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HD 196761

From Wikipedia, the free encyclopedia
G-type main sequence star in the constellation Capricornus
HD 196761
Observation data
Epoch J2000      Equinox J2000
ConstellationCapricornus
Right ascension20h 40m 11.75616s[1]
Declination−23° 46′ 25.9178″[1]
Apparent magnitude (V)6.37[2]
Characteristics
Spectral typeG8V[3]
U−Bcolor index1.393[4]
B−Vcolor index0.719[5]
Astrometry
Radial velocity (Rv)–45.3[6] km/s
Proper motion (μ)RA: +501.45[1]mas/yr
Dec.: +461.36[1]mas/yr
Parallax (π)69.53±0.40 mas[1]
Distance46.9 ± 0.3 ly
(14.38 ± 0.08 pc)
Absolute magnitude (MV)5.58[7]
Details
Mass0.81 ± 0.03[8] M☉
Radius0.88[9] R☉
Surface gravity (log g)4.54[3] cgs
Temperature5,457[7] K
Metallicity [Fe/H]-0.30[7] dex
Rotational velocity (v sin i)3.50[10] km/s
Age5.63[11] Gyr
Other designations
CD−24° 16193,GJ 796,HD 196761,HIP 101997,HR 7898,LTT 8172,SAO 189549.[2]
Database references
SIMBADdata

HD 196761 is theHenry Draper Catalogue designation for aG-type main-sequence star in the constellationCapricornus. With anapparent magnitude of 6.37 it is near the limit of what can be seen with the naked eye, but according to theBortle Scale it may be possible to view it at night from rural skies. Based uponparallax measurements by theHipparcos spacecraft, it is located about 47light years from theSolar System.[1]

It has astellar classification of G8V with about 88%[9] of theradius of the Sun and 81%[8] of theSun's mass. Compared to theSun, this star has about half the proportion of elements other than hydrogen and helium.[7][12] Theprojected rotational velocity of the star's equator is a relatively leisurely 3.50 km/s.[10] This star has been examined for aninfrared excess that could indicate the presence of acircumstellar disk of dust, but as of 2015 none has been detected.[11]

Thespace velocity components of this star are U = −59, V = 20 and W = 4 km/s. It is presently following an orbit through theMilky Way that has aneccentricity of 0.18, bringing it as close as 24.27 kly (7.44 kpc) and as distant as 34.6 kly (10.6 kpc) from theGalactic Center. Theinclination of this orbit will carry HD 196761 no more than 0.65 kly (0.20 kpc) from the plane of thegalactic disk.[7]

References

[edit]
  1. ^abcdefvan 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,S2CID 18759600.
  2. ^ab"LHS 3570 -- High proper-motion Star".SIMBAD.Centre de Données astronomiques de Strasbourg. Retrieved2010-02-20.
  3. ^abGray, 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.S2CID 119476992.
  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. Astrophysics and Space Science Library. Vol. 474. pp. 653–664.arXiv:0708.1752.Bibcode:2007A&A...474..653V.doi:10.1051/0004-6361:20078357.ISBN 978-1-4020-6341-1.S2CID 18759600.{{cite book}}:|journal= ignored (help)
  6. ^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. ^abcdeHolmberg, 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.S2CID 118577511.
  8. ^abSantos, 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,S2CID 119347084.
  9. ^abJohnson, 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. ^abMartínez-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,S2CID 43455849, archived fromthe original(PDF) on 2017-09-22, retrieved2018-11-04.
  11. ^abMoro-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,S2CID 55170390, 143.
  12. ^Themetallicity 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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