HD 75289 is a faintdouble star in the southernconstellation ofVela. The primary component has a yellow hue and anapparent visual magnitude of 6.35.[2] Under exceptionally good circumstances it might be visible to the unaided eye; however, usuallybinoculars are needed. The pair are located at a distance of 95 light years from theSun based onparallax, and are drifting further away with aradial velocity of +10 km/s.[6]
The brighter member, component A, is aG-type main-sequence star like the Sun with astellar classification of G0V. In 1982 it was classified as asupergiant, but this proved erroneous. It has an age comparable to the Sun and is consideredmetal-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 aprojected rotational velocity of 3 km/s,[7] giving it a ~16 dayrotation period. The star is radiating double[2] theluminosity of the Sun from itsphotosphere at aneffective 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, thisred dwarf star lies at anangular separation of21.5″, corresponding to aprojected separation of621 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 massivebrown dwarf companions from 400 AU up to 2,000 AU.[5]
In 1999 aexoplanetHD 75289 b with half the mass ofJupiter was detected orbiting the primary byradial velocity method.[2] This exoplanet is a typicalhot Jupiter that takes only about 3.51 days to revolve at anorbital distance of 0.0482AU.
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.456±0.010 MJ | 0.047859±0.000002 | 3.50916±0.00002 | 0.062±0.022 | — | — |
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