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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | 11h 23m 55.45273s[1] |
| Declination | +10° 31′ 46.2195″[1] |
| Apparent magnitude (V) | 4.00[2] |
| Characteristics | |
| Spectral type | F4 IV[3] |
| U−B color index | +1.420[4] |
| B−V color index | +0.456[4] |
| Variable type | Suspected[5] |
| Astrometry | |
| Radial velocity (Rv) | −10.3[6] km/s |
| Proper motion (μ) | RA: +141.45[1] mas/yr Dec.: −79.14[1] mas/yr |
| Parallax (π) | 41.26 ± 1.16 mas[1] |
| Distance | 79 ± 2 ly (24.2 ± 0.7 pc) |
| Absolute magnitude (MV) | +2.13[7] |
| Orbit[8] | |
| Primary | ι Leo A |
| Companion | ι Leo B |
| Period (P) | 186 yr |
| Semi-major axis (a) | 1.91″ |
| Eccentricity (e) | 0.53 |
| Inclination (i) | 128° |
| Longitude of the node (Ω) | 235° |
| Periastron epoch (T) | B 1948.8 |
| Argument of periastron (ω) (secondary) | 325° |
| Details | |
| Mass | 1.62−1.70[3] M☉ |
| Radius | 2.1[9] R☉ |
| Luminosity | 11.5[3] L☉ |
| Surface gravity (log g) | 3.98[10] cgs |
| Temperature | 6,739[10] K |
| Metallicity [Fe/H] | 0.06[10] dex |
| Rotational velocity (v sin i) | 16[3] km/s |
| Age | 1.7[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Leonis, Latinized from ι Leonis, is a triple star system in the constellation Leo. The system is fairly close to the Sun, at only 79 light-years (24.2 parsecs) away, based on its parallax.[1] The system has a combined apparent magnitude of 4.00[2] making it faintly visible to the naked eye. It is moving closer to the Sun with a radial velocity of −10 km/s.[6]
Iota Leonis has a spectral type of F3 IV,[3] matching that of an F-type subgiant star. It is a spectroscopic binary, which means it is a binary star with components that are too close together to be able to resolve individually through a telescope. In this case, light from only the primary star can be detected, and it is considered single-lined.[3]
The third component in the star system is designated Iota Leonis B. It orbits the central pair almost every 200 years, and with its perihelion passage in 1948, the separation between the two is steadily growing.[12] Iota Leonis B has a mass approximately 8% greater than that of the Sun.[12] It is a G-type main-sequence star, like the Sun.[13]
- ^ a b c d e f Cite error: The named reference
aaa474_2_653was invoked but never defined (see the help page). - ^ a b c Cite error: The named reference
SIMBADwas invoked but never defined (see the help page). - ^ a b c d e f g Cite error: The named reference
apj673_2was invoked but never defined (see the help page). - ^ a b Cite error: The named reference
aass26was invoked but never defined (see the help page). - ^ Cite error: The named reference
kukarin81was invoked but never defined (see the help page). - ^ a b Cite error: The named reference
gcsrvwas invoked but never defined (see the help page). - ^ Cite error: The named reference
Anderson2012was invoked but never defined (see the help page). - ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 1 August 2017. Retrieved 13 May 2017.
- ^ Cite error: The named reference
aass85_3_1015was invoked but never defined (see the help page). - ^ a b c Cite error: The named reference
apj354was invoked but never defined (see the help page). - ^ Cite error: The named reference
CNS5was invoked but never defined (see the help page). - ^ a b Fuhrmann, Klaus (2008). "Nearby stars of the Galactic disc and halo - IV". Monthly Notices of the Royal Astronomical Society. 384 (1): 173–224. Bibcode:2008MNRAS.384..173F. doi:10.1111/j.1365-2966.2007.12671.x.
- ^ "BD+11 2348B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 9 May 2017.