Lesson plan
Lambda Arietis
Lambda Arietis is a double star in the northern constellation of Aries. Its name is a Bayer designation that is Latinized from λ Arietis, and abbreviated Lambda Ari or λ Ari. Based upon an annual parallax shift of 25.32 arcseconds, this system is approximately distant from Earth. The pair have a combined apparent visual magnitude of 4.79, which is bright enough to be viewed with the naked eye. Because the yellow secondary is nearly three magnitudes fainter than the white primary, they are a challenge to split with quality 7× binoculars but are readily resolvable at 10×. The brighter component is an F-type main sequence star with a visual magnitude of 4.95 and a stellar classification of F0 V. It is an estimated 618 million years old with a high rate of rotation, showing a projected rotational velocity of 107 km/s. This star has 1.7 times the mass of the Sun and 2.5 times the Sun's radius. It is radiating 15 times the luminosity of the Sun from its photosphere at an effective temperature of 7,311 K. At an angular separation of 37.4 arcseconds is fainter, magnitude 7.75 companion. This is a G-type main sequence star with a classification of G1 V. The star is at a similar distance as the brighter component, and has a comparable proper motion. In 1988, Helmut Abt listed this as a physical pair, showing a common proper motion with a projected separation of .
Article summary
Lambda Arietis is a double star in the northern constellation of Aries. Its name is a Bayer designation that is Latinized from λ Arietis, and abbreviated Lambda Ari or λ Ari. Based upon an annual parallax shift of 25.32 arcseconds, this system is approximately distant from Earth. The pair have a combined apparent visual magnitude of 4.79, which is bright enough to be viewed with the naked eye. Because the yellow secondary is nearly three magnitudes fainter than the white primary, they are a challenge to split with quality 7× binoculars but are readily resolvable at 10×. The brighter component is an F-type main sequence star with a visual magnitude of 4.95 and a stellar classification of F0 V. It is an estimated 618 million years old with a high rate of rotation, showing a projected rotational velocity of 107 km/s. This star has 1.7 times the mass of the Sun and 2.5 times the Sun's radius. It is radiating 15 times the luminosity of the Sun from its photosphere at an effective temperature of 7,311 K. At an angular separation of 37.4 arcseconds is fainter, magnitude 7.75 companion. This is a G-type main sequence star with a classification of G1 V. The star is at a similar distance as the brighter component, and has a comparable proper motion. In 1988, Helmut Abt listed this as a physical pair, showing a common proper motion with a projected separation of .
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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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Key claims and bibliography are generated from the same tracked claims and sources as the article page.