WASP-61
In this article we are going to delve into the fascinating world of WASP-61. From its origins and evolution to its relevance in today's society, we will explore all the aspects that make WASP-61 a topic of interest and debate. We will learn about its different facets, its impact on our lives and its influence in the cultural and social sphere. Through a detailed analysis and a deep look, we will discover everything that WASP-61 has to offer and how it has marked a before and after in history. Get ready to immerse yourself in this exciting journey and discover all the facets that make WASP-61 a theme worth exploring.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lepus |
| Right ascension | 05h 01m 11.9187s[1] |
| Declination | −26° 03′ 14.9668″[1] |
| Apparent magnitude (V) | 12.49 |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | F7V |
| Astrometry | |
| Radial velocity (Rv) | 18.66[1] km/s |
| Proper motion (μ) | RA: 0.495[1] mas/yr Dec.: 3.169[1] mas/yr |
| Parallax (π) | 2.0176±0.0228 mas[1] |
| Distance | 1,620 ± 20 ly (496 ± 6 pc) |
| Details[2] | |
| Mass | 1.22±0.07 M☉ |
| Radius | 1.36±0.03 R☉ |
| Surface gravity (log g) | 4.21±0.21[3] cgs |
| Temperature | 6265±168[3] K |
| Metallicity | -0.38±0.11[3] dex |
| Rotational velocity (v sin i) | 10.3±0.5 km/s |
| Age | 3.8+1.8 −0.9 Gyr |
| Other designations | |
| Gaia DR2 2959177048983750016, TYC 6469-1972-1, 2MASS J05011191-2603149[4] | |
| Database references | |
| SIMBAD | data |
WASP-61 is a single F-type main-sequence star about 1560 light-years away. The star is likely younger than the Sun at approximately 3.8+1.8
−0.9 billion years. WASP-61 is depleted in heavy elements, having just 40% of the solar abundance of iron.[3]
Planetary system
In 2012 a transiting superjovian planet b was detected on a tight, circular orbit.[5] Its equilibrium temperature is 1565±35 K.[5]
The planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to 4.0+17.1
−18.4°.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 2.05+0.18 −0.17 MJ |
0.05146+0.00097 −0.00099 |
3.8559000±0.000003 | <0.074 | 89.35+0.45 −0.66[5]° |
1.41±0.22[7] RJ |
References
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b Bonomo, A. S.; et al. (2017), "The GAPS Programme with HARPS-N at TNG", Astronomy & Astrophysics, 602: A107, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- ^ a b c d Andreasen, D. T.; Sousa, S. G.; Tsantaki, M.; Teixeira, G. D. C.; Mortier, A.; Santos, N. C.; Suárez-Andrés, L.; Delgado-Mena, E.; Ferreira, A. C. S. (2017), "SWEET-Cat update and FASMA", Astronomy & Astrophysics, 600: A69, arXiv:1703.06671, Bibcode:2017A&A...600A..69A, doi:10.1051/0004-6361/201629967, S2CID 119534579
- ^ "WASP-61". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c Hellier, Coel; Anderson, D. R.; Collier Cameron, A.; Doyle, A. P.; Fumel, A.; Gillon, M.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Smith, A. M. S.; Southworth, J.; Triaud, A. H. M. J.; Udry, S.; West, R. G. (2012), "Seven transiting hot-Jupiters from WASP-South, Euler and TRAPPIST: WASP-47b, WASP-55b, WASP-61b, WASP-62b, WASP-63b, WASP-66b & WASP-67b", Monthly Notices of the Royal Astronomical Society, 426 (1): 739–750, arXiv:1204.5095, Bibcode:2012MNRAS.426..739H, doi:10.1111/j.1365-2966.2012.21780.x, S2CID 54713354
- ^ Brown, D. J. A.; Triaud, A. H. M. J.; Doyle, A. P.; Gillon, M.; Lendl, M.; Anderson, D. R.; Collier Cameron, A.; Hébrard, G.; Hellier, C.; Lovis, C.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Smalley, B. (2016), "Rossiter–Mc Laughlin models and their effect on estimates of stellar rotation, illustrated using six WASP systems", Monthly Notices of the Royal Astronomical Society, 464: 810–839, arXiv:1610.00600, doi:10.1093/mnras/stw2316
- ^ Stassun, Keivan G.; Collins, Karen A.; Gaudi, B. Scott (2016), "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes", The Astronomical Journal, 153 (3): 136, arXiv:1609.04389, Bibcode:2017AJ....153..136S, doi:10.3847/1538-3881/aa5df3, S2CID 119219062
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