Star in the constellation Fornax
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! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.00      Equinox J2000.00
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Evolutionary stage
! style="text-align:left" | Spectral type
! style="text-align:left" | B−V 
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HR 858 (also known as HD 17926 or TOI-396) is a star with a planetary system located 103 light-years from the Sun in the southern constellation of Fornax. It has a yellow-white hue and is visible to the naked eye, but it is a challenge to see with an apparent visual magnitude of 6.4. The star is drifting further away with a radial velocity of 10 km/s. It has an absolute magnitude of +3.82.
This object is a slightly-evolved F-type main-sequence star with a stellar classification of F6V, which indicates it is generating energy through core hydrogen fusion. It is roughly two billion years old and is spinning with a projected rotational velocity of 8.3 km/s. The star has 1.1 times the mass of the Sun and 1.3 times the Sun's radius. It is radiating 2.3 times the luminosity of the Sun from its photosphere at an effective temperature of 6,201 K.
A faint co-moving stellar companion, designated component B, at an angular separation of . This corresponds to a projected separation of . It is a red dwarf star.
Planetary system.
In May 2019, HR 858 was announced to have at least 3 exoplanets as observed by the transit method with the Transiting Exoplanet Survey Satellite. All three are orbiting close to the host star and are close in size, each about twice the radius of the Earth. Described as super-Earths by their discovery paper, measurements of their masses suggest that in terms of composition they may be better described as sub-Neptunes. Planets 'b' and 'c' may be in a 3:5 mean-motion resonance.
Further research measured the masses of the planets b and d using accurate radial velocities, giving masses of 3.55 and 7.1 ME as well as planetary densities of 2.44 and 4.9 g/cm3. The system displays significant transit timing variations. The mass of planet c could not be measured using radial velocities, but it is constrained to be less than 3.8 ME, and a not very reliable value of 2.24 ME was measured using TTVs.
! align=center| Companion
! align=center| Mass
! align=center| Semimajor axis
! align=center| Orbital period
! align=center| Eccentricity
! align=center| Inclination
! align=center| Radius
References.
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