22 Vulpeculae
star
22 Vulpeculae, also called QS Vulpeculae, is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,490 light-years away, and it has an apparent magnitude of about 5.2, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.
The pair have an orbital period of 249 d in an almost-circular orbit. The primary component is a G-type bright giant. It is over four times as massive as the Sun, and over 96 times as wide. Its companion is a B-type main-sequence star, 3.4 times as massive as the Sun. Although the secondary has an effective temperature of nearly 12,000 K and the primary just 4,700 K, the large size of the cooler star means it is nearly 20 times as luminous at 2,200 L☉. The primary star is rotating slowly with a rotation period that appears to be between about 140 and 165 days, unexpectedly faster than the orbital period. Different parts of its atmosphere may be rotating at different speeds.
The public source identifies “22 Vulpeculae” as star. This brief keeps that definition visible, then builds a research path around Vulpeculae and star.
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This entry incorporates text from “22 Vulpeculae” on English Wikipedia. Contributors are listed in the page history. Text is available under the Creative Commons Attribution-ShareAlike 4.0 License. Selected authority identifiers and statements are retrieved from Wikidata under CC0; their references and qualifiers remain part of the verification path.