HD 75289

Last updated
HD 75289
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vela
HD 75289 A
Right ascension 08h 47m 40.3896s [1]
Declination −41° 44′ 12.4563″ [1]
Apparent magnitude  (V)6.35 [2]
B
Right ascension 08h 47m 42.2616s [3]
Declination −41° 44′ 07.4408″ [3]
Apparent magnitude  (V)11.80 [4]
Characteristics
Evolutionary stage Main sequence
Spectral type G0V [2] + M2-M5V [5]
B−V color index 0.578 [2]
Astrometry
A
Radial velocity (Rv)+9.90±0.64 [6]  km/s
Proper motion (μ)RA: −20.509±0.051 [1]   mas/yr
Dec.: −227.945±0.054 [1]   mas/yr
Parallax (π)34.3167 ± 0.0281  mas [1]
Distance 95.04 ± 0.08  ly
(29.14 ± 0.02  pc)
Absolute magnitude  (MV)4.04 [2]
B
Proper motion (μ)RA: −13.817±0.194 [3]   mas/yr
Dec.: −229.657±0.230 [3]   mas/yr
Parallax (π)34.1784 ± 0.1208  mas [3]
Distance 95.4 ± 0.3  ly
(29.3 ± 0.1  pc)
Details [7]
A
Mass 1.141+0.020
−0.035  M☉
Radius 1.298±0.013  R☉
Luminosity 1.99 [2]   L☉
Surface gravity (log g)4.317±0.680  cgs
Temperature 6,184±43  K
Metallicity [Fe/H]0.32±0.08  dex
Rotation ~15.95 d [2]
Rotational velocity (v sin i)2.978±0.722 km/s
Age 4.410+0.757
−0.337  Gyr
B
Mass 0.135±0.003 [5]   M☉
Other designations
CD−41°4507, HD  75289, HIP  43177, HR  3497, SAO  220481, WDS J08477-4144, 2MASS J08474038-4144119 [8]
Database references
SIMBAD data

HD 75289 is a faint double star in the southern constellation of Vela. The primary component has a yellow hue and an apparent visual magnitude of 6.35. [2] Under exceptionally good circumstances it might be visible to the unaided eye; however, usually binoculars are needed. The pair are located at a distance of 95  light years from the Sun based on parallax, and are drifting further away with a radial velocity of +10 km/s. [6]

Contents

The brighter member, component A, is a G-type main-sequence star like the Sun with a stellar classification of G0V. In 1982 it was classified as a supergiant, but this proved erroneous. It has an age comparable to the Sun and is considered metal-rich, with a greater abundance of heavier elements compared to the Sun. [2] The star has 14% more mass than the Sun and a 30% greater girth. It is spinning with a projected rotational velocity of 3 km/s, [7] giving it a ~16 day rotation period. The star is radiating double [2] the luminosity of the Sun from its photosphere at an effective temperature of 6,184 K. [7]

In 2004, a co-moving stellar companion was identified, based on an earlier suggestion from 2001. Designated component B, this red dwarf star lies at an angular separation of 21.5″ , corresponding to a projected separation of 621  AU . However, the radial distance between the stars is unknown, so they are probably further apart. In any case, one revolution around the primary would take thousands of years to complete. The study that found the red dwarf also rules out any further stellar companions beyond 140 AU and massive brown dwarf companions from 400 AU up to 2,000 AU. [5]

Planetary system

In 1999 a exoplanet HD 75289 b with half the mass of Jupiter was detected orbiting the primary by radial velocity method. [2] This exoplanet is a typical hot Jupiter that takes only about 3.51 days to revolve at an orbital distance of 0.0482 AU.

The HD 75289 planetary system [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥0.456±0.010  MJ 0.047859±0.0000023.50916±0.000020.062±0.022——

See also

Related Research Articles

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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 142022 is a binary star system located in the southernmost constellation of Octans. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.70. The distance to this system is 112 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −10 km/s.

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.

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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 102 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 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 9578 is a candidate wide binary star system located at a distance of approximately 183 light-years from the Sun in the southern constellation of Sculptor. The main star must be viewed with binoculars or a telescope, as its low apparent visual magnitude of 8.35 is too faint to be viewed with the naked eye. The system is drifting closer to the Sun with a radial velocity of −4 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 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

HD 79498 is a double star in the northern constellation of Cancer. The primary component of this pair has an orbiting exoplanet companion. This star is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.05. The system is located at a distance of 159 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 20 km/s. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.2″·yr−1.

References

  1. 1 2 3 4 5 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 Udry, S.; et al. (2000). "The CORALIE survey for southern extra-solar planets II. The short-period planetary companions to HD 75289 and HD 130322". Astronomy and Astrophysics. 356 (2): 590–598. Bibcode: 2000A&A...356..590U . S2CID   2048031.
  3. 1 2 3 4 5 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.
  4. ↑ Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
  5. 1 2 3 Mugrauer, M.; et al. (2004). "A low-mass stellar companion of the planet host star HD 75289". Astronomy and Astrophysics. 425: 249–253. arXiv: astro-ph/0406108 . Bibcode: 2004A&A...425..249M . doi: 10.1051/0004-6361:20041009 .
  6. 1 2 Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi: 10.1086/430500 .
  7. 1 2 3 Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv: 1801.09698 . Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID   119107228. A76. Note: HARPS values used here.
  8. ↑ "HD 75289". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-10-06.
  9. ↑ Wittenmyer, Robert A.; et al. (2020). "Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society. 492 (1): 377–383. arXiv: 1912.01821 . Bibcode:2020MNRAS.492..377W. doi:10.1093/mnras/stz3436. S2CID   208617606.
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