HD 5388

Last updated
HD 5388
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Phoenix
Right ascension 00h 55m 11.88995s [1]
Declination –47° 24′ 21.4763″ [1]
Apparent magnitude  (V)6.73 [2]
Characteristics
Evolutionary stage main sequence
Spectral type F6V [2]
Apparent magnitude  (B)7.73 [3]
Apparent magnitude  (J)5.795 [4]
Apparent magnitude  (H)5.524 [4]
Apparent magnitude  (K)5.441 [4]
B−V color index 0.500 [2]
Astrometry
Radial velocity (Rv)+39.40±0.16 [1]  km/s
Proper motion (μ)RA: −80.390 [1]   mas/yr
Dec.: −178.132 [1]   mas/yr
Parallax (π)18.8155 ± 0.0268  mas [1]
Distance 173.3 ± 0.2  ly
(53.15 ± 0.08  pc)
Absolute magnitude  (MV)3.10 [2]
Details [2]
Mass 1.21  M☉
Radius 1.87+0.03
−0.04 [1]   R☉
Luminosity 4.770+0.012
−0.011 [1]   L☉
Surface gravity (log g)4.28±0.06  cgs
Temperature 6,297±32  K
Metallicity [Fe/H]−0.27±0.02  dex
Rotation 23 days
Rotational velocity (v sin i)4.2 km/s
Age 5.5±0.5 [5]   Gyr
Other designations
78 G. Phoenicis, CD–48°216, HD  5388, HIP  4311, SAO  215291, PPM  305379, LTT  4311, NLTT  3057 [6]
Database references
SIMBAD data
Exoplanet Archive data
Extrasolar Planets
Encyclopaedia 		data

HD 5388 is a single [7] star in the southern constellation of Phoenix. It has the Gould designation 78 G. Phoenicis, [8] while HD 5388 is the star's Henry Draper Catalogue identifier. This object has a yellow-white hue and is too faint to be readily visible to average human eyesight, having an apparent visual magnitude of 6.73. [2] It is located at a separation of 173  light years from the Sun based on parallax, and is drifting further away with a radial velocity of +39 km/s. [1]

This object is an ordinary F-type main-sequence star with a stellar classification of F6V, [2] indicating that it is generating energy through core hydrogen fusion. It is not chromospherically active and its metal content is half as much as the Sun. The star is larger and more massive than the Sun, [2] and radiates 4.8 [1] times the Sun's luminosity from its photosphere at an effective temperature of 6297 K. [1]

In 2009, a substellar object (HD 5388 b) thought to be a gas giant planet was detected in orbit around the star using the HARPS instrument at La Silla Observatory. [2] This was later demonstrated to be a brown dwarf rather than a planet. It has an elliptical orbit with a period of 2.13 years. [9]

The HD 5388 planetary system [2] [9] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b87.02+13.99
−10.80  MJ 		1.76777±40.40±0.021.356+0.195
−0.191 ° 		—

See also

Related Research Articles

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HD 114762 is a triple star system approximately 125 light-years (38.2 pc) away in the constellation Coma Berenices. It consists of a yellow-white F-type main-sequence star (HD 114762 A) and two red dwarf companions (HD 114762 Ab & HD 114762 B) approximately 0.36 & 130 AU distant. Both are low-metal subdwarfs. Planets around such metal-poor stars are rare. A telescope or strong binoculars are needed to view the primary. HD 114762 had been used by scientists as a "standard star", one whose radial velocity is well established, but with the discovery of the spectroscopic companion HD 114762 Ab its usefulness as a standard has been called into question.

HD 17092 is a star in the constellation of Perseus. It has an orange hue but is visible only with binoculars or better equipment, having an apparent visual magnitude of 7.73. The distance to this star is approximately 750 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +5.5 km/s.

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.7 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

HD 81040 is a star in the equatorial constellation of Leo. With an apparent visual magnitude of +7.73 it is too dim to be visible to the naked eye but can be viewed with a small telescope. The star is located at a distance of 112 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +49 km/s, having come to within 48 light-years some 527,000 years ago.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 138 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

HD 4113 is a dual star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88. The distance to this star, as estimated by parallax measurements, is 137 light years. It is receding away from the Sun with a radial velocity of +5 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 141937 is a star in the southern zodiac constellation of Libra, positioned a couple of degrees to the north of Lambda Librae. It is a yellow-hued star with an apparent visual magnitude of 7.25, which means it is too faint to be seen with the naked eye. This object is located at a distance of 108.9 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −2.2 km/s. It has an absolute magnitude of 4.71.

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.

HD 224635 and HD 224636 is a pair of stars comprising a binary star system in the constellation Andromeda. They are located approximately 94 light years away and they orbit each other every 717 years.

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 16760 is a binary star system approximately 227 light-years away in the constellation Perseus. The primary star HD 16760 is a G-type main sequence star similar to the Sun. The secondary, HIP 12635 is 1.521 magnitudes fainter and located at a separation of 14.6 arcseconds from the primary, corresponding to a physical separation of at least 660 AU. Announced in July 2009, HD 16760 has been confirmed to have a red dwarf orbiting it, formerly thought to be a brown dwarf or exoplanet.

HD 181720 is an 8th-magnitude G-type main sequence star located approximately 190 light-years away in the constellation Sagittarius. This star is larger, hotter, brighter and less massive than the Sun. Also its metal content is three-tenths as much as the Sun.

HD 6718 is a solar twin star in the equatorial constellation of Cetus. It has a yellow hue but is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.45. The distance to this object, as determined from parallax measurements, is 168 light years. It is drifting away from the Sun with a radial velocity of +35 km/s.

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 129445 is a G-type star found in the Circinus constellation located 219 light-years away from the Sun based on parallax. It is invisible to the naked eye with an apparent visual magnitude of 8.80. The star was observed by the Magellan Planet Search Program due to its absolute visual magnitude and high metallicity. The Magellan program conducted 17 doppler velocity measurements, which spans a full orbital period. The results led the program to detect a planet dubbed HD 129445 b. In 2023, the inclination and true mass of HD 129445 b were determined via astrometry.

HD 79498 is a primary of the star system located 159 light years away in the constellation Cancer. This G5 main sequence star has an apparent magnitude of 8.0 and is about the same size and mass as the Sun. It has a higher than solar abundance of elements other than hydrogen and helium; what astronomers term a metal-rich star.

Gliese 3512 is a nearby star in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye but can be observed using a telescope, having an apparent visual magnitude of +15.05. The star is located at a distance of 31 light-years from the Sun based on parallax. It has a high proper motion, traversing the celestial sphere at the rate of 1.311″ yr−1. The measurement of the star's radial velocity is poorly constrained, but it appears to be drifting further away at a rate of ~8 km/s.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 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.
  2. 1 2 3 4 5 6 7 8 9 10 Santos, Nuno C.; Mayor, Michel; Benz, Willy; Bouchy, François; et al. (2010). "The HARPS Search for Southern Extra-solar Planets XXI. Three New Giant Planets Orbiting the Metal-poor Stars HD 5388, HD 181720, and HD 190984". Astronomy and Astrophysics. 512 (A47): A47. arXiv: 0912.3216 . Bibcode:2010A&A...512A..47S. doi:10.1051/0004-6361/200913489. S2CID   118675798.
  3. ↑ Høg, E.; et al. (2000). The Tycho-2 catalogue of the 2.5 million brightest stars. Astronomy and Astrophysics. Vol. 355. pp. L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN   978-0333750889.
  4. 1 2 3 Cutri, R. M.; et al. (June 2003). 2MASS All Sky Catalog of point sources. NASA/IPAC. Bibcode:2003tmc..book.....C.
  5. ↑ Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv: 1411.4302 . Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID   54555839.
  6. ↑ "HD 5388". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-11-06.
  7. ↑ Tokovinin, Andrei (2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 87. arXiv: 1401.6827 . Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87. S2CID   56066740.
  8. ↑ Gould, Benjamin Apthorp. "Uranometria Argentina". Archived from the original on 2012-02-27. Retrieved 2019-11-06.
  9. 1 2 Sahlmann, J.; et al. (2011). "HD 5388 b is a 69 MJup companion instead of a planet". Astronomy and Astrophysics Letters. 528. L8. arXiv: 1102.3372 . Bibcode:2011A&A...528L...8S. doi:10.1051/0004-6361/201116533. S2CID   55566004.
  10. ↑ Kiefer, F.; et al. (January 2021). "Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets". Astronomy & Astrophysics. 645 A7. arXiv: 2009.14164 . Bibcode: 2021A&A...645A...7K . doi: 10.1051/0004-6361/202039168 . S2CID   221995447.

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