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ι Serpentis, Latinized as Iota Serpentis and abbreviated Iot Ser, is a triple star[7] system in the constellation Serpens, in its head (Serpens Caput). It is approximately 190 light years from Earth.[1]

Iota Serpentis
Location of ι Serpentis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 15h 41m 33.05469s[1]
Declination 19° 40′ 13.4380″[1]
Apparent magnitude (V) 4.51[2]
Characteristics
Evolutionary stage main sequence
Spectral type B9V + A1V[3]
B−V color index +0.062±0.003[2]
Astrometry
Radial velocity (Rv)−17.20[4] km/s
Proper motion (μ) RA: -60.86[1] mas/yr
Dec.: -43.69[1] mas/yr
Parallax (π)17.16 ± 0.67 mas[1]
Distance190 ± 7 ly
(58 ± 2 pc)
Absolute magnitude (MV)+0.69[2]
Orbit[5]
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[3] M☉
B
Mass1.984[3] 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[6]
Database references
SIMBADdata

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[8] or 22[5] years. First discovered as an astrometric binary, the pair have now been resolved and visual orbits have been derived.[5]

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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