Lesson plan
V346 Centauri
V346 Centauri is a variable star in the constellation Centaurus. An Algol-type eclipsing binary, its apparent magnitude has a maximum of 8.50, dropping to 8.77 during primary eclipse and to 8.72 during secondary eclipse, the latter being a total eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of about 2300 parsecs (7400 light-years), which is consistent with earlier estimates, based on its luminosity, of 2380 parsecs. The system is a confirmed member of the open cluster Stock 14, which contains many other young OB stars. Both stars in the system are hot B-type stars, with spectral types of B0.5IV and B2V. The primary star shows signs of being evolved, while the secondary is still in the main sequence. In 1936, William O'Leary and Daniel Joseph Kelly O'Connell announced their discovery that the star, then known as CPD−61°2551, is a eclipsing binary star. It was given its variable star designation, V346 Centauri, later that same year. Due to the eclipsing and double-lined nature of the system, the physical elements of the stars can be determined with high precision. The primary star has a mass of 12 times the solar mass, radius of 8.3 times the solar radius, and an effective temperature of about 27,000 K.…
Article summary
V346 Centauri is a variable star in the constellation Centaurus. An Algol-type eclipsing binary, its apparent magnitude has a maximum of 8.50, dropping to 8.77 during primary eclipse and to 8.72 during secondary eclipse, the latter being a total eclipse. From parallax measurements by the Gaia spacecraft, the system is located at a distance of about 2300 parsecs (7400 light-years), which is consistent with earlier estimates, based on its luminosity, of 2380 parsecs. The system is a confirmed member of the open cluster Stock 14, which contains many other young OB stars. Both stars in the system are hot B-type stars, with spectral types of B0.5IV and B2V. The primary star shows signs of being evolved, while the secondary is still in the main sequence. In 1936, William O'Leary and Daniel Joseph Kelly O'Connell announced their discovery that the star, then known as CPD−61°2551, is a eclipsing binary star. It was given its variable star designation, V346 Centauri, later that same year. Due to the eclipsing and double-lined nature of the system, the physical elements of the stars can be determined with high precision. The primary star has a mass of 12 times the solar mass, radius of 8.3 times the solar radius, and an effective temperature of about 27,000 K.…
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Discussion questions
- Summarise the article in your own words. Which single claim would you verify first, and why?
- Which claim in this article is most likely to be revised as the sources update? How would you check its current status?
- If two sources disagreed about one of these facts, what would you need in order to trust one over the other?
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