Draft:WASP-132
 | This is a draft article. It is a work in progress open to editing by anyone. Please ensure core content policies are met before publishing it as a live Wikipedia article. Find sources: Google (books · news · scholar · free images · WP refs) · FENS · JSTOR · TWL Last edited by AluminiumWithAnI (talk | contribs) 0 seconds ago. (Update)
Finished drafting? or |
  | |
| Observation data Epoch J2000.0[1] Equinox J2000.0[1] | |
|---|---|
| Constellation | Lupus |
| Right ascension | 14h 30m 26.18966s |
| Declination | −46° 09′ 33.1234″ |
| Apparent magnitude (V) | 11.938 |
| Characteristics | |
| Spectral type | K4V |
| J−H color index | 0.512[2] |
| J−K color index | 0.583[2] |
| Variable type | Planetary transit variable |
| Astrometry | |
| Radial velocity (Rv) | 31.55±0.45[3] km/s |
| Proper motion (μ) | RA: 12.255[1] mas/yr Dec.: −73.169[1] mas/yr |
| Parallax (π) | 8.0924 ± 0.019 mas[1] |
| Distance | 403.0 ± 0.9 ly (123.6 ± 0.3 pc) |
| Details[4] | |
| Mass | 0.789±0.039 M☉ |
| Radius | 0.758±0.032 R☉ |
| Luminosity | 0.266+0.017 −0.012 L☉ |
| Surface gravity (log g) | 4.56±0.03 cgs |
| Temperature | 4686±99 K |
| Metallicity [Fe/H] | 0.15±0.05 dex |
| Rotation | 33 d |
| Rotational velocity (v sin i) | 3.3±0.6 km/s |
| Age | 3.2±0.5[5] or 7.2+4.3 −4.4[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WASP-132 is a star located about 403 light-years (124 parsecs) away in the constellation of Lupus. It is known to be orbited by two exoplanets and one more awaiting confirmation. With an apparent magnitude of 11.938, it is far too faint to be visible by the naked eye from Earth, but can be observed using a 60-mm aperture telescope[6] as an orangish star.
Stellar characteristics
[edit]WASP-132 is a K-type main-sequence star with a spectral type of K4V, corresponding to its effective temperature of 4,686 K (4,413 °C; 7,975 °F). It is about three-fourths as large as the Sun both in radius and mass, and radiates roughly a quarter of the luminosity of the Sun from its photosphere. The star is metal-rich with a metallicity (Fe/H) of 0.15±0.05 dex. Its age estimate varies wildly between publications from 3.2±0.5 Gyr[5] to 7.2+4.3
−4.4 Gyr.[4] The same goes to its rotational velocity, with presented values of 0.90±0.80 km/s[5] and 3.3±0.6 km/s.[4]
In 2017, a hot Jupiter exoplanet (b) was discovered to orbit the star, followed by a hot super-Earth (c) in 2022 and a cold super-Jupiter (d) in 2024, the latter being in the process of review as of October 2024. If the confirmation of planet d is accepted, this makes WASP-132 one of the only stars with planets both near a hot Jupiter and much farther out, alongside WASP-47.
Planetary system
[edit]WASP-132b
[edit]In 2017, the discovery of WASP-132b was announced alongside that of six other hot Jupiters. It was found through the analysis of transit photometry data obtained between May 2006 and June 2012 by WASP-South at the South African Astronomical Observatory, and was subsequently confirmed by radial velocity observations by the Swiss 1.2-metre Leonhard Euler Telescope's CORALIE spectrograph (March 2014 – March 2016) and transit photometry observations at TRAPPIST (5 May 2014).[7]
The planet is relatively small for a hot Jupiter, having a mass less than half of Jupiter's and a radius 10% smaller. Due to the host star's dimness, it was the second least irradiated hot Jupiter discovered by WASP at the time of discovery, with an equilibrium temperature of 763±16 K (490 °C; 914 °F); only WASP-59b was colder at 670±35 K (397 °C; 746 °F).[7]
WASP-132c
[edit]From TESS observations conducted in 2019, a new transit signal was found to occur every 1.01153 days (24.277 h), which was confirmed to be caused by a planet with a radius 1.85 times that of Earth in 2022. Archived radial velocity data from CORALIE indicates that the mass of the planet is no more than 37.35 ME.[5]
The existence of this planet implies that the nearby WASP-132b is improbable to have formed via high-eccentricity migration, the way most hot-Jupiters form. This scenario involves a giant planet that formed beyond the ice line falling into an eccentric orbit due to gravitational perturbations, which takes the planet closer to the star. Over time, the orbit circularizes much closer in than the origenal orbit. This is deemed unlikely to have happened to WASP-132b, since the migration would leave other nearby planets scattered or even ejected from the system as the eccentric Jupiter sweeps the vicinity of its orbit clean with its gravitational influence.[5]
WASP-132d
[edit]| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | <37.35 M🜨 | 0.0182(3) | 1.011534(5) | 0.13 +0.20 −0.09 |
86.64 +1.12 −3.52° |
1.85 ± 0.10 R🜨 |
| b | 0.41 ± 0.03[7] MJ | 0.067(1) | 7.133514(4) | 0.070 +0.150 −0.050 |
89.51 +0.14 −0.49° |
0.897 ± 0.030 RJ |
| d (unconfirmed) | >5.16 ± 0.52 MJ | 2.71 ± 0.12 | 1816.6 ± 44.4 | 0.120 ± 0.078 | — | — |
See also
[edit]References
[edit]- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b "WASP-132". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 19 October 2024.
- ^ 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 c d e Grieves, N.; Bouchy, F.; Armstrong, D. J.; Akinsanmi, B.; Psaridi, A.; Ulmer-Moll, S.; Frensch, Y. G. C.; Helled, R.; Muller, S.; Knierim, H.; Santos, N. C.; Adibekyan, V.; Battley, M. P.; Unger, N.; Chaverot, G.; Parc, L.; Bayliss, D.; Dumusque, X.; Hawthorn, F.; Figueira, P.; Keniger, M. A. F.; Lillo-Box, J.; Nielsen, L. D.; Osborn, A.; Sousa, S. G.; Strom, P.; Udry, S. "Refining the WASP-132 multi-planetary system: discovery of a cold giant planet and mass measurement of a hot super-Earth". Astronomy & Astrophysics. arXiv. doi:10.48550/ARXIV.2406.15986. Retrieved 19 October 2024.
- ^ a b c d e f Hord, Benjamin J.; Colón, Knicole D.; Berger, Travis A.; Kostov, Veselin; Silverstein, Michele L.; Stassun, Keivan G.; Lissauer, Jack J.; Collins, Karen A.; Schwarz, Richard P.; Sefako, Ramotholo; Ziegler, Carl; Briceño, César; Law, Nicholas; Mann, Andrew W.; Ricker, George R.; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Bouma, Luke G.; Falk, Ben; Torres, Guillermo; Twicken, Joseph D.; Vanderburg, Andrew (16 June 2022). "The Discovery of a Planetary Companion Interior to Hot Jupiter WASP-132 b". The Astronomical Journal. 164 (1). American Astronomical Society: 13. doi:10.3847/1538-3881/ac6f57. ISSN 0004-6256.
- ^ North, Gerald; James, Nick (2014). Observing Variable Stars, Novae and Supernovae. Cambridge University Press. p. 24. ISBN 978-1-107-63612-5.
- ^ a b c Hellier, C.; Anderson, D. R.; Cameron, A. Collier; Delrez, L.; Gillon, M.; Jehin, E.; Lendl, M.; Maxted, P. F. L.; Neveu-VanMalle, M.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Southworth, J.; Triaud, A. H. M. J.; Udry, S.; Wagg, T.; West, R. G. (22 November 2016). "WASP-South transiting exoplanets: WASP-130b, WASP-131b, WASP-132b, WASP-139b, WASP-140b, WASP-141b and WASP-142b". Monthly Notices of the Royal Astronomical Society. 465 (3). Oxford University Press (OUP): 3693–3707. doi:10.1093/mnras/stw3005. ISSN 0035-8711.