HD 196761

Last updated
HD 196761
Observation data
Epoch J2000       Equinox J2000
Constellation Capricornus
Right ascension 20h 40m 11.75616s [1]
Declination −23° 46 25.9178 [1]
Apparent magnitude  (V)6.37 [2]
Characteristics
Spectral type G8V [3]
U−B color index 1.393 [4]
B−V color index 0.719 [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]
Distance 46.9 ± 0.3  ly
(14.38 ± 0.08  pc)
Absolute magnitude  (MV)5.58 [7]
Details
Mass 0.81 ± 0.03 [8]   M
Radius 0.88 [9]   R
Surface gravity (log g)4.54 [3]   cgs
Temperature 5,457 [7]   K
Metallicity [Fe/H]-0.30 [7]   dex
Rotational velocity (v sin i)3.50 [10]  km/s
Age 5.63 [11]   Gyr
Other designations
CD 24° 16193, GJ 796, HD 196761, HIP  101997, HR 7898, LTT 8172, SAO  189549. [2]
Database references
SIMBAD data

HD 196761 is the Henry Draper Catalogue designation for a G-type main-sequence star in the constellation Capricornus. With an apparent magnitude of 6.37 it is near the limit of what can be seen with the naked eye, but according to the Bortle Scale it may be possible to view it at night from rural skies. Based upon parallax measurements by the Hipparcos spacecraft, it is located about 47 light years from the Solar System. [1]

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

The space velocity components of this star are U = −59, V = 20 and W = 4 km/s. It is presently following an orbit through the Milky Way that has an eccentricity 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 the Galactic Center. The inclination of this orbit will carry HD 196761 no more than 0.65 kly (0.20 kpc) from the plane of the galactic disk. [7]

Related Research Articles

<span class="mw-page-title-main">Zeta Sculptoris</span> Star in the constellation Sculptor

Zeta Sculptoris, Latinized from ζ Sculptoris, is a multiple star system in the constellation Sculptor. It is faintly visible to the naked eye with an apparent magnitude of 5.04. The annual parallax shift is 6.49 mas, which yields a distance estimate of about 500 light years from the Sun. It is moving further away with a radial velocity of +8.6 km/s. Zeta Sculptoris is near the Blanco 1 cluster as viewed from Earth, although parallax measurements indicate it to be substantially closer.

<span class="mw-page-title-main">Mu Virginis</span> F-type main sequence star in the constellation Virgo

Mu Virginis, Latinized from μ Virginis, is a star in the zodiac constellation of Virgo. It was listed in the Calendarium of Al Achsasi al Mouakket as rijl al-‘awwā’, Arabic رجل العواء, meaning "The foot of the barking (dog)". With an apparent visual magnitude of 3.88, it is bright enough to be seen with the naked eye. The position of the star near the celestial equator means it is visible from most of the Earth. Based upon parallax measurements, Mu Virginis is located some 59.6 light-years from the Sun.

Zeta Trianguli Australis is a spectroscopic binary in the constellation Triangulum Australe. It is approximately 39.5 light years from Earth.

1 Cassiopeiae is a single star in the northern constellation of Cassiopeia, located around 1,130 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of +4.84. This object is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.

HD 219659 is suspected variable star in the equatorial constellation of Aquarius.

HD 220466 is a F-type subgiant or main sequence star in the constellation Aquarius. It has apparent magnitude 6.47 and is about 200 light-years away. In 1913, an apparent visual companion of apparent magnitude 10.3 was observed 1.9 arcseconds away from the star, but it is doubtful whether it exists.

HD 149837 is a binary star in the southern constellation of Ara.

HD 134335 is a giant star in the northern constellation of Boötes.

HD 130603 is a double star in the northern constellation of Boötes. As of 2010.476, the components have an angular separation of 2.06″ along a position angle of 54.7°.

HD 128093 is a double star in the constellation Boötes. The brighter component is an F-type main-sequence star with a stellar classification of F5V and an apparent magnitude of 6.33. It has a magnitude 11.33 companion at an angular separation of 28.1 along a position angle of 318°.

HD 131473 is a binary star system in the northern constellation of Boötes. The primary is an F-type subgiant with a stellar classification of F4IV, while its companion is a G-type subgiant with a stellar classification of G1IV.

40 Aquarii is a star in the equatorial constellation of Aquarius. 40 Aquarii is its Flamsteed designation; it was too faint to be included in the Bright Star Catalogue. The brightness of this star is below the normal limit for visibility with the naked eye, having an apparent visual magnitude of 6.93. Based upon parallax measurements, it is located about 726 light-years away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of -3 km/s. 40 Aquarii is positioned near the ecliptic and thus is subject to lunar occultations.

<span class="mw-page-title-main">HD 211575</span> Star in the constellation Aquarius

HD 211575 is a star in the constellation Aquarius in between "Gamma Aquarii", "Pi Aquarii" and "Sadalmelik". It is a member of the corona of the Ursa Major moving group.

<span class="mw-page-title-main">Chi Ceti</span> Double star in the constellation Cetus

Chi Ceti , is the Bayer designation for a double star in the equatorial constellation of Cetus. They appear to be common proper motion companions, sharing a similar motion through space. The brighter component, HD 11171, is visible to the naked eye with an apparent visual magnitude of 4.66, while the fainter companion, HD 11131, is magnitude 6.75. Both lie at roughly the same distance, with the brighter component lying at an estimated distance of 75.6 light years from the Sun based upon an annual parallax shift of 43.13 mass.

Omega Hydrae, Latinised from ω Hydrae, is a golden-hued star in the equatorial constellation of Hydra, located to the west-southwest of the brighter star Zeta Hydrae. Based upon an annual parallax shift of just 3.64 mas as seen from Earth, it is located roughly 900 light-years from the Sun. It is faintly visible to the naked eye with an apparent visual magnitude of 5.00.

<span class="mw-page-title-main">HD 70555</span> Star in the constellation Puppis

HD 70555 is a class K2.5II-III star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.

<span class="mw-page-title-main">HD 61831</span> Star in the constellation Puppis

HD 61831 is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.84 and it is approximately 556 light years away based on parallax.

<span class="mw-page-title-main">HD 167818</span> Star in the constellation Sagittarius

HD 167818 is a class K3II star in the constellation Sagittarius. Its apparent magnitude is 4.66 and it is approximately 760 light years away based on parallax.

139 Tauri is a single, blue-white hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of 4.81. The distance to this star, as determined from an annual parallax shift of 2.10±0.19 mas, is roughly 1,600 light years. Because this star is located near the ecliptic, it is subject to occultations by the Moon. One such event was observed April 28, 1990.

84 Ceti is the Flamsteed designation for a binary star system in the equatorial constellation of Cetus. It has an apparent visual magnitude of 5.7, making it faintly visible to the naked eye from dark suburban skies. Parallax measurements with the Hipparcos spacecraft put this system at a distance of around 74 light years.

References

  1. 1 2 3 4 5 6 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, S2CID   18759600.
  2. 1 2 "LHS 3570 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg . Retrieved 2010-02-20.
  3. 1 2 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. 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. 1 2 3 4 5 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. S2CID   118577511.
  8. 1 2 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, S2CID   119347084.
  9. 1 2 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. 1 2 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, S2CID   43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  11. 1 2 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, S2CID   55170390, 143.
  12. The metallicity of the star is −0.30, so the proportion of metals is given by:
    10−0.30 = 0.501
    or 50%.