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HD 45350 b

Coordinates:Sky map06h 28m 45.7103s, +38° 57′ 46.667″
From Wikipedia, the free encyclopedia
Extrasolar planet in the constellation of Auriga orbiting the star HD 45350
HD 45350 b / Peitruss
Discovery
Discovered byMarcy,Butler,
Vogt, et al.
Discovery siteKeck Observatory,Hawaii
 United States
Discovery dateJanuary 20, 2005
Radial velocity
Orbital characteristics
Apastron3.41 AU (510,000,000 km)
Periastron0.43 AU (64,000,000 km)
1.92 ± 0.067 AU (287,200,000 ± 10,000,000 km)[1]
Eccentricity0.778 ± 0.009[1]
963.6 ± 3.4[1]d
2.64 ± 0.01y
21.7
2,451,825.3 ± 7.1[1]
343.4 ± 2.3[1]
Semi-amplitude58.0 ± 1.7[1]
StarHD 45350

HD 45350 b is anextrasolar planet located approximately 160light-years away in theconstellation ofAuriga. It has aminimum mass about 1.79 times that ofJupiter. The mean distance of the planet from the star is more than the distance betweenMars and theSun, but due to the planet's high orbitaleccentricity, it is as close to the star asMercury is from the Sun atperiastron, while atapastron, it is eight times further.

The planet HD 45350 b is namedPeitruss. The name was selected in theNameExoWorlds campaign byLuxembourg, during the 100th anniversary of theIAU. Peitruss is derived from the name of the Luxembourg riverPétrusse.[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 0.2AU 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

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  1. ^abcdefTable 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 Journal131, #6 (June 2006), pp. 3131–3134,Bibcode:2006AJ....131.3131E,doi:10.1086/503746.
  2. ^"Approved names".NameExoworlds. Retrieved2020-01-02.
  3. ^"International Astronomical Union | IAU".www.iau.org. Retrieved2020-01-02.
  4. ^"Luxembourg".NameExoworlds. Retrieved2020-10-30.
  5. ^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 Journal134, #3 (September 2007), pp. 1276–1284,Bibcode:2007AJ....134.1276W,doi:10.1086/520880.

External links

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