Kappa Scorpii

κ Scorpii

Template:Location mark Location of κ Sco (circled)
Observation data Epoch J2000      Equinox J2000
Constellation	Scorpius
Right ascension	Template:RA
Declination	Template:DEC
Apparent magnitude (V)	2.41 - 2.42
Characteristics
Spectral type	B1.5 III
U−B Template:Engvar	−0.914
B−V Template:Engvar	−0.228
Variable type	β Cephei
Astrometry
Radial velocity (Rv)	−14.0 km/s
Proper motion (μ)	RA: −6.05 mas/yr Dec.: −25.54 mas/yr
Parallax (π)	6.75±0.17 mas
Distance	Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)	−3.46
Orbit
Period (P)	Template:Val days
Semi-major axis (a)	Template:Val mas
Eccentricity (e)	Template:Val
Inclination (i)	Template:Val°
Longitude of the node (Ω)	Template:Val°
Periastron epoch (T)	Template:Val
Argument of periastron (ω) (secondary)	Template:Val°
Semi-amplitude (K1) (primary)	Template:Val km/s
Details
κ Sco A
Mass	Template:Val Template:Solar mass
Radius	6.8 Template:Solar radius
Luminosity	6,911 Template:Solar luminosity
Surface gravity (log g)	4.01 cgs
Temperature	23,400 K
Rotation	1.90 days
Rotational velocity (v sin i)	105 km/s
Age	Template:Val Myr
κ Sco B
Mass	Template:Val Template:Solar mass
Radius	5.8 Template:Solar radius
Surface gravity (log g)	4.00 cgs
Temperature	18,800 K
Metallicity [Fe/H]	{{{metal_fe2}}} dex
Other designations
Template:Odlist
Database references
SIMBAD	data

Kappa Scorpii, Latinized from κ Scorpii, is a binary star system in the southern constellation of Scorpius. With an apparent visual magnitude of 2.4, this star system is readily visible to the naked eye. Parallax measurements place it at an estimated distance of roughly Template:Convert from the Earth.

Properties

This is a spectroscopic binary, which is a type of binary star system in which the two stars are so close together that they have not been individually resolved with a telescope. The pair orbit each other with a period of about 195 days and an eccentricity of about 0.5. The combined spectrum of this pair matches a star with a stellar classification of B1.5 III. The 'III' luminosity class indicates the presence of a giant star that has exhausted the supply of hydrogen at its core and is in a late evolutionary stage.

File:KappaScoLightCurve.png

A light curve for Kappa Scorpii, adapted from Lomb and Shobbrook (1975)

The primary component of the pair, κ Sco A, is a variable star of Beta Cephei type. It is undergoing radial pulsations with a dominant frequency of 4.99922 cycles per day, or 4.8 hours per cycle. There are overlapping secondary pulsation frequencies of about 4.85 and 5.69 cycles per day. This star has about 11 times the mass of the Sun and is nearly 7 times the Sun's radius. The effective temperature of the outer envelope is 23,400 K, giving it a blue-white hue. It is rotating rapidly, with an estimated period of only 1.9 days and an axis of rotation that is inclined by about 40° to the line of sight from the Earth.

The secondary component, κ Sco B, is smaller than the primary, but still much larger than the Sun. It has about 10 times the mass of the Sun and nearly six times the Sun's radius. The effective temperature of 18,800 K is also higher than the Sun's, which is at 5,778 K.

Traditional name

κ Scorpii has been called Girtab Template:IPAc-en, which is the Sumerian word for 'scorpion'. The name has survived through the Babylonian star catalogues, and was originally applied to an asterism comprising this star, Lambda Scorpii, Upsilon Scorpii, and Iota Scorpii.

In Chinese, (), meaning Tail, refers to an asterism consisting κ Scorpii, μ¹ Scorpii, ε Scorpii, ζ¹ Scorpii and ζ² Scorpii, η Scorpii, θ Scorpii, ι¹ Scorpii and ι² Scorpii, λ Scorpii and υ Scorpii. Consequently, the Chinese name for κ Scorpii itself is (), "the Seventh Star of Tail".

Modern legacy

κ Scorpii appears on the flag of Brazil, symbolising the state of Paraíba.