Iota_Delphini

Iota Delphini

Iota Delphini

A-type giant star in the constellation Delphinus

Iota Delphini (ι Del, ι Delphini) is a star in the constellation Delphinus. It has an apparent magnitude of about 5.4, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Gaia spacecraft, this star is located at a distance of 196 light years.

Quick Facts Constellation, Right ascension ...

Iota Delphini's spectral type is A1IV, meaning it is an A-type subgiant.[14] Observations of the star's spectrum reveal a periodic Doppler shift. This means that Iota Delphini is a spectroscopic binary with a period of 11 days and an eccentricity of 0.23.[7] However, almost no information is known about the companion star.

Iota Delphini appears to be an Am star,[6] also known as a metallic-line star. These types of stars have spectra indicating varying amounts of metals, like iron.[15] Observations of Iota Delphini's spectrum have showed lower amounts of calcium and higher amounts of iron than usual.[6]

References

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    Launhardt, R.; Henning, Th.; Quirrenbach, A.; Ségransan, D.; Avenhaus, H.; Van Boekel, R.; Brems, S. S.; Cheetham, A. C.; Cugno, G.; Girard, J.; Godoy, N.; Kennedy, G. M.; Maire, A. -L.; Metchev, S.; Müller, A.; Musso Barcucci, A.; Olofsson, J.; Pepe, F.; Quanz, S. P.; Queloz, D.; Reffert, S.; Rickman, E. L.; Ruh, H. L.; Samland, M. (2020). "ISPY-NACO Imaging Survey for Planets around Young stars. Survey description and results from the first 2.5 years of observations". Astronomy and Astrophysics. 635: 635. arXiv:2002.01807. Bibcode:2020A&A...635A.162L. doi:10.1051/0004-6361/201937000. S2CID 211032080.
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    "iot Del". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 15 January 2016.
  14. [14]
    Allen, J. S. "The Classification of Stellar Spectra". UCL Department of Physics and Astronomy: Astrophysics Group. Retrieved 1 January 2014.
  15. [15]
    Am star Archived 2017-08-04 at the Wayback Machine, The Internet Encyclopedia of Science, David Darling. Accessed on line August 14, 2008.
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