Iota Serpentis
| 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 | |
| Spectral type | A1V + A1V [2] |
| B−V color index | +0.06 [2] |
| Astrometry | |
| Radial velocity (Rv) | -17.20[3] km/s |
| Proper motion (μ) | RA: -60.86[1] mas/yr Dec.: -43.69[1] mas/yr |
| Parallax (π) | 17.16 ± 0.67[1] mas |
| Distance | 190 ± 7 ly (58 ± 2 pc) |
| Absolute magnitude (MV) | 0.68 [4] |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Serpentis (ι Ser, ι Serpentis) is a star system in the constellation Serpens, in its head (Serpens Caput). It is approximately 190 light years from Earth.[1]
At the centre of the system is a spectroscopic binary, Iota Serpentis A and B. These are both white A-type main sequence dwarfs and both have apparent magnitudes of +5.3. This binary has an orbital period variously reported as 11[5] or 22[6] years; spectroscopic evidence indicates a third companion of A and B. A and B also have two distant companions, Iota Serpentis C, a 13th magnitude star 143 arcseconds away and Iota Serpentis D, a 12th magnitude star 151 arcseconds distant.
References
- 1 2 3 4 5 6 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. Vizier catalog entry - 1 2 3 4 "Iota Serpentis". SIMBAD Astronomical Database. Retrieved 2015-10-17.
- ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
- ↑ Absolute magnitude calculated as , where is the star's absolute magnitude, is the star's apparent magnitude, and is the star's measured parallax in arcseconds.
- ↑ 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.
- ↑ 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.
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