WASP-132

Last updated

WASP-132
Lupus IAU.svg
Red circle.svg
Approximate location of WASP-132 (circled)
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 [2]
Characteristics
Spectral type K4V [3]
J−H color index 0.512 [4]
J−K color index 0.583 [4]
Variable type Planetary transit variable
Astrometry
Radial velocity (Rv)31.55±0.45 [5]  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 [6]
Mass 0.782±0.034  M☉
Radius 0.753+0.028
−0.026  R☉
Luminosity 0.253+0.032
−0.028  L☉
Surface gravity (log g)4.576+0.028
−0.036  cgs
Temperature 4714+87
−88  K
Metallicity [Fe/H]0.18±0.12  dex
Rotation 33 d
Rotational velocity (v sin i)0.90±0.80 [6] or 3.3±0.6 [3]  km/s
Age 3.2±0.5 [6] or 7.2+4.3
−4.4 [3]   Gyr
Other designations
Gaia DR3  6099012478412247296, TOI-822, TIC  127530399, WASP-132, 2MASS J14302619-4609330
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 [7] as an orangish star.

Contents

Stellar characteristics

WASP-132 is a K-type main-sequence star with a spectral type of K4V, corresponding to its effective temperature of 4,714 K (4,441 °C; 8,026 °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 0.18±0.12 dex. Its age estimate varies wildly between publications from 3.2±0.5 Gyr [6] to 7.2+4.3
−4.4 Gyr. [3] The same goes for its rotational velocity, with presented values of 0.90±0.80  km/s [6] and 3.3±0.6 km/s. [3]

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

The WASP-132 planetary system [3] [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c6.26+1.84
−1.83  M🜨 		0.01833±0.000791.01153624+0.00000093
−0.00000086		—88.82+0.67
−0.69 ° 		1.841+0.094
−0.093  R🜨
b0.428±0.015  MJ 0.0674±0.00297.1335164±0.00000190.0163+0.069
−0.067		89.46+0.13
−0.11 ° 		0.901±0.038  RJ
d≥5.16±0.52  MJ 2.71±0.121816.6±44.40.120±0.078——

WASP-132b

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). [8]

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). [8]

WASP-132c

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 and subsequent observations with HARPS indicate that the mass of the planet is approximately 6.26+1.84
−1.83  M🜨 , corresponding to a bulk density of 5.47+1.96
−1.71 g⋅cm−3, consistent with an Earth-like composition. [3]

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 original 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. [6]

WASP-132d

In June 2024, an additional planet was reported to have been discovered in a 1,800-day (4.9-year) orbit with a semi-major axis of 2.71 AU, much farther out than the previous two planets and roughly where the main belt would be in the Solar System. This planet was discovered via doppler spectroscopy (aka the radial velocity method), through the analysis of CORALIE and HARPS radial velocity data, taking into account the Rossiter-McLaughlin effect caused by the other two planets. This planet has a minimum mass of 5.16 MJ, easily making it a super-Jupiter. [3]

Possible distant companion

In WASP-132d's discovery paper, also described is a linear trend in the CORALIE radial velocity curves, hinting at the existence of an object located even farther out. Should it exist, it would have a minimum mass of roughly 18.5 MJ, likely making it a brown dwarf or low-mass star, and orbit WASP-132 with a period of >18 years. [3]

See also

Related Research Articles

HD 169830 is a star in the southern constellation of Sagittarius. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.90. The star is located at a distance of 120 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −17.3 km/s, and is predicted to come as close as 20.7 ly (6.4 pc) in 2.08 million years. HD 169830 is known to be orbited by two large Jupiter-like exoplanets.

HD 216770 is a star with an orbiting exoplanet in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 8.11, it is too faint to be visible to the naked eye. It is located at a distance of 120 light years from the Sun, as determined by parallax measurements, and is drifting further away with a radial velocity of 31.1 km/s. The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.302 arcsec yr−1.

HD 179949 is a 6th magnitude star in the constellation of Sagittarius. It is a yellow-white dwarf, a type of star hotter and more luminous than the Sun. The star is located about 90 light years from Earth and might be visible under exceptionally good conditions to an experienced observer without technical aid; usually binoculars are needed.

Pi Mensae, also known as HD 39091, is a G-dwarf star in the constellation of Mensa. This star has a high proper motion. The apparent magnitude is 5.67, which can be visible to the naked eye in exceptionally dark, clear skies. It is nearly 60 light-years away. The star is slightly larger than the Sun in terms of mass, size, luminosity, temperature and metallicity, and is about 730 million years younger. It hosts three known planets.

<span class="mw-page-title-main">WASP-4b</span> Extrasolar planet in the constellation Phoenix

WASP-4b is an exoplanet, specifically a hot Jupiter, approximately 891 light-years away in the constellation of Phoenix.

HD 118203 is a star with an orbiting exoplanet located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.

<span class="mw-page-title-main">WASP-8</span> Star in the constellation of Sculptor

WASP-8 is a binary star system 294 light-years away. The star system is much younger than the Sun at 300 million to 1.2 billion years age, and is heavily enriched in heavy elements, having nearly twice the concentration of iron compared to the Sun.

WASP-15, also named Nyamien, is a magnitude 11 star located about 1000 light-years away in the constellation Centaurus. The star, which is more massive, larger, hotter, and more luminous than the Sun, is also less metal-rich than the Sun. WASP-15 has one known planet in its orbit, WASP-15b; the planet is a Hot Jupiter with an anomalously high radius, a phenomenon which may be explained by the presence of an internal heat source. The star was first observed by the SuperWASP program in 2006; future measurements in 2007 and 2008, as well as follow-up observations and analysis, eventually led to the discovery of WASP-15b using the transit method and Doppler spectroscopy.

WASP-18 is a magnitude 9 star located 400 light-years away in the Phoenix constellation of the southern hemisphere. It has a mass of 1.29 solar masses.

<span class="mw-page-title-main">HD 15082</span> Star in the constellation Andromeda

HD 15082 is a star located roughly 397 light years away in the northern constellation of Andromeda. The star is a Delta Scuti variable and a planetary transit variable. A hot Jupiter type extrasolar planet, named WASP-33b or HD 15082b, orbits this star with an orbital period of 1.22 days. It is the first Delta Scuti variable known to host a planet.

<span class="mw-page-title-main">WASP-43b</span> Extrasolar planet in the constellation Sextans

WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

WASP-43 is a K-type star about 284 light-years away in the Sextans constellation. It is about half the size of the Sun, and has approximately half the mass. WASP-43 has one known planet in orbit, a Hot Jupiter called WASP-43b. At the time of publishing of WASP-43b's discovery on April 15, 2011, the planet was the most closely orbiting Hot Jupiter discovered. The small orbit of WASP-43b is thought to be caused by WASP-43's unusually low mass. WASP-43 was first observed between January and May 2009 by the SuperWASP project, and was found to be cooler and slightly richer in metals than the Sun. WASP-43 has also been found to be an active star that rotates at a high velocity.

WASP-24 is an F-type star with the Hot Jupiter planet WASP-24b in orbit. WASP-24 is slightly larger and more massive than the Sun, it is also has a similar Metallicity and is hotter than the Sun. WASP-24 was first observed by the SuperWASP planet-searching organization, which flagged it as a potential host to a planet before following up with radial velocity and spectral measurements. Analysis of these confirmed the planetary nature of WASP-24b, which was later released to the public on the SuperWASP website.

WASP-44 is a G-type star about 1,180 light-years away in the constellation Cetus that is orbited by the Jupiter-size planet WASP-44b. The star is slightly less massive and slightly smaller than the Sun; it is also slightly cooler, but is more metal-rich. The star was observed by SuperWASP, an organization searching for exoplanets, starting in 2009; manual follow-up observations using WASP-44's spectrum and measurements of its radial velocity led to the discovery of the transiting planet WASP-44b. The planet and its star were presented along with WASP-45b and WASP-46b on May 17, 2011 by a team of scientists testing the idea that hot Jupiters tend to have circular orbits, an assumption that is made when the orbital eccentricity of such planets are not well-constrained.

HD 106515 is a binary star in the constellation of Virgo.

<span class="mw-page-title-main">Next-Generation Transit Survey</span> Ground-based robotic search for exoplanets

The Next-Generation Transit Survey (NGTS) is a ground-based robotic search for exoplanets. The facility is located at Paranal Observatory in the Atacama Desert in northern Chile, about 2 km from ESO's Very Large Telescope and 0.5 km from the VISTA Survey Telescope. Science operations began in early 2015. The astronomical survey is managed by a consortium of seven European universities and other academic institutions from Chile, Germany, Switzerland, and the United Kingdom. Prototypes of the array were tested in 2009 and 2010 on La Palma, and from 2012 to 2014 at Geneva Observatory.

WASP-47 is a star similar in size and brightness to the Sun about 881 light-years away in the constellation Aquarius. It lies within the Kepler K2 campaign field 3. It was first noticed to have a hot Jupiter exoplanet orbiting every 4 days in 2012 by the Wide Angle Search for Planets (WASP) team. While it was thought to be a typical hot Jupiter system, three more planets were found in 2015: an outer gas giant within the habitable zone, a hot Neptune exterior to the hot Jupiter's orbit and a super-Earth interior to the hot Jupiter's orbit. WASP-47 is the only planetary system known to have both planets near the hot Jupiter and another planet much further out.

HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

WASP-80 is a K-type main-sequence star about 162 light-years away from Earth. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 could be similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

References

  1. 1 2 3 4 5 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.
  2. ↑ "WASP-132 Overview". NASA Exoplanet Archive . Retrieved 21 October 2024.
  3. 1 2 3 4 5 6 7 8 9 Grieves, Nolan; Bouchy, François; Armstrong, David J.; Akinsanmi, Babatunde; Psaridi, Angelica; Ulmer-Moll, Solène; Frensch, Yolanda G. C.; Helled, Ravit; Müller, Simon; Knierim, Henrik; Santos, Nuno C.; Adibekyan, Vardan; Parc, Léna; Lendl, Monika; Battley, Matthew P. (1 January 2025). "Discovery of a cold giant planet and mass measurement of a hot super-Earth in the multi-planetary system WASP-132". Astronomy & Astrophysics. 693: A144. arXiv: 2406.15986 . doi:10.1051/0004-6361/202348177. ISSN   0004-6361.
  4. 1 2 "WASP-132". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 19 October 2024.
  5. ↑ 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.
  6. 1 2 3 4 5 6 7 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. arXiv: 2205.02501 . Bibcode:2022AJ....164...13H. doi: 10.3847/1538-3881/ac6f57 . ISSN   0004-6256.
  7. ↑ North, Gerald; James, Nick (2014). Observing Variable Stars, Novae and Supernovae. Cambridge University Press. p. 24. ISBN   978-1-107-63612-5.
  8. 1 2 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. arXiv: 1604.04195 . doi: 10.1093/mnras/stw3005 . ISSN   0035-8711.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.