New CCD photometry and light curve analysis of two WUMaBinaries: 1SWASP J133417.80+394314.4 and V2790 Orion

Shokry, Ahmed; Zead, I.; El-Depsey, M.H.; Darwish, M.S.; Hassan, I.A.; Shaltout, A.; Saad, S. M.; Nouh, M. I.

doi:10.1016/j.newast.2020.101400

Cited by 6 publications

(1 citation statement)

References 21 publications

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“…Despite their detection in surveys like ZTF [9] and GAIA [10], the number of thoroughly analysed systems remains small compared to what is detected by these surveys. To provide a broader context, many studies have focused on short-period binary systems (P 0.3 days), revealing insights into their intricate dynamics and evolution (e.g., [11][12][13][14][15][16][17][18][19][20][21]).…”

Section: Introductionmentioning

confidence: 99%

Light curve modeling of the two short period eclipsing binaries ATO J009.3383 + 34.2329 and CRTS J004004.7 + 385531

Darwish,

Abdelkawy

2024

Phys. Scr.

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In this study, we present a detailed photometric analysis of two short-period eclipsing binary systems, $\textbf{ATO J009.3383+34.2329}$ and $CRTS J004004.7+385531$. The photometric data for our analysis was obtained from the Zwicky Transient Facility (ZTF) catalogue at $gri$ filters and the Transiting Exoplanet Survey Satellite (TESS) database. Based on our analysis, we classify both systems as W Uma-type binaries, with A-subtype. To estimate the physical and geometrical parameters of these systems, we employ the PHEOBE code. This results in two totally eclipsing systems with degree of \textbf{inclination} (i) of around 68 and 88 {$\deg$}, respectively. The $ATO J009.3383+34.2329$ indicates a low mass ratio ($q$) binary with $q$=0.107, while $CRTS J004004.7+385531$ exhibits a moderate $q$ value of 0.545. A cool spot on the surface of the secondary \textbf{star} of $CRTS J004004.7+385531$ with a 30\% cooler atmosphere of the surrounding surface is detected. This is explained by \textbf{magnetic activity} on the surface of $CRTS J004004.7+385531$. Our findings reveal overcontact fill-out factor $f$ with 54 and 52\% for $ATO J009.3383+34.2329$ and $CRTS J004004.7+385531$, respectively. In addition to the light curve modeling, we calculate new epochs and ephemeris for both binary systems. The absolute parameters for the two systems are estimated. Eventually, the systems' evolutionary status along ZAMS and TAMS are discussed.

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Section: Introductionmentioning

confidence: 99%

Light curve modeling of the two short period eclipsing binaries ATO J009.3383 + 34.2329 and CRTS J004004.7 + 385531

Darwish,

Abdelkawy

2024

Phys. Scr.

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BVRcIc light curves, period and spectroscopic study of a low mass-ratio contact binary HV Aqr

et al. 2023

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Physical characterization of late-type contact binary systems observed by LAMOST: a comprehensive statistical analysis

Abdel Rahman,

Darwish

2023

Sci Rep

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This paper presents a catalog of approximately 1800 Eclipsing W UMa systems (EWs) using parameters from LAMOST, VSX, ZTF and Gaia. Our detailed statistical analysis includes frequency distributions of parameters, confidence intervals, and hypothesis testing to provide deeper insights into the physical properties of this important eclipsing binary class. We focus on key parameters, including Period, Effective Temperature, Surface Gravity, metallicity, Radial Velocity, and spectral type of the systems. Our study reveals that the mean values for period, effective temperature, logarithmic surface gravity, metallicity, and radial velocity for EW systems are 0.377 days, 5775 K, 4, -0.185, and -4.085 km/s, respectively. The 95% confidence intervals for these parameters are 0.372 to 0.382 days, 5730 to 5820 K, -0.202 to -0.168, 3.97 to 4.03, and -6.47 to -1.7 km/s, respectively. Hypothesis testing of the estimated intervals results in the acceptance of the null hypothesis, indicating that EW systems are characterized within the specified limits. Our study also confirms that the majority of EW systems are late-type stars, primarily classified as F spectral type, followed by G and K. Interestingly, among the sample, 88 systems are classified as A spectral type, with a mean surface temperature of 7400 K. We examine the correlation between orbital periods and atmospheric parameters in the VSX and ZTF catalogs. While ZTF periods align well with established relations (correlation coefficient: 0.74), a weaker correlation is found in the VSX catalog. This highlights the need for a revision of VSX periods for improved accuracy in the studied sample of EWs.

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New CCD photometry and light curve analysis of two WUMaBinaries: 1SWASP J133417.80+394314.4 and V2790 Orion

Cited by 6 publications

References 21 publications

Light curve modeling of the two short period eclipsing binaries ATO J009.3383 + 34.2329 and CRTS J004004.7 + 385531

Light curve modeling of the two short period eclipsing binaries ATO J009.3383 + 34.2329 and CRTS J004004.7 + 385531

BVRcIc light curves, period and spectroscopic study of a low mass-ratio contact binary HV Aqr

Physical characterization of late-type contact binary systems observed by LAMOST: a comprehensive statistical analysis

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