Observation data Epoch J2000.0 Equinox | |
---|---|
Constellation | Leo |
54 Leo A | |
Right ascension | 10h 55m 36.80266s [1] |
Declination | +24° 44′ 59.0440″ [1] |
Apparent magnitude (V) | 4.477 [2] |
54 Leo B | |
Right ascension | 10h 55m 37.24836s [3] |
Declination | +24° 44′ 56.5478″ [3] |
Apparent magnitude (V) | 6.29 [4] |
Characteristics | |
54 Leo A | |
Spectral type | A0 V [5] |
B−V color index | +0.001 [5] |
54 Leo B | |
Spectral type | A2 Vn [5] |
B−V color index | +0.07 [4] |
Astrometry | |
54 Leo A | |
Radial velocity (Rv) | −0.49±0.98 [6] km/s |
Proper motion (μ) |
RA: −78.057
[1]
mas/
yr Dec.: −16.520 [1] mas/ yr |
Parallax (π) | 9.8275 ± 0.3537 mas [1] |
Distance | 330 ± 10
ly (102 ± 4 pc) |
Absolute magnitude (MV) | –0.29 [7] |
54 Leo B | |
Radial velocity (Rv) | 1.30±0.92 [6] km/s |
Proper motion (μ) |
RA: −75.374
[3]
mas/
yr Dec.: −18.595 [3] mas/ yr |
Parallax (π) | 10.1748 ± 0.0569 mas [3] |
Distance | 321 ± 2
ly (98.3 ± 0.5 pc) |
Details | |
54 Leo A | |
Mass | 2.4+0.44 −0.36 [8] M☉ |
Radius | 2.88 [9] R☉ |
Surface gravity (log g) | 3.5±0.25 [8] cgs |
Temperature | 9000±500 [8] K |
Rotational velocity (v sin i) | 185 [10] km/s |
Age | 411+137 −168 [8] Myr |
54 Leo B | |
Radius | 2.59 [9] R☉ |
Rotational velocity (v sin i) | 250±20 [9] km/s |
Other designations | |
54 Leo, BD+25 2314, CCDM J10556+2445, HIP 53417, Struve 1487
[11] | |
54 Leo A: HD 94601, HR 4259, SAO 81583 | |
54 Leo B: HD 94602, HR 4260, SAO 81584 | |
Database references | |
SIMBAD | data |
54 Leonis is a binary star [12] system in the zodiac constellation of Leo, located around 321 [3] light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.30. [13] As of 2017, the pair had an angular separation of 6.60 ″ along a position angle of 113°. [14] They have a physical separation of around 533 AU (79,700 Gm). [9]
The magnitude 4.477 [2] primary, designated component A, is an A-type main-sequence star with a stellar classification of A0 V, [5] which indicates it is generating energy through hydrogen fusion at its core. It has a high rate of spin, showing a projected rotational velocity of 185 km/s. This is giving the star an oblate shape with an equatorial bulge that is an estimated 8% larger than the polar radius. [10] The star is roughly 411 [8] million years old with 2.4 [8] times the mass of the Sun and about 2.88 [9] times the Sun's radius.
The fainter magnitude 6.29 [4] secondary, component B, is a smaller A-type main-sequence star with a class of A2 Vn. [5] The 'n' suffix indicates wide "nebulous" lines due to rapid rotation. It is spinning with an even higher projected rotational velocity of 250 [9] km/s. The star has about 2.59 [9] times the Sun's radius.
Asteroid 729 Watsonia occulted HIP 53417 on March 3, 2013 at 01:48. [15]