rho CrB planetary system
rho CrB is a Sun-like main-sequence star of spectral type G0 V approximately 57.0 light-years from Earth (17.47 parsecs). It hosts 4 confirmed exoplanets.
Host star
- Name
- rho CrB
- Spectral type
- G0 V
- Effective temperature
- 5,817 K
- Mass
- 0.95 M☉ (solar masses)
- Radius
- 1.34 R☉ (solar radii)
- Distance
- 17.47 pc (57.0 ly)
- Hipparcos catalog
- HIP 78459
Confirmed planets (4)
| Planet | Class | Mass (M⊕) | Radius (R⊕) | Period (d) | Distance (AU) | Eq. temp (K) | Discovered |
|---|---|---|---|---|---|---|---|
| rho CrB e | Super-Earth | 3.79 | 1.77 | 12.95 | 0.1061 | — | 2023 |
| rho CrB b | Neptune-like | 347.39 | 13.70 | 39.84 | 0.2245 | 614 | 1997 |
| rho CrB c | Mini-Neptune | 28.20 | 5.78 | 102.19 | 0.4206 | 448 | 2016 |
| rho CrB d | Mini-Neptune | 21.60 | 4.94 | 282.20 | 0.8270 | — | 2023 |
The planets in detail
rho CrB e is a Super-Earth with about 1.77 Earth radii and 3.79 Earth masses. It orbits rho CrB at 0.1061 AU with a 12.9-day year, and no published equilibrium temperature. It was confirmed in 2023 via radial velocity (Doppler) measurements.
rho CrB b is a Neptune-like world with about 13.70 Earth radii and 347.39 Earth masses. It orbits rho CrB at 0.2245 AU with a 39.8-day year, bathed in 35× Earth's stellar flux, and a scorching equilibrium temperature of 614 K. It was confirmed in 1997 via radial velocity (Doppler) measurements.
rho CrB c is a Mini-Neptune with about 5.78 Earth radii and 28.20 Earth masses. It orbits rho CrB at 0.4206 AU with a 102-day year, bathed in 10× Earth's stellar flux, and a warm equilibrium temperature of 448 K. It was confirmed in 2016 via radial velocity (Doppler) measurements.
rho CrB d is a Mini-Neptune with about 4.94 Earth radii and 21.60 Earth masses. It orbits rho CrB at 0.8270 AU with a 282-day year, and no published equilibrium temperature. It was confirmed in 2023 via radial velocity (Doppler) measurements.
Discovery
The rho CrB system was first identified in 1997, with confirmation work continuing through 2023 using radial velocity (Doppler) measurements. Detection facilities: Lowell Observatory, Fred Lawrence Whipple Observatory, Multiple Observatories.
Observing from Earth
Exoplanets cannot be resolved visually with amateur telescopes — the host star's glare is overwhelming and even space-based direct imaging requires sophisticated coronagraphs. What you can observe is the host star itself at right ascension 240.2601°, declination 33.3002°. Use the 3D orrery above to inspect orbital geometry, planetary scale, and the habitable-zone overlay — the orbits are computed from the published Keplerian elements and animate at user-controlled time rates.
