Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Lepus |
Right ascension | 05h 12m 17.90190s[2] |
Declination | −11° 52′ 09.1863″[2] |
Apparent magnitude (V) | 4.45[3] |
Characteristics | |
Spectral type | B7.5 Vn[4] + K7.2 XR? + G8 Ve[5] |
U−B color index | −0.40[3] |
B−V color index | −0.10[3] |
Astrometry | |
Radial velocity (Rv) | +23.50[6] km/s |
Proper motion (μ) | RA: +24.39[2] mas/yr Dec.: −31.02[2] mas/yr |
Parallax (π) | 14.07 ± 0.16 mas[2] |
Distance | 232 ± 3 ly (71.1 ± 0.8 pc) |
Absolute magnitude (MV) | 0.01[7] |
Details | |
ι Lep A | |
Mass | 3.37±0.02[8] M☉ |
Luminosity | 153[8] L☉ |
Surface gravity (log g) | 4.25[9] cgs |
Temperature | 13,781±469[9] K |
Rotational velocity (v sin i) | 185[9] km/s |
Age | 94[7] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Iota Leporis (ι Leporis) is a triple star[5] system in the southern constellation of Lepus. It is visible to the naked eye as a point source of blue-white light with an apparent visual magnitude of 4.45.[3] Based upon an annual parallax shift of 14.07 mas as measured from Earth,[2] the system is located roughly 232 light years from the Sun.
The primary, designated component A, is a B-type main-sequence star with a stellar classification of B7.5 Vn,[4] where the 'n' suffix indicates "nebulous" absorption lines caused by rotation. It is about 94[7] million years old and has a high rate of spin with a projected rotational velocity of 185 km/s.[9] With an estimated 3.4[8] times the mass of the Sun, it is radiating 153[8] times the Sun's luminosity from its photosphere at an effective temperature of around 13,781 K.[9]
There is a close companion that is a source of X-ray emission. Most likely this star has at least 1.05 times the mass of the Sun.[7] The third component, AM Leporis, is a BY Draconis variable[11] of apparent magnitude 9.92,[3] and spectral type G8Ve[12] at an angular separation of 12.7".[13]
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