UY Scuti
Star in the constellation Scutum
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Nomenclature and observational history
UY Scuti was first catalogued in 1860 by German astronomers at the Bonn Observatory, who were completing a survey of stars for the Bonner Durchmusterung Stellar Catalogue. It was designated BD-12°5055, the 5,055th star between 12°S and 13°S counting from 0h right ascension.
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 Scuti is located a few degrees north of the A-type star Gamma Scuti and northeast of the Eagle Nebula. It is also near the Scutum OB3 association, which is located between 1.33 and 2.23 kiloparsecs (kpc) away, although it is not considered to be a member. Although the star is very luminous, it is, at its brightest, only 9th magnitude as viewed from Earth, due to its distance and location in the Zone of Avoidance within the Cygnus rift.
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Characteristics
UY Scuti is a dust-enshrouded bright red supergiant, losing its mass at 5.8×10−5 M☉ per year, which leads to an extensive and complex circumstellar environment of gas and dust. Sometimes described as an extreme red supergiant or hypergiant, it has been compared to another pulsating but cooler supergiant, S Persei, and is also found to be a maser source of H
2O, SiO, and OH masers. However, they are too weak for the star to be considered a true OH/IR supergiant, unlike VY Canis Majoris and IRC +10420. It has some emission-lines and is classified as a semiregular variable with an approximate pulsation period of 740 days. Based on an old 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.
The distance of UY Scuti is poorly known, but most estimates place it somewhere around 2 kpc. It has no known companion star, and so its mass is also uncertain. However, it is expected on theoretical grounds to be between 7 and 10 M☉.
In mid 2012, AMBER interferometry 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 analyzed to be the largest, the most luminous and the coolest 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 kpc (about 9,500±1,030 light-years) which was originally derived in 1970 based on the modelling of the spectrum of UY Scuti. 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). The calculated radius has led UY Sct to be sometimes described as the largest star known. However, potentially larger radius estimates have already been implied and published for other supergiant stars, such as VX Sagittarii, NML Cygni, MY Cephei, and Stephenson 2 DFK 1. In addition, other leading candidates have been suggested, such as frequently both VY Canis Majoris and the extragalactic WOH G64 A, which resides within the Large Magellanic Cloud.
Direct measurements of the parallax of UY Scuti published in the Gaia Data Release 2 give a parallax of 0.6433±0.1059 mas, implying a much 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 due to a very high level of astrometric noise. The distance of UY Scuti has been re-measured by Bailer-Jones et al. in 2021, based on a method that uses the stellar parallax from Gaia EDR3, its color and apparent brightness, giving it a distance of 1,800 pc (5,900 ly). A 2023 measurement using photometry and the Gaia DR3 distance puts the radius at a value of 909 R☉, together with a luminosity of 124,000 L☉ assuming an effective temperature of 3,550 K from an adopted spectral class of M3.5.
Supernova
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 a star 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.