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.[2] The star is drifting further away with a radial velocity of 10 km/s.[1] It has an absolute magnitude of +3.82.[5]
 Position of HR 858 in Fornax | |
| Observation data Epoch J2000.00 Equinox J2000.00 | |
|---|---|
| Constellation | Fornax |
| Right ascension | 02h 51m 56.246s[1] |
| Declination | −30° 48′ 52.26″[1] |
| Apparent magnitude (V) | 6.382[2] |
| Characteristics | |
| Evolutionary stage | F6V[3] + M[4] |
| Spectral type | Main sequence |
| B−V color index | +0.484[5] |
| Astrometry | |
| Radial velocity (Rv) | +9.77±0.12[1] km/s |
| Proper motion (μ) | RA: 123.435(25) mas/yr[1] Dec.: 105.996(37) mas/yr[1] |
| Parallax (π) | 31.5418 ± 0.0352 mas[1] |
| Distance | 103.4 ± 0.1 ly (31.70 ± 0.04 pc) |
| Absolute magnitude (MV) | +3.82[5] |
| Details[6] | |
| A | |
| Mass | 1.204±0.052 M☉ |
| Radius | 1.258±0.019 R☉ |
| Luminosity | 2.31±0.12 L☉ |
| Surface gravity (log g) | 4.30±0.06 cgs |
| Temperature | 6,354±70 K |
| Metallicity [Fe/H] | 0.025±0.050 dex |
| Rotation | 6.7±1.3 d |
| Rotational velocity (v sin i) | 7.5±0.2 km/s |
| Age | 2.0±0.6 Gyr |
| B | |
| Radius | 0.17±0.04[4] R☉ |
| Temperature | 2,800±300[4] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
This object is a slightly-evolved F-type main-sequence star with a stellar classification of F6V,[3] which indicates it is generating energy through core hydrogen fusion. It is roughly two[8] 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.[4]
A faint co-moving stellar companion, designated component B, at an angular separation of 8.4″. This corresponds to a projected separation of 270 AU. It is a red dwarf star.[4]
Planetary system
editIn 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,[4] measurements of their masses suggest that in terms of composition they may be better described as sub-Neptunes.[6] Planets 'b' and 'c' may be in a 3:5 mean-motion resonance.[4]
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.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 3.55+0.94 −0.96 M🜨 |
0.04888±0.00066 | 3.585287+0.000009 −0.000012 |
0 | 85.98+0.26 −0.25° |
2.004+0.045 −0.047 R🜨 |
| c | <3.8 M🜨 | 0.06870±0.00092 | 5.973865+0.000015 −0.000016 |
0 | 86.59+0.15 −0.14° |
1.979+0.054 −0.051 R🜨 |
| d | 7.1±1.6 M🜨 | 0.1046±0.0014 | 11.230511+0.000043 −0.000045 |
0 | 87.72+0.10 −0.11° |
2.001+0.063 −0.064 R🜨 |
Notes
editReferences
edit- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Høg, E.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ a b c d e f g h Vanderburg, Andrew; et al. (2019). "TESS Spots a Compact System of Super-Earths around the Naked-Eye Star HR 858". The Astrophysical Journal. 881 (1): L19. arXiv:1905.05193. Bibcode:2019ApJ...881L..19V. doi:10.3847/2041-8213/ab322d. S2CID 153311715.
- ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c d Bonfanti, A.; Amateis, I.; et al. (November 2024). "Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396". Astronomy & Astrophysics. arXiv:2411.14911.
- ^ "HR 858". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-04.
- ^ Pace, G. (March 2013). "Chromospheric activity as age indicator. An L-shaped chromospheric-activity versus age diagram". Astronomy & Astrophysics. 551: 4. arXiv:1301.5651. Bibcode:2013A&A...551L...8P. doi:10.1051/0004-6361/201220364. S2CID 56420519. L8.