HD 192310

HR 7722
Diagram showing star positions and boundaries of the Capricornus constellation and its surroundings


A star chart of the constellation of Capricornus showing the position of HR 7722 (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Capricornus
Right ascension 20h 15m 17.39122s[1]
Declination −27° 01′ 58.7121″[1]
Apparent magnitude (V) 5.73[2]
Characteristics
Spectral type K2+ V[3]
U−B color index 0.64[2]
B−V color index 0.88[2]
Variable type Suspected
Astrometry
Radial velocity (Rv)-54.2[4] km/s
Proper motion (μ) RA: 1241.85[1] mas/yr
Dec.: -180.96[1] mas/yr
Parallax (π)112.22 ± 0.30[1] mas
Distance29.06 ± 0.08 ly
(8.91 ± 0.02 pc)
Absolute magnitude (MV)6.0[5]
Details
Mass0.78 ± 0.04[6] M☉
Radius0.79–0.85[7] R☉
Luminosity0.385 ± 0.007[8] L☉
Surface gravity (log g)4.38 ± 0.19[9] cgs
Temperature5069 ± 49[9] K
Metallicity [Fe/H]-0.01 ± 0.05[9] dex
Rotation47.7 ± 4.9 days[8]
Rotational velocity (v sin i)<3[8] km/s
Age7.5–8.9[5] Gyr
Other designations
5 G. Capricorni, CD -27°14659, FK5, GCTP 4804.00, Gl 785, HD 192310, HIP 99825, LHS 488, LTT 8009, NSV 12933, SAO 189065.
Database references
SIMBADdata
ARICNSdata

HR 7722 (also known as 5 G. Capricorni or Gliese 785) is a star in the southern constellation of Capricornus. It is located in the solar neighborhood at a distance of just over 29 light years, and is within the range of luminosity needed to be viewed from the Earth with the unaided eye. (According to the Bortle scale, it can be viewed from dark suburban skies.) HR 7722 is suspected of being a variable star, but this is unconfirmed.

This is a K-type main sequence star with a stellar classification of K2+ V.[3] HR 7722 has about 78% of the Sun's mass[6] and, depending on the estimation method, 79% to 85% of the radius of the Sun.[7] The effective temperature of the photosphere is about 5069 K, giving it the orange-hued glow of a K-type star.[10] It is older than the Sun, with age estimates in the range 7.5–8.9 billion years.[5] The proportion of elements other than hydrogen and helium, known as the metallicity, is similar to that of the Sun.[9] It is spinning slowly, completing a rotation roughly every 48 days.[8]

The space velocity components of this star are (U, V, W) = (–69, –13, –14) km/s. It is following an orbit through the Milky Way galaxy that has an orbital eccentricity of 0.18 at a mean galactocentric distance of 8.1 kpc.[11] The star will achieve perihelion in around 82,200 years when it comes within 20.18 ly (6.188 pc) of the Sun.[12]

Planetary system

The system has a Neptune-mass planet "b", discovered in 2010.[13] A second planet "c" was found in this system in 2011 by the HARPS GTO program, along with HD 85512 b and the planets of 82 G. Eridani. The uncertainty in the mass of the second planet is much higher than for the first because of the lack of coverage around the full orbit. Both planets may be similar in composition to Neptune. They are orbiting along the inner and outer edges of the habitable zone for this star.[8][14]

The HD 192310 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥16.9 ± 0.9 M⊕ 0.32 ± 0.005 74.72 0.13 ± 0.04 — —
c ≥24 ± 5 M⊕ 1.18 ± 0.025 525.8 ± 9.2 0.32 ± 0.11 — —

See also

References

  1. 1 2 3 4 5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
  2. 1 2 3 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  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/0603770Freely accessible, Bibcode:2006AJ....132..161G, doi:10.1086/504637
  4. ↑ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198Freely accessible, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959
  5. 1 2 3 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686Freely accessible, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785
  6. 1 2 Santos, N. C.; Israelian, G.; Mayor, M. (July 2001), "The metal-rich nature of stars with planets", Astronomy and Astrophysics, 373 (3): 1019–1031, arXiv:astro-ph/0105216Freely accessible, Bibcode:2001A&A...373.1019S, doi:10.1051/0004-6361:20010648
  7. 1 2 Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics, 367: 521–524, arXiv:astro-ph/0012289Freely accessible, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451
  8. 1 2 3 4 5 Pepe, F.; et al. (2011), "The HARPS search for Earth-like planets in the habitable zone: I – Very low-mass planets around HD20794, HD85512 and HD192310", VizieR On-line Data Catalog: J/A+A/534/A58, arXiv:1108.3447Freely accessible, Bibcode:2011yCat..35349058P
  9. 1 2 3 4 Ecuvillon, A.; et al. (May 2004), "Nitrogen abundances in planet-harbouring stars", Astronomy and Astrophysics, 418 (2): 703–715, arXiv:astro-ph/0401396Freely accessible, Bibcode:2004A&A...418..703E, doi:10.1051/0004-6361:20035717
  10. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16.
  11. ↑ Porto de Mello, Gustavo; del Peloso, Eduardo F. (April 2006), "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun", Astrobiology, 6 (2): 308–331, arXiv:astro-ph/0511180Freely accessible, Bibcode:2006AsBio...6..308P, doi:10.1089/ast.2006.6.308, PMID 16689649
  12. ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648Freely accessible, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, A35.
  13. ↑ Schneider, Jean, "Gl 785", Extrasolar Planets Encyclopaedia, retrieved 2011-10-29
  14. ↑ Schneider, Jean, "HD 192310 c", Extrasolar Planets Encyclopaedia, retrieved 2011-10-29
This article is issued from Wikipedia - version of the 6/23/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.