HD 192310

Last updated
HD 192310
Capricornus constellation map.svg
Red circle.svg
Location of HD 192310 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Capricornus
Right ascension 20h 15m 17.39138s [1]
Declination −27° 01′ 58.7116″ [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 [4]
Astrometry
Radial velocity (Rv)−54.41±0.13 [1]  km/s
Proper motion (μ)RA: 1242.763  mas/yr [1]
Dec.: −181.175  mas/yr [1]
Parallax (π)113.4872 ± 0.0516  mas [1]
Distance 28.74 ± 0.01  ly
(8.812 ± 0.004  pc)
Absolute magnitude  (MV)6.0 [5]
Details
Mass 0.78 ± 0.04 [6]   M☉
Radius 0.79–0.85 [7]   R☉
Luminosity 0.385 ± 0.007 [8]   L☉
Surface gravity (log g)4.38 ± 0.19 [9]   cgs
Temperature 5069 ± 49 [9]   K
Metallicity [Fe/H]-0.01 ± 0.05 [9]   dex
Rotation 47.7 ± 4.9 days [8]
Rotational velocity (v sin i)<3 [8]  km/s
Age 7.5–8.9 [5]   Gyr
Other designations
5 G. Capricorni, CD-27°14659, GCTP  4804.00, Gl  785, HD  192310, HIP  99825, HR  7722, LHS  488, LTT  8009, NSV 12933, SAO  189065
Database references
SIMBAD data
ARICNS data

HD 192310 (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 28.7 light-years (8.8 parsecs ), 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.) HD 192310 is suspected of being a variable star, but this is unconfirmed.

Contents

Description

This is a K-type main sequence star with a stellar classification of K2+ V. [3] HD 192310 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 the now-doubtful HD 85512 b and the planets of 82 G. Eridani. The uncertainty in the mass of the second planet was 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]

A study in 2023 updated the parameters of these two planets, and identified a number of additional radial velocity signals. While most of these signals were attributed to stellar activity, one was considered a planet candidate. If real, this third planet would be a super-Earth orbiting closer to the star than the two known planets. [15] : 31  However, another 2023 study did not find this candidate signal and also attributed it to stellar activity. [16] : 10 

The HD 192310 planetary system [16]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥16.1±0.7  M🜨 0.32±0.0174.25±0.040.11±0.02——
c ≥15.9±0.9  M🜨 1.21±0.02534.9+5.9
−5.1		0.06+0.05
−0.04		——

See also

Related Research Articles

HD 37124 is a star in the equatorial constellation of Taurus, positioned about a half degree to the SSW of the bright star Zeta Tauri. The apparent visual magnitude of this star is 7.68, which is too dim to be visible to the naked eye. It is located at a distance of 103 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −23 km/s. Three extrasolar planets have been found to orbit the star.

HD 169830 is a star in the southern constellation of Sagittarius. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.90. The star is located at a distance of 120 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −17.3 km/s, and is predicted to come as close as 20.7 ly (6.4 pc) in 2.08 million years. HD 169830 is known to be orbited by two large Jupiter-like exoplanets.

HD 93083 is an orange-hued star in the southern constellation of Antlia. It has the proper name Macondo, after the mythical village of the novel One Hundred Years of Solitude. The name was selected by Colombia during the IAU's NameExoWorlds campaign. The star has an apparent visual magnitude of 8.30, which is too faint to be visible to the naked eye. It is located at a distance of 93 light years from the Sun based on parallax. HD 93083 is drifting further away with a radial velocity of +43.65 km/s, having come to within 43 light-years some 484,000 years ago.

HD 4208 is a star in the southern constellation of Sculptor. It has a yellow hue with an apparent visual magnitude of 7.78, making it too dim to be visible to the naked eye. But with binoculars or small telescope it should be an easy target. This object is located at a distance of 111.6 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +57 km/s.

HD 28185 is a yellow dwarf star similar to the Sun located 128 light-years away from Earth in the constellation Eridanus. The designation HD 28185 refers to its entry in the Henry Draper catalogue. The star is known to possess one long-period extrasolar planet.

HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus.

HD 4308 is a single star in the southern constellation of Tucana. It has a yellow hue and is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of 6.54. This object is located at a distance of 72 light years, as determined from parallax measurements. It is a population II star and is considered to be a member of the thick disk. The star is receding from the Sun with a radial velocity of +95 km/s.

<span class="mw-page-title-main">HD 47536</span> Star in the constellation Canis Major

HD 47536 is a single star in the southern constellation of Canis Major. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.25. The star is located at a distance of approximately 408 light years from the Sun based on parallax. It is drifting further away with a radial velocity of 80 km/s.

HD 111232 is a star in the southern constellation of Musca. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 7.59. The distance to this star is 94.5 light years based on parallax. It is drifting away from the Sun with a radial velocity of +104 km/s, having come to within 14.1 light-years some 264,700 years ago. The absolute magnitude of this star is 5.25, indicating it would have been visible to the naked eye at that time.

HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24, it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of 105.4 light-years from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s. It has an absolute magnitude of 4.67.

HD 142415 is a single star in the southern constellation of Norma, positioned next to the southern constellation border with Triangulum Australe and less than a degree to the west of NGC 6025. With an apparent visual magnitude of 7.33, it is too faint to be visible to the naked eye. The distance to this star is 116 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −12 km/s. It is a candidate member of the NGC 1901 open cluster of stars.

HD 196050 is a triple star system located in the southern constellation of Pavo. This system has an apparent magnitude of 7.50 and the absolute magnitude is 4.01. It is located at a distance of 165 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +61 km/s. It is also called by the Hipparcos designation HIP 101806.

HD 213240 is a possible binary star system in the constellation Grus. It has an apparent visual magnitude of 6.81, which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.

HD 162020 is a star in the southern constellation of Scorpius with a likely red dwarf companion. It has an apparent visual magnitude of 9.10, which is too faint to be visible to the naked eye. The distance to this system is 101 light years based on stellar parallax. It is drifting closer to the Sun with a radial velocity of −27 km/s, and is predicted to come to within ~18 light-years in 1.1 million years.

HIP 70849 is a star with two non-stellar companions in the southern constellation Lupus. It is a 10th magnitude star, making it too faint to be visible to the naked eye. The system is located at a distance of 78.7 light-years from the Sun based on parallax measurements.

HD 44594 is a star in the southern constellation Puppis. It has an apparent visual magnitude of 6.64, so it can be seen with the naked eye from the southern hemisphere under good viewing conditions. Based upon parallax measurements, it is located at a distance of 85 light-years from the Earth, giving it an absolute magnitude of 4.56.

41 Comae Berenices is a single, orange-hued star in the northern constellation of Coma Berenices. It is visible to the naked eye, having an apparent visual magnitude of 4.80. Based upon an annual parallax shift of 8.6 mas, it is located around 379 light years away. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

HD 96700 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Hydra. It has an apparent visual magnitude of 6.51, which puts it below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is around 83 light years away from the Sun. It is drifting further away with a radial velocity of 12.8 km/s.

HD 42618 is a well-studied star with an exoplanetary companion in the equatorial constellation of Orion. With an apparent visual magnitude of 6.85 it is too faint to be readily visible to the naked eye. This system is located at a distance of 79.6 light years from the Sun based on parallax measurements. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.321″ per year. HD 42618 is drifting closer with a radial velocity of −53.5 km/s and is predicted to come as near as 42.6 light-years in around 297,000 years.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  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/0603770 , Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID   119476992
  4. ↑ Samus, N. N.; Durlevich, O. V.; et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S, 1: B/gcvs, Bibcode:2009yCat....102025S
  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: 0807.1686 , Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID   27151456
  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/0105216 , Bibcode:2001A&A...373.1019S, doi:10.1051/0004-6361:20010648, S2CID   119347084
  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 (2): 521–524, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID   425754
  8. 1 2 3 4 5 Pepe, F.; et al. (2011), "The HARPS search for Earth-like planets in the habitable zone", VizieR On-line Data Catalog: J/A+A/534/A58, vol. 534, pp. A58, arXiv: 1108.3447 , Bibcode:2011yCat..35340058P, doi:10.1051/0004-6361/201117055, S2CID   15088852
  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/0401396 , Bibcode:2004A&A...418..703E, doi:10.1051/0004-6361:20035717, S2CID   55400558
  10. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, 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/0511180 , Bibcode:2006AsBio...6..308P, doi:10.1089/ast.2006.6.308, PMID   16689649, S2CID   119459291
  12. ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv: 1412.3648 , Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID   59039482, A35
  13. ↑ Howard, Andrew W.; Johnson, John Asher; et al. (March 2011). "The NASA-UC Eta-Earth Program: III. A Super-Earth orbiting HD 97658 and a Neptune-mass planet orbiting Gl 785". The Astrophysical Journal . 730 (1): 10. arXiv: 1011.0414 . Bibcode:2011ApJ...730...10H. doi:10.1088/0004-637X/730/1/10. S2CID   17943021.
  14. ↑ Schneider, Jean, "HD 192310 c", Extrasolar Planets Encyclopaedia, archived from the original on 2011-11-08, retrieved 2011-10-29
  15. ↑ Laliotis, Katherine; Burt, Jennifer A.; et al. (April 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal . 165 (4): 176. arXiv: 2302.10310 . Bibcode:2023AJ....165..176L. doi:10.3847/1538-3881/acc067.
  16. 1 2 Cretignier, M.; Dumusque, X.; et al. (August 2023). "YARARA V2: Reaching sub m/s precision over a decade using PCA on line-by-line RVs". arXiv: 2308.11812 [astro-ph.EP].
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.