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