HD 75289

HD 75289 B
Observation data; Epoch 2000 Equinox 2000
Constellation	Vela
Right ascension	8h 47m 42.24s
Declination	-41° 44' 7.70"
Apparent magnitude (V)	?
Distance	94.36? ly; (28.94? pc)
Spectral type	M2-M5 V
Other designations
	n/a

HD 75289
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Vela
Right ascension	08h 47m 40.3894s
Declination	–41° 44′ 12.452″
Apparent magnitude (V)	6.36
Characteristics
Spectral type	G0V
B−V color index	0.58
Astrometry
Radial velocity (Rv)	+14 km/s
Proper motion (μ)	RA: –20.50 mas/yr ; Dec.: –227.68 mas/yr
Parallax (π)	34.55 ± 0.56 mas
Distance	94 ± 2 ly ; (28.9 ± 0.5 pc)
Absolute magnitude (MV)	4.05
Details
Mass	1.05 M☉
Radius	1.25 R☉
Luminosity	1.82 L☉
Surface gravity (log g)	4.25 cgs
Temperature	6011 K
Metallicity	0.29
Rotation	~24.6
Age	4.96 years
Other designations
	CD-41° 4507, HIP 43177, HR 3497, GC 12153 , SAO 220481

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.

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.^[1] 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^[2]
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
b	>0.467 ± 0.041 $M$ _J	0.0482 ± 0.0028	3.509267 ± 0.000064	0.034 ± 0.029	—	—

HD 75289 B

HD 75289 B is a possible 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.

References

^ 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.
^ 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.

External links

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[Udry2000-1] 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.

[Butler2006-2] 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.

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