = 1.17±0.06 kpc. The mass function slope in the cluster for the stars in the mass range of 0.72-7.32 M ⊙ is found to be γ = -1.26±0.19. We find that mass segregation is still taking place in the cluster which is yet to be dynamically relaxed. This work also presents first high-precision variability survey in the central 13 ′ × 13 ′ region of the cluster. The V band photometric data accumulated on 43 nights over a period of more than 3 years reveals 76 variable stars among which 72 are periodic variables. Among them, 59 are short-period (P < 1 day)and 13 are long-period (P > 1 day). The variable stars have V magnitudes ranging between 9.1 to 19.4 mag and periods between 41 minutes to 10.74 days. On the basis of their locations in the H-R diagram, periods and characteristic light curves, the 20 periodic variables belong to the cluster. We classified them as 2 δ-Scuti, 3 γ-Dor, 2 slowly pulsating B stars, 5 rotational variables, 2 non-pulsating B stars and 6 as miscellaneous variables.

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Section: Introductionmentioning

confidence: 99%

Photometric, kinematic, and variability study in the young open cluster NGC 1960

Joshi

Maurya

John

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Stars in the ensemble identified as variables were also removed from the ensemble and this process was repeated iteratively, until all the selected stars in the ensemble were found to be non-variable. The same procedure was adopted in Dar et al (2018a) and Dar et al (2018b). For standardization, we used the criteria adopted in Wang et al (2015), Kang et al (2007) and Kiss et al (2001).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Variable stars in M37

Dar¹,

Parihar²,

Saleh³

et al. 2018

Res. Astron. Astrophys.

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The CCD photometric observations of open star cluster M37 (NGC 2099) were carried out up to a limiting magnitude of V ∼ 20 in both B and V filters to search for variable stars using a 2k×4k CCD and the 1.3 m telescope at the Vainu Bapu Observatory, Kavalur. A total of 314 stars were in the first observing run, out of which 60 were identified as variables. Eight out of the identified 60 variables are classified as W UMa binary stars. For model fitting, we used PHOEBE based on the W-D code to estimate the physical parameters of these newly detected W UMa binaries that theoretically best match the observed light curves.

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