Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Cetus |
Right ascension | 02h 12m 59.99769s [1] |
Declination | +08° 50′ 48.2023″ [1] |
Apparent magnitude (V) | +4.36 [2] [combined] |
Characteristics | |
Spectral type | G7III Ba0.4 Fe-1 [3] + DA4 [4] |
B−V color index | 0.878±0.024 [2] |
Astrometry | |
Radial velocity (Rv) | −3.93±0.09 [2] km/s |
Proper motion (μ) |
RA: −24.498
[1]
mas/
yr Dec.: −5.952 [1] mas/ yr |
Parallax (π) | 9.5451 ± 0.3275 mas [1] |
Distance | 340 ± 10
ly (105 ± 4 pc) |
Absolute magnitude (MV) | –0.99 [5] |
Orbit [6] | |
Period (P) | 1,642.1±1.3 |
Semi-major axis (a) | ≥ 0.896 ± 0.020 AU (134 ± 3 Gm) |
Eccentricity (e) | 0 (fixed) |
Periastron epoch (T) | 34,985±5 MJD |
Semi-amplitude (K1) (primary) | 5.91±0.14 km/s |
Details | |
A | |
Mass | 3.80 [5] M☉ |
Radius | 18.2+1.0 −2.4 [1] R☉ |
Luminosity | 209.9±8.2 [1] L☉ |
Surface gravity (log g) | 2.60 [1] cgs |
Temperature | 5,184±50 [5] K |
Metallicity [Fe/H] | −0.01 [5] dex |
Age | 100 [7] Myr |
B | |
Mass | 0.8 [5] M☉ |
Surface gravity (log g) | 8.4 [8] cgs |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Xi1 Ceti , Latinized from ξ1 Ceti, is a binary star [10] system located in the equatorial constellation of Cetus. It is visible to the naked eye with a combined apparent visual magnitude of +4.36. [2] The distance to this system is approximately 340 light years based on parallax measurements, and it is drifting closer to the Sun with a radial velocity of −4 km/s. [2] The proximity of the star to the ecliptic means it is subject to lunar occultations. [11]
The spectroscopic binary nature of Xi1 Ceti was discovered in 1901 by William Wallace Campbell using the Mills spectrograph at the Lick Observatory. [12] [6] The pair have a circular orbit with a period of 4.5 years and a separation of 3.8 AU. [5] It is a suspected eclipsing binary with an amplitude of 0.03 in magnitude, which would suggest the orbital plane has a high inclination. [13]
The primary, designated component A, is a mild barium [14] giant star with a stellar classification of G7III Ba0.4 Fe-1. [3] Morgan and Keenan in 1973 had classified it as a bright giant star with an anomalous underabundance of the CN molecule. [15] Evidence has been found for an overabundance of s-process elements, [5] although this is disputed. [7] The star has 3.8 [5] times the mass and 18 [1] times the radius of the Sun. The companion, component B, is a small white dwarf companion with 80% of the mass of the Sun and a class of DA4. [4] It was detected in 1985 by its ultraviolet emission. [8]
In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Xi1 Ceti itself is "the Fifth Star of Circular Celestial Granary", Tiān Qūn Wu. [16]
{{
cite web}}
: CS1 maint: postscript (
link)
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Cetus |
Right ascension | 02h 12m 59.99769s [1] |
Declination | +08° 50′ 48.2023″ [1] |
Apparent magnitude (V) | +4.36 [2] [combined] |
Characteristics | |
Spectral type | G7III Ba0.4 Fe-1 [3] + DA4 [4] |
B−V color index | 0.878±0.024 [2] |
Astrometry | |
Radial velocity (Rv) | −3.93±0.09 [2] km/s |
Proper motion (μ) |
RA: −24.498
[1]
mas/
yr Dec.: −5.952 [1] mas/ yr |
Parallax (π) | 9.5451 ± 0.3275 mas [1] |
Distance | 340 ± 10
ly (105 ± 4 pc) |
Absolute magnitude (MV) | –0.99 [5] |
Orbit [6] | |
Period (P) | 1,642.1±1.3 |
Semi-major axis (a) | ≥ 0.896 ± 0.020 AU (134 ± 3 Gm) |
Eccentricity (e) | 0 (fixed) |
Periastron epoch (T) | 34,985±5 MJD |
Semi-amplitude (K1) (primary) | 5.91±0.14 km/s |
Details | |
A | |
Mass | 3.80 [5] M☉ |
Radius | 18.2+1.0 −2.4 [1] R☉ |
Luminosity | 209.9±8.2 [1] L☉ |
Surface gravity (log g) | 2.60 [1] cgs |
Temperature | 5,184±50 [5] K |
Metallicity [Fe/H] | −0.01 [5] dex |
Age | 100 [7] Myr |
B | |
Mass | 0.8 [5] M☉ |
Surface gravity (log g) | 8.4 [8] cgs |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Xi1 Ceti , Latinized from ξ1 Ceti, is a binary star [10] system located in the equatorial constellation of Cetus. It is visible to the naked eye with a combined apparent visual magnitude of +4.36. [2] The distance to this system is approximately 340 light years based on parallax measurements, and it is drifting closer to the Sun with a radial velocity of −4 km/s. [2] The proximity of the star to the ecliptic means it is subject to lunar occultations. [11]
The spectroscopic binary nature of Xi1 Ceti was discovered in 1901 by William Wallace Campbell using the Mills spectrograph at the Lick Observatory. [12] [6] The pair have a circular orbit with a period of 4.5 years and a separation of 3.8 AU. [5] It is a suspected eclipsing binary with an amplitude of 0.03 in magnitude, which would suggest the orbital plane has a high inclination. [13]
The primary, designated component A, is a mild barium [14] giant star with a stellar classification of G7III Ba0.4 Fe-1. [3] Morgan and Keenan in 1973 had classified it as a bright giant star with an anomalous underabundance of the CN molecule. [15] Evidence has been found for an overabundance of s-process elements, [5] although this is disputed. [7] The star has 3.8 [5] times the mass and 18 [1] times the radius of the Sun. The companion, component B, is a small white dwarf companion with 80% of the mass of the Sun and a class of DA4. [4] It was detected in 1985 by its ultraviolet emission. [8]
In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Xi1 Ceti itself is "the Fifth Star of Circular Celestial Granary", Tiān Qūn Wu. [16]
{{
cite web}}
: CS1 maint: postscript (
link)