Luhman 16
| Observation data Epoch J2016.0 Equinox J2016.0 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10h 49m 18.771s |
| Declination | −53° 19′ 09.88″ |
| Apparent magnitude (V) | 16.20 |
| Characteristics | |
| Spectral type | A: L7.5 B: T0.5±1 |
| Apparent magnitude (i (DENIS filter system)) | 14.94±0.03 |
| Apparent magnitude (J (2MASS filter system)) | 10.73±0.03 |
| Apparent magnitude (J (DENIS filter system)) | 10.68±0.05 |
| Apparent magnitude (H (2MASS filter system)) | 9.56±0.03 |
| Apparent magnitude (KS (2MASS filter system)) | 8.84±0.02 |
| Apparent magnitude (KS (DENIS filter system)) | 8.87±0.08 |
| Astrometry | |
| Proper motion (μ) | RA: −2,768.511 mas/yr Dec.: +358.472 mas/yr |
| Parallax (π) | 500.993±0.050 mas |
| Distance | 6.5102 ± 0.0006 ly (1.9960 ± 0.0002 pc) |
| Orbit | |
| Period (P) | 26.55±0.08 yr |
| Semi-major axis (a) | 1.764±0.003" (3.52 AU) |
| Eccentricity (e) | 0.344±0.001 |
| Inclination (i) | 79.92±0.008° |
| Longitude of the node (Ω) | 130.02±0.01° |
| Periastron epoch (T) | 2018.060±0.003 |
| Argument of periastron (ω) (secondary) | 136.67±0.09° |
| Details | |
| Luhman 16A | |
| Mass | 35.4±0.2 MJup |
| Radius | 0.102±0.005 R☉ |
| Luminosity | (2.2±0.4)×10−5 L☉ |
| Temperature | 1305+180 −135 K |
| Rotation | 6.94 hours |
| Age | 400–800 or 510±95 Myr |
| Luhman 16B | |
| Mass | 29.4±0.2 MJup |
| Radius | 0.102±0.005 R☉ |
| Luminosity | 2.1+0.7 −0.5×10−5 L☉ |
| Temperature | 1320+185 −135 K |
| Rotation | 5.28 hours |
| Age | 400–800 or 510±95 Myr |
| Other designations | |
| LUH 16, Luhman–WISE 1, WISE J104915.57−531906.1, DENIS-P J104919.0−531910, 2MASS J10491891−5319100, IRAS Z10473-5303, AKARI J1049166−531907, GSC2.2 S11132026703, GSC2.3 S4BM006703, TIC 119862115, GJ 11551 | |
| Database references | |
| SIMBAD | The system |
| A | |
| B | |
| Exoplanet Archive | data |
Luhman 16 (also designated WISE 1049−5319 or WISE J104915.57−531906.1) is a binary brown-dwarf system in the southern constellation Vela at a distance of 6.51 light-years (2.00 parsecs) from the Sun. These are the closest-known brown dwarfs and the closest system found since the measurement of the proper motion of Barnard's Star in 1916, and the third-closest-known system to the Sun (after the Alpha Centauri system and Barnard's Star). The primary is of spectral type L7.5 and the secondary of type T0.5±1 (and is hence near the L–T transition). The masses of Luhman 16 A and B are 35.4 and 29.4 Jupiter masses, respectively, and their ages are estimated to be 400–800 million years. Luhman 16 A and B orbit each other at a distance of about 3.5 astronomical units with an orbital period of approximately 26.6 years.