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Probable binary star system in the constellation Crater
Zeta Crateris (ζ Crateris ) is a
binary star
[3] system in the southern
constellation of
Crater . Zeta Crateris appears to be about half-way between
Epsilon Corvi to the southeast and
Delta Crateris to the northwest, and marks the lower left corner of the rim of the bowl.
Eta Crateris lies somewhat less than half of the way from Zeta Crateris to
Gamma Corvi , the bright star above, (north) of Epsilon Corvi.
Zeta Crateris is a
photometrically constant
[11] system that is visible to the naked eye with an
apparent visual magnitude of 4.740.
[2] With an annual
parallax shift of 9.24
[1]
mas as viewed from Earth, Zeta Crateris is located roughly 350
light years from the
Sun . At that distance, the visual magnitude of the system is diminished by an
extinction factor of 0.21 due to
interstellar dust .
[7]
The two components of this system had an
angular separation of 0.20
arc seconds along a
position angle of 22°, as of 1991.
[12] The primary, component A, is a magnitude 4.95
evolved
giant star with a
stellar classification of G8 III.
[4] It is a
red clump star that is generating energy through the fusion of helium at its core.
[13] Zeta Crateris has expanded to 13
[8] times the
radius of the Sun and shines with 157
[9] times the
Sun's luminosity . This energy is being radiated into outer space from the
outer envelope at an
effective temperature of 4,992 K.
[7]
The secondary, component B, is a magnitude 7.84 star.
[12] Zeta Crateris is a confirmed member of the
Sirius supercluster
[14] and is a candidate member of the
Ursa Major Moving Group , a collection of stars that share a similar motion through space and may have at one time been members of the same
open cluster .
[15]
References
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b
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a
b
c
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^
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^
a
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arXiv :
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doi :
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Gaia DR2 record for this source at
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^
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f
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^
a
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^
a
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^
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Centre de données astronomiques de Strasbourg . Retrieved 2017-03-01 .
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^
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