HD 147018

HD 147018 is a star in the southern constellation of Triangulum Australe. It has a yellow-orange hue with an apparent visual magnitude of 8.30, which is too faint to be seen with the naked eye but can be viewed with a small telescope. The star is located at a distance of 132 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −27.5 km/s.

The stellar classification of HD 147018 is G8/K0V or G9V, matching a late G-type main-sequence star that is generating energy through core hydrogen fusion. It is roughly six billion years old and is spinning with a projected rotational velocity of 1.56 km/s. The star has 93% of the mass of the Sun and 94% of the Sun's radius. The metallicity, or abundance of heavier elements, is higher than in the Sun. The star is radiating 71% of the luminosity of the Sun from its photosphere at an effective temperature of 5,441 K.

In August 2009, two extrasolar planets, HD 147018 b and HD 147018 c, were reported to be orbiting this star. The planets were found using the radial velocity method, using the CORALIE spectrograph at La Silla Observatory, Chile.