Source: wikipedia https://en.wikipedia.org/wiki/HD_143699
S P A C E | ‘HD 143699’
I will email about this, for members of S P A C E.
Cool.
Observation data Epoch J2000 Equinox J2000 |
|
---|---|
Constellation | Lupus |
Right ascension | 16h 03m 24.18956s[1] |
Declination | −38° 36′ 09.1424″[1] |
Apparent magnitude (V) | 4.90[2] |
Characteristics | |
Spectral type | B5/7 III/IV[3] |
B−V color index | −0.146±0.043[2] |
Astrometry | |
Radial velocity (Rv) | −1.9±2.8[2] km/s |
Proper motion (μ) | RA: −18.488[1] mas/yr Dec.: −28.147[1] mas/yr |
Parallax (π) | 9.2268 ± 0.4693 mas[1] |
Distance | 350 ± 20 ly (108 ± 6 pc) |
Absolute magnitude (MV) | −0.54[2] |
Details | |
Mass | 4.31±0.07[4] M☉ |
Radius | 4.4[5] R☉ |
Luminosity | 438+39 −36[4] L☉ |
Temperature | 14521+202 −401[4] K |
Rotational velocity(v sin i) | 123[4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 143699 is a single[7] star in the southern constellation of Lupus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.90.[2] Based upon an annual parallax shift of 9.2 mas,[1] it is located around 350 light years away. It is most likely (90%[8] chance) a member of the Upper Centaurus–Lupus[9] subgroup of the Sco OB2moving group.
This star has a stellar classification of B5/7 III/IV,[3] suggesting it is an evolving star that is entering the giant stage. However, according to Zorec and Royer (2012) it is only 56% of the way through its main sequence lifespan.[4] It is a chemically peculiar magnetic B star,[10] showing an averaged quadratic field strength of (167.2±140.4)×10−3 T.[11]Helium-weak, it displays an underabundance of helium in its spectrum.[12] Radio emissions have been detected from this source.[10]
HD 143699 has 4.3[4] times the mass of the Sun and 4.4[5] times the Sun’s radius. It has a high rate of spin with a projected rotational velocity of 123 km/s.[4] The star is radiating 438[4] times the Sun’s luminosity from its photosphere at an effective temperature of 14,521 K.[4]