Utilizing a non-public observatory, astronomers have carried out the primary photometric examine of a peculiar W UMa-type binary generally known as CSS J003106.8+313347. Outcomes of the examine, printed July 27 on the preprint server arXiv, shed extra gentle on the properties of this method.
Normally, W Ursae Majoris-type, or W UMa-type binaries (EWs) are eclipsing binaries with a brief orbital interval (beneath one day) and steady gentle variation throughout a cycle. They’re composed of two dwarf stars with comparable temperature and luminosity, sharing a standard envelope of fabric and are thus involved with each other. Due to this fact, they’re usually dubbed “contact binaries.”
Situated some 4,900 light years away, CSS J003106.8+313347 is an EW with an obvious magnitude of 14.73. The orbital interval of the system is estimated to be roughly 0.344 days.
Provided that little or no is understood about CSS J003106.8+313347, a group of astronomers led by Ehsan Paki of the Binary Programs of South and North (BSN) challenge determined to take a better take a look at this method with a non-public observatory positioned in Toulon, France. They noticed the binary on two nights in late 2022 and purchased practically 300 pictures.
“We carried out the primary photometric examine of the CSS J003106.8+313347 W Ursae Majoris (W UMa)-type system primarily based on ground-based observations,” the researchers wrote within the paper.
The observations discovered that the first star of CSS J003106.8+313347 has an effective temperature of 5,477 Ok, whereas the secondary star is 321 Ok hotter. This discovering signifies that the first and secondary stars have spectral sorts G8 and G5, respectively.
In line with the examine, the first star within the CSS J003106.8+313347 system has a radius of about 1.29 solar radii and its mass is roughly 1.67 solar lots. The star’s luminosity was measured to be 1.35 solar luminosities.
Relating to the secondary element, it seems that it has a radius of round 1.09 solar radii and a mass of some 1.17 solar lots. The luminosity of this star was discovered to be at a stage of 1.22 solar luminosities.
The Hertzsprung–Russell (HR) diagram of CSS J003106.8+313347 exhibits that the first star is above the terminal-age fundamental sequence (TAMS), whereas the secondary star is between the zero-age fundamental sequence (ZAMS) and TAMS. The astronomers famous that that is in keeping with present theories attempting to elucidate the evolution of binary stars.
The observations additionally discovered that orbital angular momentum of CSS J003106.8+313347 is 52.08. The authors of the paper concluded that this discovering, along with all the brand new outcomes, means that the system is an overcontact binary.
Extra info:
Ehsan Paki et al, The First Photometric Examine of the Binary System CSS J003106.8+313347, arXiv (2023). DOI: 10.48550/arxiv.2307.15132
Journal info:
arXiv
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Analysis investigates eclipsing binary CSS J003106.8+313347 (2023, August 7)
retrieved 7 August 2023
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