Matches in DBpedia 2016-04 for { ?s ?p "Iota Pegasi (24 Peg, HD 210027) is a star located within the constellation Pegasus. It is about 38 light-years from Earth. It is a spectroscopic binary system.Iota Pegasi A is a yellowish-white star somewhat brighter than the sun. It and the dimmer Iota Pegasi B orbit each other with a period of about 10 days. In about four billion years from now, component A will evolve off the main sequence into a giant. In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years."@en }
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- Iota_Pegasi abstract "Iota Pegasi (24 Peg, HD 210027) is a star located within the constellation Pegasus. It is about 38 light-years from Earth. It is a spectroscopic binary system.Iota Pegasi A is a yellowish-white star somewhat brighter than the sun. It and the dimmer Iota Pegasi B orbit each other with a period of about 10 days. In about four billion years from now, component A will evolve off the main sequence into a giant. In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years.".
- Q1367410 abstract "Iota Pegasi (24 Peg, HD 210027) is a star located within the constellation Pegasus. It is about 38 light-years from Earth. It is a spectroscopic binary system.Iota Pegasi A is a yellowish-white star somewhat brighter than the sun. It and the dimmer Iota Pegasi B orbit each other with a period of about 10 days. In about four billion years from now, component A will evolve off the main sequence into a giant. In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years.".