On detection in the second survey, the star was found to have changed slightly in brightness, suggesting that it was a new variable star. In accordance with the international standard for designation of variable stars, it was called UY Scuti, denoting it as the 38th variable star of the constellation Scutum.
UY Sct is a dust-enshrouded bright red supergiant and is classified as a semiregular variable with an approximate pulsation period of 740 days. Based on a radius of 1,708 R☉, this pulsation would be an overtone of the fundamental pulsation period, or it may be a fundamental mode corresponding to a smaller radius.
In the summer of 2012, AMBERinterferometry with the Very Large Telescope (VLT) in the Atacama Desert in Chile was used to measure the parameters of three red supergiants near the Galactic Center region: UY Scuti, AH Scorpii, and KW Sagittarii. They determined that all three stars are over 1,000 times bigger than the Sun and over 100,000 times more luminous than the Sun. The stars' sizes were calculated using the Rosseland radius, the location at which the optical depth is 2⁄3, with distances adopted from earlier publications. UY Scuti was found to be the largest and the most luminous of the three stars measured, at 1,708 ± 192 R☉ (1.188×109 ± 134,000,000 km; 7.94 ± 0.89 AU) based on an angular diameter of 5.48±0.10 mas and an assumed distance of 2.9±0.317 kiloparsecs (kpc) (about 9,500±1,030 light-years) which was originally derived in 1970 based on the modelling of the spectrum of UY Sct. The luminosity is then calculated to be 340,000 L☉ at an effective temperature of 3,365 ± 134 K, giving an initial mass of 25 M☉ (possibly up to 40 M☉ for a non-rotating star).
A hypothetical object travelling at the speed of light would be observed to take about seven hours to travel along UY Scuti's great circle whereas it would take 14.5 seconds to circle the Sun.
Direct measurements of the parallax of UY Sct published in the Gaia Data Release 2 give a parallax of 0.6433±0.1059 mas, implying a closer distance of approximately 1.5 kiloparsecs (4,900 ly), and consequently much lower luminosity and radius values of around 86,300–87,100 L☉ and 755 R☉ respectively. However, the Gaia parallax might be unreliable, at least until further observations, due to a very high level of astrometric noise.Gaia Early Data Release 3 has published a parallax of 0.5166±0.0494 mas for this star, again with a large value for astrometric noise, rated at a significance of 122 where anything over 2 is "probably significant".
UY Scuti's has no known companion star and so its mass is uncertain. However, it is expected on theoretical grounds to be between 7 and 10 M☉. Mass is being lost at 5.8×10−5M☉ per year, leading to an extensive and complex circumstellar environment of gas and dust.
Based on current models of stellar evolution, UY Scuti has begun to fuse helium, and continues to fuse hydrogen in a shell around the core. The location of UY Scuti deep within the Milky Way disc suggests that it is a metal-rich star.
After fusing heavy elements, its core will begin to produce iron, disrupting the balance of gravity and radiation in its core and resulting in a core collapse supernova. It is expected that stars like UY Scuti should evolve back to hotter temperatures to become a yellow hypergiant, luminous blue variable, or a Wolf–Rayet star, creating a strong stellar wind that will eject its outer layers and expose the core, before exploding as a type IIb, IIn, or type Ib/Ic supernova.
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