HIP 67522
(Redirected from HIP 67522 c)
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus[1] |
| Right ascension | 13h 50m 06.280s[2] |
| Declination | −40° 50′ 08.88″[2] |
| Apparent magnitude (V) | 9.80±0.03[3] |
| Characteristics | |
| Evolutionary stage | Main sequence[4] |
| Spectral type | G0V[5] |
| Astrometry | |
| Radial velocity (Rv) | 8.26±2.19[2] km/s |
| Proper motion (μ) | RA: −28.907 mas/yr[2] Dec.: −22.248 mas/yr[2] |
| Parallax (π) | 8.0170±0.0182 mas[2] |
| Distance | 406.8 ± 0.9 ly (124.7 ± 0.3 pc) |
| Details[4] | |
| Mass | 1.22±0.05 M☉ |
| Radius | 1.38±0.06 R☉ |
| Luminosity | 1.75±0.09 L☉ |
| Temperature | 5,675±75 K |
| Rotation | 1.418±0.016 days |
| Rotational velocity (v sin i) | 54.2±0.7 km/s |
| Age | 17±2 Myr |
| Other designations | |
| CD−40 8189, HD 120411, HIP 67522, TOI-6551, TIC 166527623[6] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HIP 67522 is a G-class star which, by comparison with the Sun, is slightly larger (1.38 R☉) and cooler (5,675 K versus 5,772 K for the Sun). It lies 407 light-years (125 parsecs) away in the constellation Centaurus. Its visual magnitude of 9.8 makes it much too faint to be seen by the unaided eye.[4]
Two exoplanets, HIP 67522 b and HIP 67522 c, are known to orbit the star and transit its face as seen from Earth. Their orbital periods are much less than Mercury's 88 days around the Sun, being 6.96 days for b and 14.33 days for c.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.0748+0.0016 −0.0018 |
6.9594731(22) | 0.064+0.187 −0.049 |
89.88+1.08 −0.93° |
0.891+0.021 −0.02 RJ |
| c | — | 0.1228+0.0042 −0.0053 |
14.334892(12) | 0.077+0.195 −0.056 |
89.2+1.75 −0.64° |
0.708+0.031 −0.032 RJ |
References
[edit]- ^ 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.
- ^ a b c d e 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.
- ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355. Bibcode:2000A&A...355L..27H.
- ^ a b c Rizzuto, Aaron C.; et al. (13) (22 June 2020). "TESS Hunt for Young and Maturing Exoplanets (THYME). II. A 17 Myr Old Transiting Hot Jupiter in the Sco-Cen Association". The Astronomical Journal. 160 (1): 33. arXiv:2005.00013. Bibcode:2020AJ....160...33R. doi:10.3847/1538-3881/ab94b7.
- ^ Torres, C. A. O.; Quast, G. R.; Da Silva, L.; de la Reza, R.; Melo, C. H. F.; Sterzik, M. (2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics. 460 (3): 695. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602.
- ^ "HIP 67522". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-12-22.
- ^ "HIP 67522 Overview".
- ^ Barber, Madyson G.; Thao, Pa Chia; et al. (September 2024). "TESS Investigation—Demographics of Young Exoplanets (TI-DYE). II. A Second Giant Planet in the 17 Myr System HIP 67522". The Astrophysical Journal Letters. 973 (1): L30. arXiv:2407.04763. Bibcode:2024ApJ...973L..30B. doi:10.3847/2041-8213/ad77d9.
