Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Capricornus |
Right ascension | 20h 27m 19.21088s [1] |
Declination | −18° 12′ 42.1980″ [1] |
Apparent magnitude (V) | +5.096 [2] |
Characteristics | |
Spectral type | B8 II-III [3] or B3-5 V [4] |
U−B color index | −0.311 [2] |
B−V color index | +0.013 [2] |
Astrometry | |
Radial velocity (Rv) | −13 [5] km/s |
Proper motion (μ) |
RA: +16.914
[6]
mas/
yr Dec.: −16.983 [6] mas/ yr |
Parallax (π) | 4.9614 ± 0.3495 mas [6] |
Distance | 660 ± 50
ly (200 ± 10 pc) |
Absolute magnitude (MV) | −1.01 [7] |
Details | |
π Cap Aa | |
Mass | 5.9±0.1 [8] M☉ |
Luminosity | 238 [9] L☉ |
Temperature | 9,623 [9] K |
Rotational velocity (v sin i) | 30 [10] km/s |
Age | 43.4±7.8 [8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Pi Capricorni, Latinized from π Capricorni, is a triple star system in the southern constellation of Capricornus. It has the traditional star name Okul[ citation needed] or Oculus (meaning eye in Latin). [12] This system appears blue-white in hue and is visible to the naked eye as a 5th magnitude star. [2] It is located approximately 660 light years distant from the Sun based on parallax, [6] but is drifting closer with a radial velocity of −13 km/s. [5]
In Chinese, 牛宿 (Niú Su), meaning Ox (asterism), refers to an asterism consisting of π Capricorni, β Capricorni, α2 Capricorni, ξ2 Capricorni, ο Capricorni and ρ Capricorni. [13] Consequently, the Chinese name for π Capricorni itself is 牛宿四 (Niú Su sì, English: the Fourth Star of Ox.) [14]
The primary member, component A, is a spectroscopic binary whose two components are separated by 0.1 arcseconds. The brighter of the two, component Aa, is a blue-white B-type bright giant or main sequence star with an apparent magnitude of +5.08. It is around 43 million years old with six times the mass of the Sun. [8] The star is radiating 238 times the Sun's luminosity from its photosphere at an effective temperature of 9,623 K. [9] The third member, component B, is an eighth magnitude star at an angular separation of 3.4 ″ from the primary. [15]
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cite web}}
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Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Capricornus |
Right ascension | 20h 27m 19.21088s [1] |
Declination | −18° 12′ 42.1980″ [1] |
Apparent magnitude (V) | +5.096 [2] |
Characteristics | |
Spectral type | B8 II-III [3] or B3-5 V [4] |
U−B color index | −0.311 [2] |
B−V color index | +0.013 [2] |
Astrometry | |
Radial velocity (Rv) | −13 [5] km/s |
Proper motion (μ) |
RA: +16.914
[6]
mas/
yr Dec.: −16.983 [6] mas/ yr |
Parallax (π) | 4.9614 ± 0.3495 mas [6] |
Distance | 660 ± 50
ly (200 ± 10 pc) |
Absolute magnitude (MV) | −1.01 [7] |
Details | |
π Cap Aa | |
Mass | 5.9±0.1 [8] M☉ |
Luminosity | 238 [9] L☉ |
Temperature | 9,623 [9] K |
Rotational velocity (v sin i) | 30 [10] km/s |
Age | 43.4±7.8 [8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Pi Capricorni, Latinized from π Capricorni, is a triple star system in the southern constellation of Capricornus. It has the traditional star name Okul[ citation needed] or Oculus (meaning eye in Latin). [12] This system appears blue-white in hue and is visible to the naked eye as a 5th magnitude star. [2] It is located approximately 660 light years distant from the Sun based on parallax, [6] but is drifting closer with a radial velocity of −13 km/s. [5]
In Chinese, 牛宿 (Niú Su), meaning Ox (asterism), refers to an asterism consisting of π Capricorni, β Capricorni, α2 Capricorni, ξ2 Capricorni, ο Capricorni and ρ Capricorni. [13] Consequently, the Chinese name for π Capricorni itself is 牛宿四 (Niú Su sì, English: the Fourth Star of Ox.) [14]
The primary member, component A, is a spectroscopic binary whose two components are separated by 0.1 arcseconds. The brighter of the two, component Aa, is a blue-white B-type bright giant or main sequence star with an apparent magnitude of +5.08. It is around 43 million years old with six times the mass of the Sun. [8] The star is radiating 238 times the Sun's luminosity from its photosphere at an effective temperature of 9,623 K. [9] The third member, component B, is an eighth magnitude star at an angular separation of 3.4 ″ from the primary. [15]
{{
cite web}}
: CS1 maint: postscript (
link)