Jupiter-Like exoplanet orbiting the star HD 154345 b
HD 154345 b
Planet HD 154345 b (min mass ~1 MJ) in the background with two hypothetical moons visible. Image was created with Celestia V1.41 using a custom map for the Planet and its moons
Wright et al. discovered the planet in March 2006 using the
radial velocity method to detect the small wobbling movement of the star caused by the
gravity of the planet. The discovery was published in May 2007.[1]
While the existence of HD 154345 b has been unclear due to the correlation of its orbital period with the star's activity cycle,[3] a study in 2021 further confirmed its planetary nature.[4] In 2023, the inclination and true mass of HD 154345 b were determined via
astrometry.[2]
Characteristics
The planet has a mass slightly greater than that of
Jupiter. It orbits its parent star at a distance of 4.18 AU. Its
orbital period is about 9.15 Earth years and its orbit is near-circular.[2] There are no interior planets of
minimum mass (m sini) greater than 0.3 Jupiter.[5] Jupiter-like planets with these orbital and system characteristics are unlikely to be perturbed from the star's inclination.[6] Since the star's inclination is known as around 50°, this would make the planet's most likely mass greater than Jupiter's mass but less than twice that mass.[7]
As such HD 154345 b is presumed to be a
gas giant "Jupiter twin".[5] Depending on composition the two planets may be around the same size, or HD 154345 b may be larger. This planet may also harbor a system of moons and rings.[citation needed]
^Wright, J. T. (October 2015). Boisse, I.; Demangeon, O.; Bouchy, F.; Arnold, L. (eds.). Twenty Years of Precise Radial Velocities at Keck and Lick Observatories. Proceedings of colloquium 'Twenty years of giant exoplanets' held at Observatoire de Haute Provence, France, October 5-9, 2015. Observatoire de Haute-Provence, Institut Pythéas. pp. 8–17.
arXiv:1603.08384.
Bibcode:
2015tyge.conf....8W.