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Iota Aquarii
B-type main sequence star in the constellation Aquarius From Wikipedia, the free encyclopedia
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Iota Aquarii is a binary star[7] system in the equatorial constellation of Aquarius. Its identifier is a Bayer designation that is Latinised from ι Aquarii, and abbreviated Iota Aqr or ι Aqr, respectively. This star is visible to the naked eye with an apparent magnitude of +4.279.[3] Based upon parallax measurements, the distance to this star is around 211 light-years (65 parsecs).[2] The system is drifting closer to the Sun with a radial velocity of −10 km/s.[6]
The binary nature of this system was reported in 2009 following a radial velocity survey using the HARPS instrument.[5] A 2010 infrared search for companions around this star was unsuccessful.[12] The presence of a stellar companion was confirmed through direct spectral detection in 2016. The companion shows a significant velocity variation over a 77-day interval, suggesting a short orbital period.[7]
The spectrum of the primary, component A, fits a stellar classification of B8 V,[4] showing that this is a B-type main-sequence star. It is roughly 124[7] million years old and is spinning rapidly with a projected rotational velocity of 135 km/s.[10] The star has 3.2[7] times the mass of the Sun and 2.7[8] times the Sun's radius. It is radiating 74[1] times the luminosity of the Sun from its photosphere at an effective temperature of ~11,284 K.[8] The secondary, component B, has a spectrum of a solar-mass star.[7] The system is a source for X-ray emission.[13]
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