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HD 30856

From Wikipedia, the free encyclopedia
K-type subgiant star in the constellation Pisces
HD 30856 / Mouhoun
Location of HD 30856 (circled)
Observation data
Epoch J2000.0[1]      Equinox J2000.0[1]
ConstellationEridanus[2]
Right ascension04h 50m 17.8614408264s[1]
Declination−24° 22′ 07.833769068″[1]
Apparent magnitude (V)7.911[1][3]
Characteristics
Evolutionary stageRed-giant branch star[1]
Spectral typeK0III[1][3]
B−Vcolor index0.961[1][3]
Astrometry
Radial velocity (Rv)35.71[1] km/s
Proper motion (μ)RA: 18.469[1]mas/yr
Dec.: −19.837[1]mas/yr
Parallax (π)7.5965±0.0179 mas[1]
Distance429 ± 1 ly
(131.6 ± 0.3 pc)
Orbit[4]
PrimaryHD 30856 A
CompanionHD 30856 B
Semi-major axis (a)0.786″
Details
HD 30856 A
Mass1.17[5] / 1.35[4] M
Radius4.40[5] R
Luminosity9.9±0.5[6] L
Surface gravity (log g)3.20[5] cgs
Temperature4895[5] / 4982 ± 44[4] K
Metallicity [Fe/H]−0.06±0.03[6] dex
Rotational velocity (v sin i)2.85[6] km/s
HD 30856 B
Mass0.54±0.01[4] M
Surface gravity (log g)4.7[4] cgs
Temperature3700–4150[4] K
Other designations
CD−24 2616,Gaia DR3 4893980371818915456,HD 30856,HIP 22491,SAO 169805,TIC 612908,TYC 6466-1769-1,GSC 06466-01769,2MASS J04501787-2422077[1]
Database references
SIMBADdata

HD 30856 (proper nameMouhoun) is abinary system between HD 30856 A (often simply HD 30856[6][7]), aK-typegiant star, and HD 30856 B, ared dwarf companion, located in the constellation ofEridanus about 430light-years distant.[2][1] Asuper-Jupiterexoplanet, HD 30856 b (proper name Nakanbé), is known to orbit the primary star.[6]

Stellar characteristics

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HD 30856 A is an evolved star in thered-giant branch, with a spectral type of K0 III, a radius of 4.4R, and a mass of 1.17M. The surface temperature of HD 30856 is estimated to be about 4,895K, which gives it an orange color. The star is roughly 10 times as bright as theSun, which, combined with a distance of 429 light-years, places itsapparent magnitude at 7.91,[3][5][6] too dim to be visible fromEarth by the naked eye.[8] The star is aged approximately 3.8billion years,[6] making it younger than the Sun (4.6 billion years old[9]).

Companion star

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Through the use ofadaptive optics, observations at theKeck II telescope in Hawaii revealed the existence of another star, designated HD 30856 B, about 0.8arcseconds east-southeast of HD 30856.[4] HD 30856 B has a mass of 0.54M and a temperature of 3700–4150 K,[4][a] typical for anM0V–M1V red dwarf.[10][11][12][b]

Since the star shares a very similarproper motion with HD 30856 A, the two stars are believed to be in a binary system. HD 30856 B revolves around the primary star (A) in a wide orbit, with asemi-major axis of 93 ± 8AU.[4]

Nomenclature

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In 2019, thePeople's Republic of Burkina Faso was assigned to giving the HD 30856 A system a proper name as part of theIAU100 NameExoWorlds Project,[2] planned to celebrate the hundredth anniversary of theInternational Astronomical Union (IAU), which grants the right to name an exoplanetary system to every state and territory in the world. Names were submitted and selected within Burkina Faso, which were then presented to the IAU to be officially recognized.[13] On 17 December 2019, the IAU announced that HD 30856 A and its planet, b, were named Mouhoun and Nakanbé, respectively.[7]

Mouhoun is named after theBlack Volta (locally called Mouhoun), Burkina Faso's largest river that serves a crucial societal role in the western part of the country. Nakanbé is the native name for theWhite Volta, the second largest river in the nation with its source located in theSahel region.[7]

Planetary system

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In 2011,radial-velocity observations made at theW. M. Keck Observatory revealed the existence of one exoplanet around HD 30856 A.[6] The planet, HD 30856 Ab, is thought to be agas giant at least 1.5 times the mass ofJupiter, which orbits its host star at a distance of 1.85AU once every 847 days (2.32 years).[5] Its orbit is nearly circular (i.e., with a loweccentricity),[5] similar to planets in theSolar System.[14]

The HD 30856 planetary system[5]
Companion
(in order from star)
MassSemimajor axis
(AU)
Orbital period
(days)
EccentricityInclinationRadius
HD 30856 Ab (Nakanbé)>1.547 MJ1.85847.468 ± 19.8110.061 ± 0.0581.228 RJ

References

[edit]
  1. ^abcdefghijklm"HD 30856".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2024-07-30.
  2. ^abc"List of stars and planets".Name ExoWorlds. IAU. Retrieved2019-09-15.
  3. ^abcdESA (1997), "The HIPPARCOS and TYCHO catalogues. Astrometric and photometric star catalogues derived from the ESA HIPPARCOS Space Astrometry Mission",Esa Special Publication, ESA SP Series,1200,Noordwijk,Netherlands: ESA Publications Division,Bibcode:1997ESASP1200.....E,ISBN 9290923997
  4. ^abcdefghiNgo, Henry; Knutson, Heather A.; Bryan, Marta L.; Blunt, Sarah; Nielsen, Eric L.; Batygin, Konstantin; Bowler, Brendan P.; Crepp, Justin R.; Hinkley, Sasha; Howard, Andrew W.; Mawet, Dimitri (2017-06-01)."No Difference in Orbital Parameters of RV-detected Giant Planets between 0.1 and 5 au in Single versus Multi-stellar Systems".The Astronomical Journal.153 (6): 242.arXiv:1704.02326.Bibcode:2017AJ....153..242N.doi:10.3847/1538-3881/aa6cac.ISSN 0004-6256.
  5. ^abcdefghLuhn, Jacob K.; Bastien, Fabienne A.; Wright, Jason T.; Johnson, John A.; Howard, Andrew W.; Isaacson, Howard (2019-04-01)."Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts".The Astronomical Journal.157 (4): 149.arXiv:1811.03043.Bibcode:2019AJ....157..149L.doi:10.3847/1538-3881/aaf5d0.ISSN 0004-6256.
  6. ^abcdefghJohnson, John Asher; Clanton, Christian; Howard, Andrew W.; Bowler, Brendan P.; Henry, Gregory W.; Marcy, Geoffrey W.; Crepp, Justin R.; Endl, Michael; Cochran, William D.; MacQueen, Phillip J.; Wright, Jason T.; Isaacson, Howard (2011-12-01). "Retired a Stars and Their Companions. Vii. 18 New Jovian Planets".The Astrophysical Journal Supplement Series.197 (2): 26.arXiv:1108.4205.Bibcode:2011ApJS..197...26J.doi:10.1088/0067-0049/197/2/26.ISSN 0067-0049.
  7. ^abc"Approved names"(PDF).NameExoWorlds.IAU. p. 4. Retrieved2024-07-30.
  8. ^John E. Bortle (February 2001)."The Bortle Dark-Sky Scale".Sky & Telescope. Archived fromthe original on 2009-03-23. Retrieved2009-11-18.
  9. ^Connelly, J. N.; Bizzarro, M.; Krot, A. N.; Nordlund, Å.; Wielandt, D.; Ivanova, M. A. (2 November 2012). "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk".Science.338 (6107):651–655.Bibcode:2012Sci...338..651C.doi:10.1126/science.1226919.PMID 23118187.S2CID 21965292.(registration required)
  10. ^Pecaut, Mark J.; Mamajek, Eric E. (1 September 2013)."Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-main-sequence Stars".The Astrophysical Journal Supplement Series.208 (1): 9.arXiv:1307.2657.Bibcode:2013ApJS..208....9P.doi:10.1088/0067-0049/208/1/9.ISSN 0067-0049.S2CID 119308564.
  11. ^Mamajek, Eric (2 March 2021)."A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence". University of Rochester, Department of Physics and Astronomy. Retrieved5 July 2021.
  12. ^Cifuentes, C.; Caballero, J.A.; Cortés-Contreras, M.; Montes, D.; Abellán, F.J.; Dorda, R.; Holgado, G. (2020). "CARMENES input catalogue of M dwarfs. V. Luminosities, colours, and spectral energy distributions".Astronomy and Astrophysics.642 (October 2020): 32.arXiv:2007.15077.Bibcode:2020A&A...642A.115C.doi:10.1051/0004-6361/202038295.
  13. ^"Methodology".Name ExoWorlds. IAU. Retrieved2019-09-15.
  14. ^Limbach, MA; Turner, EL (2015)."Exoplanet orbital eccentricity: multiplicity relation and the Solar System".Proc Natl Acad Sci U S A.112 (1):20–4.arXiv:1404.2552.Bibcode:2015PNAS..112...20L.doi:10.1073/pnas.1406545111.PMC 4291657.PMID 25512527.

Footnotes

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  1. ^The source publication provides three separate estimates, namely 3940 ± 200 K, 3945 ± 70 K, and 3731 ± 29 K.
  2. ^According to the listed sources, typical M0V and M1V stars have masses of 0.57 / 0.54M and surface temperatures of 3850 / 3660 K, respectively.

See also

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External links

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