This holiday season, we received an incredible surprise from our StellarNet team—a star named in our honor!
The star is located in the Andromeda constellation, close to the Pegasus constellation. Its coordinates, RA/DEC: 00H 49M 48.8S +41° 04′ 44.2, place it near the Andromeda Galaxy (M31). This region of the sky is notable for its proximity to one of the most easily observed spiral galaxies and offers year-round visibility from many locations in the northern hemisphere. The star lies near the celestial equator, making it accessible for viewing from both hemispheres.
What is Stellar Classification?
Stellar classification organizes stars based on their spectra, which are analyzed by splitting their light into a spectrum to identify chemical elements through spectral lines. These lines, influenced mainly by the temperature of the star’s photosphere, also reveal elemental abundances.
The Morgan–Keenan (MK) system classifies stars into types O, B, A, F, G, K, and M, from hottest to coolest, with subdivisions (e.g., A0 to A9). Additional classes, such as W, S, C, D, L, T, and Y, account for less common objects like white and brown dwarfs.
Luminosity classes, indicated by Roman numerals (e.g., I for supergiants, V for main-sequence stars), describe a star’s size and brightness. The Sun, classified as G2V, is a main-sequence star with a surface temperature of about 5,800 K. This system provides a concise way to describe a star’s temperature, size, and composition.
A simple chart for classifying the main star types using Harvard classification.
What Classification is Our Star?
Our star is classified as a B5V spectral type, a blue-white main-sequence star. The “B5” designation indicates it falls within the B spectral type, placing it among stars with high surface temperatures ranging from approximately 10,000 to 15,000 K. The “5” further refines its position within the B-class, making it slightly cooler than a B0 star but still extremely hot and luminous compared to stars like our Sun.
The “V” in its classification specifies that it is a main-sequence star, meaning it is actively fusing hydrogen into helium in its core. This is the most stable phase in a star’s life cycle. Stars like this emit strong ultraviolet radiation and shine with a brilliance hundreds of times greater than the Sun, contributing to their striking blue-white appearance.
Given its classification, our B5V star is young and energetic, likely a few tens of millions of years old. It represents a significant step up in temperature, mass, and luminosity compared to a G-class star like the Sun, making it an impressive and dynamic celestial object to observe and study.
Thank You!
A huge thank you to our incredible team for an amazing year! We’re thrilled to have our very own StellarNet Star to look up to and celebrate in the years ahead. Join us as we continue to track its journey across the night sky!
