HD 177565 b is an extrasolar planet orbiting the G-type main-sequence star HD 177565 55.3 light-years away from the Solar System.[3]
 An artist's impression of HD 177565 b orbiting its host star. | |
| Discovery[1] | |
|---|---|
| Discovered by | Feng, F. et. al. |
| Discovery site | La Silla Observatory |
| Discovery date | May 10, 2017 |
| Orbital characteristics[1] | |
| Periastron | 0.187 AU (28,000,000 km) |
| Apoastron | 0.305 AU (45,600,000 km) |
| 0.246 ± 0.019 AU (36,800,000 ± 2,800,000 km) | |
| Eccentricity | 0.059300+0.17170 −0.05745 |
| 44.505+0.586 −0.293 d | |
| 310°+46° −306° | |
| Semi-amplitude | 2.71+1.12 −0.99 km/s |
| Star | HD 177565 |
| Physical characteristics | |
| Mass | ≥15.10+6.40 −6.05 M🜨[1] |
| Temperature | 539 K (266 °C; 511 °F)[2] |
Nomenclature
editThe planet gets its name from its host star's Henry Draper Catalogue designation, HD 177565 and the "b" designation from being the first exoplanet detected in the system.
Discovery
editHD 177565 b was discovered by astronomer F. Feng and colleagues at the La Silla Observatory on May 10, 2017 by using doppler spectroscopy measurements from the High Accuracy Radial Velocity Planet Searcher spectrograph. Combining the radial velocity measurements from HD 177565 & HD 41248 and periodograms via the Athaga tool, the team was able to derive orbits for this planet and HD 41248 b and c.
Properties
editSince the planet was detected indirectly, its physical properties such as its radius and density cannot be observed. HD 177565 b takes 44.5 days to complete a relatively circular orbit at a separation of 0.246 AU, which is slightly lower compared to the planet Mercury's distance from the Sun. Its inclination and hence its true mass are also currently immeasurable, so only the minimum mass can be determined. HD 177565 b has a minimum mass 15.1 times the mass of Earth, making it a hot Neptune; it has an equilibrium temperature of 539 K.[2]
See also
editReferences
edit- ^ a b c Feng, F.; Tuomi, M.; Jones, H. R. A. (May 16, 2017). "Agatha: disentangling periodic signals from correlated noise in a periodogram framework". Monthly Notices of the Royal Astronomical Society. 470 (4). Oxford University Press (OUP): 4794–4814. arXiv:1705.03089. Bibcode:2017MNRAS.470.4794F. doi:10.1093/mnras/stx1126. ISSN 0035-8711. S2CID 73635720.
- ^ a b Mandell, Avi M.; Lustig-Yaeger, Jacob; Stevenson, Kevin B.; Staguhn, Johannes (October 5, 2022). "MIRECLE: Science Yield for a Mid-infrared Explorer-class Mission to Study Nontransiting Rocky Planets Orbiting the Nearest M Stars Using Planetary Infrared Excess". The Astronomical Journal. 164 (5). American Astronomical Society: 176. arXiv:2207.13727. Bibcode:2022AJ....164..176M. doi:10.3847/1538-3881/ac83a5. ISSN 0004-6256. S2CID 251135126.
- ^ 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.