82 G. Eridani d

Naming

The planets of 82 G. Eridani are named with lowercase letters in order of discovery, following the exoplanet naming convention. However, designations are inconsistent across sources due to a complex history of detections.

HD 20794 d originally referred to a different planet with a 90-day period, (Planet "e" is a candidate from 2017 that has not been supported by subsequent studies.)

Characteristics

82 G. Eridani d's existence was inferred solely on Doppler spectroscopy. A limitation of this method is that only a lower bound value in the mass can be obtained, assuming the orbital inclination relative to Earth is a right angle. Based on current data, 82 G. Eridani d's mass is at least six Earth masses; this value could be significantly higher if the planet is being viewed in an inclined orbit. This mass suggests the planet is likely a super-Earth, but does not rule out the possibility that it is a mini-Neptune, with no solid surface and a thick hydrogen/helium atmosphere, inhospitable to life. The true radius of the planet remains unknown, but estimates suggest if it is terrestrial it could be or so, and if it has a composition rich in volatiles it could be larger than .

82 G. Eridani d takes 650 day to complete an orbit around its sun. It is located at an average orbital distance of 1.35 AU, which would make it within the habitable zone (HZ), a region where water can exist in a liquid state. However, due to its eccentric orbit, the distance varies from 0.8 to 2.0 AU. At its longest separation from 82 G. Eridani, the apoastron, it orbits beyond the habitable zone, and the irradiaton received decreases by a factor of 7 compared to periastron. About 59% of its orbit is spent in the optimistic habitable zone, 34% is spent in the conservative HZ, and 3% outside the HZ. It is believed that water on the surface would freeze in the apoastron due to the low temperature.

Discovery and observations

The planet was first spotted in a radial velocity survey in 2023 by M. Cretignier and three other authors. The team observed five nearby Sun-like stars: Tau Ceti, HD 192310, 61 Virginis, HD 109200 and 82 G. Eridani. In 82 G. Eridani, they confirmed two planets with orbital periods of 18 and 89 days, which were already known to exist since 2011, and detected a periodic signal of 650 days, which could be the orbital period of another planet, in a more distant and eccentric orbit. The findings were published in August 2023, in the journal Astronomy and Astrophysics and the preprint repository arXiv. At that time 82 G. Erdani d was not confirmed.

The planet was confirmed in a follow-up study by N. Nari et al., which was published on October 15, 2024, about a year after the initial detection, also in the journal Astronomy and Astrophysics. The 650-day periodic signal was found to be the orbital period of planet d, and the same planets confirmed by Cretignier et al. were also detected. The confirmation was done by the doppler spectroscopy method, joining two-decade radial velocity observations from the HARPS and ESPRESSO spectrographs. The YARARA pipeline was then used to improve the quality of the HARPS observations.

Doppler spectroscopy, also known as the radial velocity method, consists on observing small variations in the spectrum of a star, which are radial velocity variations and happen because the planet is able to gravitationally pull its host star, making its motion in Earth's direction vary slightly. The spectral lines of the host star are observed to become redder (redshift) in half of the planet's orbit, when the host star is being pulled against Earth, and later to become bluer (blueshift) in the other half, when the host star is being pulled towards Earth. 82 G. Eridani d pulls its host star at a speed of 60 centimeters per second.

Host star

Main article: 82 G. Eridani

82 G. Eridani, also known as HD 20794 and e Eridani, is a nearby star visible to the unaided eye, as a faint point of light of apparent magnitude 4.25, in the constellation Eridanus. Its distance, inferred from its parallax shift, is , making it therefore one of the nearest stars.

The star has a spectral type of G8V, which is similar to the Sun's spectral type of G2V. The luminosity class "V" classifies 82 G. Eridani as a main sequence star fusing atoms of hydrogen into helium at its core. It is smaller and fainter than the Sun, with about 80% of the Sun's mass and 92% of the Sun's radius. It irradiates 60% of the solar luminosity from its photosphere at an effective temperature of 5470 K, giving it a yellow-white hue typical of late G-type stars.

It is a high-velocity starit is moving quickly compared to the averageand hence is a member of Population II, generally older stars whose motions take them well outside the plane of the Milky Way. Like many other Population II stars, 82 G. Eridani is somewhat deficient in metals (elements heavier than hydrogen and helium), though much less deficient than many, and is older than the Sun.

In addition to planet d, 82 G. Eridani also hosts two other planets in closer orbits: 82 G. Eridani b, which is a likely super-Earth with an orbital period of 18 days and a minimum mass of , and 82 G. Eridani c, also likely a super-Earth, with an orbital period of 89 days and a minimum mass of . All of them were discovered by doppler spectroscopy, with planets b and c being discovered in 2011 by F. Pepe et al.

Notes

References

References

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