51 Eridani

Johann Bayer gave the star its Bayer designation of c Eridani,^[12] using lowercase letters once he had exhausted all the letters of the Greek alphabet, in his 1603 star chart Uranometria.^[13] It was catalogued as 51 Eridani by John Flamsteed in 1725.^[14]

Located around 97 light-years distant, it shines with a luminosity approximately 5.72 times that of the Sun and has a surface temperature of 7,400 K. A cold debris disk has been detected with a likely inner border of 82 astronomical units (AU).^[15] A yellow-white main-sequence star of spectral type F0V, 51 Eridani is a member of the Beta Pictoris moving group and hence thought to be around 23 million years old.^[5] Somewhat more luminous than it should be for its surface temperature, 51 Eridani has also been classified as spectral type F0IV—a type corresponding to ageing stars that have used up their core hydrogen fuel and become subgiants; however, in this case it is a phenomenon of very young stars 5 to 30 million years old that have yet to settle on the main sequence.^[16]

Photometric measurements with the TESS space telescope show that this is a Gamma Doradus-like pulsating star. Nine pulsation frequencies have been detected.^[3]

51 Eridani b is a young Jupiter-like planet and was photographed, in near-infrared light, on 21 December 2014.^[17] The study, led by Bruce Macintosh, a professor of physics at Stanford University and confirmed by Christian Marois found that methane and water were abundant in the atmosphere of the planet and its diameter was only slightly larger than Jupiter's.^[11] It was assumed to be the least massive exoplanet directly imaged when discovered.^[18] The planetary orbit was found to be significantly eccentric by 2019.^[19]

Gaia astrometry also suggests an additional planet on orbit smaller than 51 Eridani b.^[19]