Epoch J2000 Equinox J2000
|Right ascension||15h 15m 30.16295s|
|Declination||+33° 18′ 53.3926″|
|Apparent magnitude (V)||3.482|
|Right ascension||15h 15m 38.34906s|
|Declination||+33° 19′ 15.3161″|
|Apparent magnitude (V)||7.81|
|Spectral type||G8 III + G0 V|
|U−B color index||+0.656/+0.02|
|B−V color index||+0.951/+0.59|
|Radial velocity (Rv)||–12.3 km/s|
|Proper motion (μ)||RA: +84.74 mas/yr
Dec.: –111.58 mas/yr
|Parallax (π)||26.78 ± 0.16 mas|
|Distance||121.8 ± 0.7 ly
(37.3 ± 0.2 pc)
|Absolute magnitude (MV)||+0.700|
|Radial velocity (Rv)||–12.1 km/s|
|Proper motion (μ)||RA: +83.48 mas/yr
Dec.: –110.41 mas/yr
|Parallax (π)||27.05 ± 0.73 mas|
|Distance||121 ± 3 ly
(37.0 ± 1.0 pc)
|Radius||10.5 ± 0.2 R☉|
|Surface gravity (log g)||2.56 cgs|
|Metallicity [Fe/H]||–0.44 dex|
|Rotational velocity (v sin i)||3.6 km/s|
Delta Boötis (δ Boo, δ Boötis) is a double star in the northern constellation Boötes. Based upon parallax measurements, it is located at a distance of approximately 121.8 light-years (37.3 parsecs) from the Earth. This star is sometimes called Princeps, meaning prince or prime in Latin. The origin of this name is unclear, although it usually appears in an astrological context. The It has an apparent visual magnitude of this star is 3.5, making it visible to the naked eye even during a Full Moon.
In Chinese, 七公 (Qī Gōng), meaning Seven Excellencies, refers to an asterism consisting of δ Boötis, 42 Herculis, τ Herculis, φ Herculis, χ Herculis, ν1 Boötis and μ1 Boötis. Consequently, δ Boötis itself is known as 七公七 (Qī Gōng qī, English: the Seventh Star of Seven Excellencies.)
This system consists of a pair of stars located in physical proximity to each other and sharing a similar motion through space, suggesting that they may form a binary star system. Based upon their angular separation and their distance, they have a projected separation of 3,800 Astronomical Units (AU). However, their separation along the line of sight from the Earth remains uncertain, so all that can really be said is that they are separated by at least 3,800 AU. If they are gravitationally bound to each other, it requires a minimum of 120,000 years to complete an orbit.
The brighter member of the pair has a stellar classification of G8 III, indicating that it has exhausted the supply of hydrogen at its core and evolved into a giant star. It now has a radius more than ten times the radius of the Sun. Compared to the Sun, this star appears deficient in elements other than hydrogen and helium—what astronomers term the star's metallicity. The outer envelope of this star has an effective temperature of 4,847 K, which is what gives it the characteristic yellow hue of a G-type star.
The secondary component has a stellar classification of G0 V, which suggests it is a main sequence star that may be similar in physical properties to the Sun. The apparent visual magnitude of this star is 7.81, making it much less luminous than the primary component.
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- The actual brightness ratio is given by 2.512Δm, where Δm is the difference in magnitude. For this pair, Δm = –4.33, so the ratio is 2.512−4.33 = 0.019. Hence the secondary component is 1.9% as bright as the primary.