CHAPTER: Epsilon Pegasi was completed!

  Epsilon Pegasi is a K2 Ib supergiant star located in the constellation Pegasus. As a K-type star, it exhibits a surface temperature of approximately 4,000 to 4,300 Kelvin, producing a distinct orange hue due to its cooler photosphere. Its spectral classification denotes a massive star that has evolved off the main sequence and is currently in the supergiant phase, characterized by a significantly expanded radius and high luminosity.

  With an apparent magnitude of around 2.4, Epsilon Pegasi is one of the brightest stars in its constellation. Parallax measurements place it at an approximate distance of 210 parsecs (or about 685 light-years) from Earth. Its luminosity is estimated to be around 5,000 times that of the Sun, though values vary depending on measurement methods and assumptions regarding interstellar extinction.

  Epsilon Pegasi has a relatively slow rotational velocity compared to main sequence stars, typical of evolved supergiants. It has also exhibited evidence of low-amplitude variability, suggesting pulsations common in massive evolved stars. The stellar atmosphere is characterized by broadened absorption lines and strong metallic features, consistent with its temperature and size.

  This star is in a late evolutionary stage, likely burning helium or heavier elements in its core or shells, having exhausted hydrogen in its core. Its future evolution may lead to further instability, potentially resulting in mass loss through stellar winds or eventual transition into a type II supernova, depending on its initial mass. Epsilon Pegasi provides a significant observational benchmark for understanding late-stage stellar evolution in intermediate- to high-mass stars.

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  CHAPTER: Alpha Leonis is coming soon!

  Alpha Leonis is a B7 V main-sequence star located in the constellation Leo. It is a spectroscopic binary system, with the primary component being a rapidly rotating B-type star exhibiting a projected rotational velocity of approximately 300 km/s. This extreme rotational velocity leads to significant equatorial bulging due to centrifugal force, resulting in an oblate stellar shape. The star’s equatorial radius is estimated to be about 32% greater than its polar radius.

  With an effective surface temperature around 12,000 Kelvin, Alpha Leonis emits a bluish-white light, consistent with its spectral classification. The rapid rotation also causes gravitational darkening, where the equator appears dimmer and cooler than the poles due to variation in surface gravity and temperature. Its luminosity is estimated to be approximately 350 times that of the Sun, though this value is influenced by viewing angle and rotational effects.

  Alpha Leonis lies at an approximate distance of 24.3 parsecs (79 light-years) from Earth, determined through astrometric parallax. It is part of a binary system with a lower-mass companion, likely a late-type main-sequence star, which has an orbital period of around 40 days. The companion is not visible in direct imaging due to the brightness of the primary, but its presence is confirmed via Doppler shift analysis of the primary’s spectral lines.

  As a massive, high-temperature star, Alpha Leonis has a relatively short main-sequence lifespan compared to solar-type stars. Its evolutionary trajectory will likely involve expansion into a giant phase, possibly culminating in a collapse into a white dwarf, depending on its mass loss and binary interactions.