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HD 45350 b - Wikipedia

Coordinates:

06^h 28^m 45.7103^s, +38° 57′ 46.667″

From Wikipedia, the free encyclopedia

HD 45350 b / Peitruss
Discovery
Discovered by	Marcy, Butler, Vogt, et al.
Discovery site	Keck Observatory, Hawaii United States
Discovery date	January 20, 2005
Detection method	Radial velocity
Orbital characteristics
Apastron	3.41 AU (510,000,000 km)
Periastron	0.43 AU (64,000,000 km)
Semi-major axis	1.92 ± 0.067 AU (287,200,000 ± 10,000,000 km)^[1]
Eccentricity	0.778 ± 0.009^[1]
Orbital period (sidereal)	963.6 ± 3.4^[1] d 2.64 ± 0.01 y
Average orbital speed	21.7
Time of periastron	2,451,825.3 ± 7.1^[1]
Argument of periastron	343.4 ± 2.3^[1]
Semi-amplitude	58.0 ± 1.7^[1]
Star	HD 45350

HD 45350 b is an extrasolar planet located approximately 160 light-years away in the constellation of Auriga. It has a minimum mass about 1.79 times that of Jupiter. The mean distance of the planet from the star is more than the distance between Mars and the Sun, but due to the planet's high orbital eccentricity, it is as close to the star as Mercury is from the Sun at periastron, while at apastron, it is eight times further.

The planet HD 45350 b is named Peitruss. The name was selected in the NameExoWorlds campaign by Luxembourg, during the 100th anniversary of the IAU. Peitruss is derived from the name of the Luxembourg river Pétrusse.^[2]^[3] The 2019–2020 class of 3B from the Luxembourgish Echternach high school won the contest to name both the star and its planet. The students who helped name both celestial objects were Lucien Nicolas Berger, Léna Boucq Kieffel, Ben de Boer, Cédric Dehlez, Nicolas Delhez, Sergio Manuel Dias Costa, Pierre Fusshoeller, Jil Menei, Philippe Schaack and Claire Zeien. The overseeing committee members who organized the contest and the vote of the respective celestial objects were Eric Buttini, Patrick Michaely, Nicolas Faber, Jeanny-Jungbluth-Schmidt and Yanna Di Ronco.^[4]

Dynamical simulations covering a period of 10⁷ years show that a second, low-mass, planet could only orbit stably if it were no more than 0.2 AU away from the star; in the simulations, these planets show oscillations in eccentricity up to an eccentricity of 0.25. Radial velocity observations rule out any such planet whose mass is greater than 4 Neptune masses.^[5]

References

^ ^a ^b ^c ^d ^e ^f Table 2, combined solution, Determination of the Orbit of the Planetary Companion to the Metal-Rich Star HD 45350, Michael Endl, William D. Cochran, Robert A. Wittenmyer, and Artie P. Hatzes, Astronomical Journal 131, #6 (June 2006), pp. 3131–3134, Bibcode:2006AJ....131.3131E, doi:10.1086/503746.
^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
^ "Luxembourg". NameExoworlds. Retrieved 2020-10-30.
^ Dynamical and Observational Constraints on Additional Planets in Highly Eccentric Planetary Systems, Robert A. Wittenmyer, Michael Endl, William D. Cochran, and Harold F. Levison, Astronomical Journal 134, #3 (September 2007), pp. 1276–1284, Bibcode:2007AJ....134.1276W, doi:10.1086/520880.

External links

"HD 45350". Exoplanets. Archived from the original on 2008-05-18. Retrieved 2008-08-20.
HD 45350b Simulation
Michael Endl; Cochran; Wittenmyer; Hatzes (2006). "Determination Of The Orbit Of The Planetary Companion To The Metal Rich Star HD 45350". The Astronomical Journal. 131 (6): 3131–3134. arXiv:astro-ph/0603007. Bibcode:2006AJ....131.3131E. doi:10.1086/503746. S2CID 119389442.

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