HD 168443

Last updated
HD 168443
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Serpens
Right ascension 18h 20m 03.933288s [1]
Declination −09° 35′ 44.614581″ [1]
Apparent magnitude  (V)6.92 [2]
Characteristics
Spectral type G6V [3]
B−V color index 0.724±0.014 [2]
Astrometry
Radial velocity (Rv)−48.69±0.10 [2]  km/s
Proper motion (μ)RA: −91.792±0.036  mas/yr [1]
Dec.: −223.979±0.030  mas/yr [1]
Parallax (π)25.5913 ± 0.0410  mas [1]
Distance 127.4 ± 0.2  ly
(39.08 ± 0.06  pc)
Absolute magnitude  (MV)4.198 [4]
Details [4]
Mass 0.995±0.019  M☉
Radius 1.51±0.06  R☉
Luminosity 2.413±0.009 [5]   L☉
Surface gravity (log g)4.07±0.06  cgs
Temperature 5,491±44  K
Metallicity [Fe/H]+0.04±0.03  dex
Rotational velocity (v sin i)2.20±0.50 km/s
Age 11.3+1.0
−0.8 [2]   Gyr
Other designations
BD−09°4692, GJ  4052, HD  168443, HIP  89844, SAO  142228, LTT  7289 [6]
Database references
SIMBAD data
Exoplanet Archive data

HD 168443 is an ordinary yellow-hued star in the Serpens Cauda segment of the equatorial constellation of Serpens. It is known to have two substellar companions. With an apparent visual magnitude of 6.92, [2] the star lies just below the nominal lower brightness limit of visibility to the normal human eye. This system is located at a distance of 127  light years from the Sun based on parallax, [1] but is drifting closer with a radial velocity of −48.7 km/s. [2]

Contents

This stellar object is a core hydrogen fusing G-type main-sequence star with a classification of G6V, although it is likely evolved [4] with an age of around 11 billion years. [2] It is slightly lower in mass than the Sun but has a radius that is larger by 51%. The star is spinning with a leisurely projected rotational velocity of 2.2 km/s [4] and it has a very inactive chromosphere. [3] [4] It is radiating 2.4 [5] times the luminosity of the Sun from its photosphere at an effective temperature of 5,491 K. [4]

Planetary system

HD 168443 is known to be orbited by a super-Jupiter exoplanet, discovered in 1999, and a brown dwarf, discovered in 2001. The brown dwarf takes 30 times longer to orbit the star than the planet. [7] [8] [9] Both have eccentric orbits. [4] An orbital fit to Hipparcos astrometric data suggested the brown dwarf has a mass of 34±12  MJ . [9] A 2022 study utilizing both Hipparcos and Gaia data instead measured a true mass of 17.3 MJ for HD 168443 c, close to the minimum mass. [10] Test simulations of massless particles orbiting in between these two bodies show that all such objects are quickly ejected within two million years. That suggests any other planetary companions would be orbiting further out from the star. [11]

The HD 168443 planetary system [4] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥7.659±0.0975  MJ 0.2931±0.0018158.11247±0.00030.52883±0.00103——
c17.306+2.550
−0.906  MJ 		2.8373±0.0181,749.83±0.570.2113±0.0017191.218+22.283
−16.088 ° 		—

See also

Related Research Articles

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 114729 is a Sun-like star with an orbiting exoplanet in the southern constellation of Centaurus. Based on parallax measurements, it is located at a distance of 124 light years from the Sun. It is near the lower limit of visibility to the naked eye, having an apparent visual magnitude of 6.68 The system is drifting further away with a heliocentric radial velocity of 26.3 km/s. The system has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.373″·yr−1.

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 38529 is a binary star approximately 138 light-years away in the constellation of Orion.

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

HD 125612 is a binary star system with three exoplanetary companions in the equatorial constellation of Virgo. It is too dim to be visible to the naked eye, having an apparent visual magnitude of 8.31. The system is located at a distance of 188 light years from the Sun based on parallax measurements, but it is drifting closer with a radial velocity of −18 km/s.

HD 107148 is a wide binary star system in the constellation of Virgo. A pair of exoplanets have been confirmed in orbit around the brighter star. This system is located at a distance of 161 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of 25.2 K. Although having an absolute magnitude of 4.47, at that range the system is too faint to be visible with the naked eye, having an apparent visual magnitude of 8.01.

<span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

HD 136118 is a star in the Serpens Caput section of the Serpens constellation. The star is too dim to be readily visible to the naked eye, having an apparent visual magnitude of 6.93. It is located at a distance of 165 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −3 km/s.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

HD 195019 is a binary star system in the northern constellation of Delphinus. The brighter star has a close orbiting exoplanet companion. This system is located at a distance of 122 light years from the Sun based on parallax measurements, but it is drifting closer with a radial velocity of −91.3 km/s. Although it has an absolute magnitude of 4.01, at that distance the system is considered too faint to be viewed with the naked eye, having a combined apparent visual magnitude of 6.87. However, it should be readily visible with a pair of binoculars or a small telescope.

HD 72659 is a star in the equatorial constellation of Hydra. With an apparent visual magnitude of 7.46, his yellow-hued star is too faint to be viewed with the naked eye. Parallax measurements provide a distance estimate of 169.4 light years from the Sun, and it has an absolute magnitude of 3.98. The star is drifting closer with a radial velocity of −18.3 km/s.

HD 106252 is a star with a brown dwarf companion in the constellation Virgo. An apparent visual magnitude of 7.41 means this star is too faint to be visible to the naked eye. It is located at a distance of 210 light years from the Sun based on parallax measurements, and is receding with a radial velocity of 15 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 178911 is a triple star system with an exoplanetary companion in the northern constellation of Lyra. With a combined apparent visual magnitude of 6.70, it is a challenge to view with the naked eye. The system is located at a distance of approximately 161 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −38 km/s.

HD 183263 is a star with a pair of orbiting exoplanets located in the equatorial constellation of Aquila. It has an apparent visual magnitude of 7.86, which is too faint to be visible to the naked eye. The distance to this system is 178 light years based on parallax measurements, but it is drifting closer with a heliocentric radial velocity of −50 km/s. Judging from its motion through space, this star is predicted to approach to within 32 light-years of the Sun in around 952,000 years. At that distance, it will be faintly visible to the naked eye.

HD 190228 is a star with an orbiting substellar companion in the northern constellation of Vulpecula. Its apparent magnitude is 7.30 – too faint to be seen with the naked eye – and the absolute magnitude is 3.34. Based on parallax measurements, it is located at a distance of 205 light-years from the Sun. The system is drifting closer with a radial velocity of −50 km/s.

HD 115404 is a binary star system located in the constellation Coma Berenices. Parallax measurements made by Hipparcos put the system at 36 light-years, or 11 parsecs, away. The combined apparent magnitude of the system is 6.52, with the magnitudes of the components being 6.66 and 9.50.

BD+14 4559 is a star with an exoplanetary companion in the northern constellation of Pegasus. During the 2019 NameExoWorlds campaign, the star was named Solaris by Poland after a 1961 science fiction novel about an ocean-covered exoplanet by Polish writer Stanislaw Lem. With an apparent visual magnitude of 9.78, the star is too faint to be viewed with the naked eye. The system is located at a distance of 161 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −44 km/s. It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.234″ yr−1.

HD 29587 is a Sun-like star with a candidate brown dwarf companion in the northern constellation of Perseus. It has an apparent visual magnitude of 7.29, which means it is too faint to be viewed with the naked eye. Based upon an annual parallax shift of 36.3 mas, it is located 89.8 light years away. The star is moving away from the Earth with a heliocentric radial velocity of +113 km/s, having come to within 55.8 ly some 148,000 years ago. It is a hyper-velocity halo star moving at a rate of 170 km/s relative to the local standard of rest.

HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  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. 1 2 3 4 5 6 7 8 Pilyavsky, Genady; et al. (December 2011). "A Search for the Transit of HD 168443b: Improved Orbital Parameters and Photometry". The Astrophysical Journal. 743 (2): 8. arXiv: 1109.5166 . Bibcode:2011ApJ...743..162P. doi:10.1088/0004-637X/743/2/162. S2CID   13190486. 162.
  5. 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  6. ↑ "HD 168443". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-12-06.
  7. ↑ Marcy, Geoffrey W.; et al. (1999). "Two New Planets in Eccentric Orbits". The Astrophysical Journal. 520 (1): 239–247. arXiv: astro-ph/9904275 . Bibcode:1999ApJ...520..239M. doi:10.1086/307451. S2CID   16827678.
  8. ↑ Marcy, Geoffrey W.; et al. (2001). "Two Substellar Companions Orbiting HD 168443". The Astrophysical Journal. 555 (1): 418–425. Bibcode:2001ApJ...555..418M. doi: 10.1086/321445 .
  9. 1 2 Reffert, S.; Quirrenbach, A. (2006). "Hipparcos astrometric orbits for two brown dwarf companions: HD 38529 and HD 168443". Astronomy and Astrophysics. 449 (2): 699–702. Bibcode:2006A&A...449..699R. doi: 10.1051/0004-6361:20054611 . hdl: 1887/7483 .
  10. 1 2 Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series . 262 (21): 21. arXiv: 2208.12720 . Bibcode:2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57 . S2CID   251864022.
  11. ↑ Barnes, Rory; Raymond, Sean N. (December 2004). "Predicting Planets in Known Extrasolar Planetary Systems. I. Test Particle Simulations". The Astrophysical Journal. 617 (1): 569–574. arXiv: astro-ph/0402542 . Bibcode:2004ApJ...617..569B. doi:10.1086/423419. S2CID   12380925.
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.