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HD 141399

4 Apr 2019, 08:12 UTC
HD 141399

HD 141399 is an extrasolar system located 118 ligh-years away in the constellation Böotes. It is made of one star and four giant planets detected by radial velocity.
The central star is a slightly evolved orange dwarf (spectral type K0V), with a similar mass as the Sun (1.07 solar masses) but a larger radius (1.46 solar radii) and a slightly lower temperature (5330 °C, compared to 5500 °C for the Sun). It is therefore similar to what the Sun will be in about 5-6 billion years. With a magnitude of 7.2, it can be seen with binoculars.
The innermost planet, HD141399 b, has a minimum mass of 0.45 Jupiter masses, i.e 1.5 times Saturn’s mass. It has an orbital period of 94 days and a semi-major axis of 0.415 au (1 au = the Sun-Earth distance), i.e. an orbit similar to Mercury’s one (88 days and 0.38 au).
The second planet, HD 141399 c, has a minimum mass of 1.33 Jupiter mass. It has an orbital period of 202 days and a semi-major axis of 0.69 au, i.e. an orbit similar to Venus’s one (224.7 days and 0.73 au).
The third planet has a mass of 1.18 Jupiter masses. It has an orbital period of 1070 days and a semi-major axis of 2.09 au, that would place it just at the inner limit of the main asteroid belt between Mars and Jupiter if it were in the Solar System.
Finally, the outermost planet, HD 141399 e, has a minimum mass of two third of Jupiter’s mass, i.e. about twice the mass of Saturn. Its orbital period and semi-major axis are poorly constrained (~3000-5600 days, ~3.5-6.5 au), but are comparable to those of Jupiter.

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