Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Scorpius |
Right ascension | 17h 12m 09.19565s [1] |
Declination | –43° 14′ 21.0905″ [1] |
Apparent magnitude (V) | 3.33 [2] |
Characteristics | |
Spectral type | F5 IV [3] |
U−B color index | +0.09 [2] |
B−V color index | +0.41 [2] |
Astrometry | |
Radial velocity (Rv) | –27.0 [4] km/s |
Proper motion (μ) |
RA: +24.47
[1]
mas/
yr Dec.: –288.55 [1] mas/ yr |
Parallax (π) | 44.39 ± 0.16 mas [1] |
Distance | 73.5 ± 0.3
ly (22.53 ± 0.08 pc) |
Absolute magnitude (MV) | +1.58 [5] |
Details [6] | |
Mass | 1.75 [7] M☉ |
Radius | 3.307±0.050 R☉ |
Luminosity | 17.94±0.45 L☉ |
Surface gravity (log g) | 3.65±0.20 cgs |
Temperature | 6,533±46 K |
Metallicity [Fe/H] | −0.29±0.10 dex |
Rotational velocity (v sin i) | 150.00 km/s |
Age | 1.1 [5] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Eta Scorpii, Latinized from η Scorpii, is a star in the southern zodiac constellation of Scorpius. With an apparent visual magnitude of 3.33, [2] this is one of the brighter members of the Scorpius and is the furthest south of the constellation stars with a Bayer designation. [9] The distance to this star can be estimated using parallax measurements, yielding a value of 73.5 light-years (22.5 parsecs) with a 0.4% margin of error. [1]
The stellar classification of this star has undergone some revision over time, with the star being classified anywhere from an F-type main sequence star to a giant star. [8] In 2006, the NStars program assigned it a class of F5 IV, [3] where the luminosity class of 'IV' indicates this is a subgiant star that is exhausting the supply of hydrogen at its core and is in the process of evolving into a giant star. It has around 175% [7] of the Sun's mass with an estimated age of 1.1 billion years. [5] The star is radiating about 18 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 6,533 K. [6] It is this heat that gives it a yellow-white hue that is typical for an F-type star. [10]
Eta Scorpii is rotating rapidly, with a projected rotational velocity of 150 km s−1. [7] This is causing the star to spin on its axis with a period of less than a day. [11] It is an X-ray emitter with its stellar corona giving off an X-ray luminosity of 4.4×1028 ergs s−1. [12] In 1991 it was identified as a possible barium star, as it displays an enhanced abundance of the element barium in its spectrum. [13] Overall, the abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is similar to the abundance in the Sun. [5]