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Iota Serpentis

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Star in the constellation Serpens
Iota Serpentis
Location of ι Serpentis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 15 41 33.05469
Declination 19° 40′ 13.4380″
Apparent magnitude (V) 4.51
Characteristics
Evolutionary stage main sequence
Spectral type B9V + A1V
B−V color index +0.062±0.003
Astrometry
Radial velocity (Rv)−17.20 km/s
Proper motion (μ) RA: -60.86 mas/yr
Dec.: -43.69 mas/yr
Parallax (π)17.16 ± 0.67 mas
Distance190 ± 7 ly
(58 ± 2 pc)
Absolute magnitude (MV)+0.69
Orbit
Period (P)8015.0±6.3 d
Semi-major axis (a)0.21033±0.00047″
Eccentricity (e)0.0941±0.0028
Inclination (i)83.608±0.043°
Longitude of the node (Ω)69.684±0.033°
Periastron epoch (T)54,180±33 HMJD
Argument of periastron (ω)
(secondary)
80.5±1.8°
Details
A
Mass1.999 M
B
Mass1.984 M
Other designations
ι Ser, 21 Serpentis, BD+20° 3138, GC 21102, HD 140159, HIP 76852, HR 5842, SAO 101682, ADS 9744, CCDM J15416+1940
Database references
SIMBADdata

ι Serpentis, Latinized as Iota Serpentis and abbreviated Iot Ser, is a triple star system in the constellation Serpens, in its head (Serpens Caput). It is approximately 190 light years from Earth.

At the centre of the system is a spectroscopic binary, Iota Serpentis A and B. These are both white main sequence dwarfs and both have apparent magnitudes of +5.3. This binary has an orbital period variously reported as 11 or 22 years. First discovered as an astrometric binary, the pair have now been resolved and visual orbits have been derived.

There are two visual companions, Iota Serpentis C, a 13th magnitude star 143 arcseconds away and Iota Serpentis D, a 12th magnitude star 151 arcseconds distant.

References

  1. ^ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Vizier catalog entry
  2. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ Martin, C.; et al. (1998). "Mass determination of astrometric binaries with Hipparcos. III. New results for 28 systems". Astronomy and Astrophysics Supplement. 133 (2): 149. Bibcode:1998A&AS..133..149M. doi:10.1051/aas:1998459.
  4. Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  5. ^ Muterspaugh, Matthew W.; et al. (2010). "The Phases Differential Astrometry Data Archive. II. Updated Binary Star Orbits and a Long Period Eclipsing Binary". The Astronomical Journal. 140 (6): 1623–1630. arXiv:1010.4043. Bibcode:2010AJ....140.1623M. doi:10.1088/0004-6256/140/6/1623. S2CID 6030289.
  6. "iot Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-09.
  7. Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  8. van den Bos, W. H. (1965). "Note on the Double Star Iota Serpentis". Monthly Notes of the Astronomical Society of Southern Africa. 24: 123. Bibcode:1965MNSSA..24..123V.
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