HD 75289

HD 75289 is a 6th magnitude star in the constellation of Vela. Like our Sun, it is a yellow dwarf but slightly more massive, hotter and luminous. The spectral type of the star is G0 V. Under exceptionally good circumstances it might be visible to the unaided eye; however, usually binoculars are needed.

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) 6.36
HD 75289 B
Right ascension  08h 47m 42.2616s[2]
Declination −41° 44′ 07.4408″[2]
Apparent magnitude (V)
Characteristics
Spectral type G0V + M2-M5V
B−V color index 0.58
Astrometry
HD 75289 A
Radial velocity (Rv)+14 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[1] mas
Distance95.04 ± 0.08 ly
(29.14 ± 0.02 pc)
Absolute magnitude (MV)4.05
HD 75289 B
Proper motion (μ) RA: −13.817±0.194[2] mas/yr
Dec.: −229.657±0.230[2] mas/yr
Parallax (π)34.1784 ± 0.1208[2] mas
Distance95.4 ± 0.3 ly
(29.3 ± 0.1 pc)
Details
Mass1.05 M☉
Radius1.25 R☉
Luminosity1.82 L☉
Surface gravity (log g)4.25 cgs
Temperature6011 K
Metallicity0.29
Rotation~24.6
Age4.96 years
Other designations
CD−41° 4507, HIP 43177, HR 3497, SAO 220481[3]
Database references
SIMBADdata

In 2004, a possible red dwarf companion was detected.

Planetary system

In 1999 a planet HD 75289 b with half the mass of Jupiter was detected by radial velocity method.[4] This planet 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[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >0.467 ± 0.041 MJ 0.0482 ± 0.0028 3.509267 ± 0.000064 0.034 ± 0.029 — —

HD 75289 B

HD 75289 B is a red dwarf star orbiting HD 75289. The stars share the same proper motion so they are probably related. Apparent distance between the two stars is about 21.5 arcseconds, at a distance of 94 light years that would be 621 astronomical units. 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 2000 AU.[6]

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References
  1. 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. 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.
  3. "HD 75289". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-06.
  4. 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.
  5. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
  6. 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.


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