HD 196761

HD 196761
Observationsdata
Epok: J2000.0
StjärnbildStenbocken
Rektascension20t 40m 11,75616s[1]
Deklination-23° 46′ 25,9178″[1]
Skenbar magnitud ()+6,37 (V)[2]
Stjärntyp
SpektraltypG8 V[3]
U–B+1,393[4]
B–V+0,719[5]
Astrometri
Radialhastighet ()-45,3[6] km/s
Egenrörelse (µ)RA: +501,45[1] mas/år
Dek.: +461,36[1] mas/år
Parallax ()69,53 ± 0,40[1]
Avstånd46,9 ± 0,3  (14,38 ± 0,08 pc)
Absolut magnitud ()+5,58[7]
Detaljer
Massa0,81 ± 0,03[8] M
Radie0,88[9] R
Luminositet0,590[10] L
Temperatur5 457[7] K
Metallicitet-0,30 (Fe/H)[7] dex
Vinkelhastighet3,50[11] km/s
Ålder5,63[12] miljarder år
Andra beteckningar
LHS 3570, CD-24 16193, CPD-24 7050, GJ 796, HD 196761, HIC 101997, HIP 101997, HR 7898, IRAS 20372-2357, MASS J20401173-2346262, NLTT 49644, PLX 4911, PPM 271457, SAO 189549, TYC 6921-1792-1, uvby98 100196761, WISEA J204012.13-234620.9, Gaia DR2 6854626246593473792 [13][2]

HD 196761 är en ensam stjärna belägen i den mellersta delen av stjärnbilden Stenbocken. Den har en skenbar magnitud av ca 6,37[2] och är mycket svagt synlig för blotta ögat där ljusföroreningar ej förekommer. Baserat på parallaxmätning inom Hipparcosuppdraget på ca 69,5[6] mas, beräknas den befinna sig på ett avstånd på ca 47 ljusår (ca 14 parsek) från solen. Den rör sig närmare solen med en heliocentrisk radialhastighet på ca -45 km/s.[6]

Egenskaper

HD 196761 är en solliknande gul till vit stjärna i huvudserien av spektralklass G8 V,[3] som har en andel av element tyngre än väte och helium, känd som metallicitet, som är ungefär hälften solens.[7][14] Den har en massa som är ca 0,8[8] solmassor, en radie som är ca 0,9[9] solradier och har ca 0,6 gånger solens utstrålning av energi[10] från dess fotosfär vid en effektiv temperatur av ca 5 500 K.[7]

HD 196761 har undersökts med avseende på överskott av infraröd strålning, som kan ange närvaro av en omgivande stoftskiva, men fram till 2015 har ingen sådan upptäckts.[12]

Referenser

Den här artikeln är helt eller delvis baserad på material från engelskspråkiga Wikipedia, HD 196761, 7 februari 2021.

Noter

  1. ^ [a b c d e] van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ [a b c] "LHS 3570 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Hämtad 2010-02-20.
  3. ^ [a b] Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637.
  4. ^ Rufener, F. (October 1976). "Second catalogue of stars measured in the Geneva Observatory photometric system". Astronomy & Astrophysics Supplement Series. 26: 275–351. Bibcode:1976A&AS...26..275R.
  5. ^ van Leeuwen, Floor (2007). Hipparcos, the new Reduction of the Raw data. Astron. Astrophys. Astrophysics and Space Science Library. 474. pp. 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. ISBN 978-1-4020-6341-1.
  6. ^ [a b c] Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
  7. ^ [a b c d e] Holmberg, J.; Nordström, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics Supplement Series. 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191.
  8. ^ [a b] Santos, N. C.; et al. (July 2001), "The metal-rich nature of stars with planets", Astronomy and Astrophysics, 373 (3): 1019–1031, arXiv:astro-ph/0105216, Bibcode:2001A&A...373.1019S, doi:10.1051/0004-6361:20010648.
  9. ^ [a b] Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the Sun". Astrophysical Journal Supplement Series. 53: 643–711. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
  10. ^ [a b] https://www.universeguide.com/star/101997/hd196761. Hämtad 2021-02-07.
  11. ^ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
  12. ^ [a b] Moro-Martín, A.; et al. (March 2015), "Does the Presence of Planets Affect the Frequency and Properties of Extrasolar Kuiper Belts? Results from the Herschel Debris and Dunes Surveys", The Astrophysical Journal, 801 (2): 28, arXiv:1501.03813, Bibcode:2015ApJ...801..143M, doi:10.1088/0004-637X/801/2/143, 143.
  13. ^ http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+196761%7CHämtad 2021-02-07.
  14. ^ The metallicity of the star is −0.30, so the proportion of metals is given by: 10−0.30 = 0.501 or 50%.

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