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Wide binary star system in the constellation Phoenix
HD 142 is a wide
binary star
[5] system in the southern
constellation of
Phoenix . The main component has a yellow-white hue and is dimly visible to the naked eye with an
apparent visual magnitude of 5.7.
[3] The system is located at a distance of 85.5
light years from the
Sun based on
parallax measurements, and is drifting further away with a
radial velocity of +6 km/s.
[17]
The primary component is an
F-type main-sequence star with a
stellar classification of F7V,
[6] which indicates it is undergoing
core
hydrogen fusion . It is an estimated 2.5
[12] billion years old and is spinning with a
projected rotational velocity of 10 km/s.
[13] The star has 1.25 times the
mass of the Sun and 1.4 times the
Sun's radius . It is radiating 2.9 times the
luminosity of the Sun from its
photosphere at an
effective temperature of 6,338 K.
[12]
A magnitude 11.5
[5] companion star was detected in 1894 making this a
binary star system.
[18] The binary companion was confirmed to be
gravitationally bound in 2007 and determined to be a
red dwarf of
spectral type K8.5-M1.5
[7] with 54% of the Sun's mass.
[14] The pair have a projected separation of 120.6
AU .
[14]
Planetary system
In 2001, the
Anglo-Australian Planet Search team led by
Chris Tinney announced the discovery of an
extrasolar planet orbiting the primary star.
[19]
[20] An additional linear trend in the
radial velocity data was noticed in 2006
[21] that could have been due to another planet or to the stellar companion.
[22] In 2012, additional measurements allowed the detection of a second planet. A third possible planet with a period of 108 days was seen in the data, but with a false alarm probability of five percent.
[23] Another paper by the same team updated the parameters for b and c but did not mention the possible planet d.
[24]
An
astrometric measurement of HD 142 b's inclination and true mass was published in 2022 as part of
Gaia DR3 .
[25] Another 2022 study determined the inclination and true mass of planet c, and confirmed the existence of planet d.
[26]
See also
References
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^
a
b
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^
a
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Gaia DR2 record for this source at
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^
a
b
c Eggleton, P. P.; Tokovinin, A.A. (September 2008).
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^
a
b Gray, R. O.; et al. (2006).
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^
a
b Eggenberger, A.; et al. (2007).
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doi :
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^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters . 38 (5): 331.
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^
a
b
c
d Vallenari, A.; et al. (Gaia collaboration) (2023).
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arXiv :
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S2CID
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^ Holmberg; et al. (2009).
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^
a
b
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S2CID
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Gaia DR3 record for this source at
VizieR .
^
a
b
c Ghezzi, L.; et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal , 720 (2): 1290–1302,
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^
a
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^
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b
c Tokovinin, A.; Kiyaeva, O. (February 2016).
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^
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^
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^
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^ Tinney, C. G.; et al. (2002).
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^ Butler, R. P.; et al. (2006).
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^ Wright, J. T.; et al. (2007).
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^ Wittenmyer, Robert A.; et al. (2020). "Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society . 492 (1): 377–383.
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^
a
b Gaia Collaboration; et al. (2023). "Gaia Data Release 3". Astronomy & Astrophysics . 674 : A34.
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^
a
b Feng, Fabo; Butler, R. Paul; et al. (August 2022).
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External links
"HD 142" . Open Exoplanet Catalogue . Retrieved 2014-09-08 .