Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Indus |
Right ascension | 21h 14m 56.85987s [1] |
Declination | −55° 52′ 18.4581″ [1] |
Apparent magnitude (V) | 12.9 [2] |
Characteristics | |
Spectral type | G6V [2] |
Astrometry | |
Radial velocity (Rv) | −3.28±1.62 [1] km/s |
Proper motion (μ) | RA: 12.521 mas/yr [1] Dec.: -16.150 mas/yr [1] |
Parallax (π) | 2.6878 ± 0.0131 mas [1] |
Distance | 1,213 ± 6 ly (372 ± 2 pc) |
Details [3] | |
Mass | 0.828±0.067 M☉ |
Radius | 0.858±0.024 R☉ |
Surface gravity (log g) | 4.489±0.013 [4] cgs |
Temperature | 5600±150 K |
Metallicity [Fe/H] | −0.37±0.13 dex |
Rotation | 16.0±1.0 d |
Rotational velocity (v sin i) | 1.9±1.2 km/s |
Age | 9.6+3.4 −4.2 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
WASP-46 is a G-type main-sequence star about 1,210 light-years (370 parsecs ) away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. [2] Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit. [6]
The star displays an excess ultraviolet emission associated with starspot activity, [7] and is suspected to be surrounded by a dust and debris disk. [8]
In 2011 a transiting hot superjovian planet, WASP-46b, was detected. [2] The planet's equilibrium temperature is 1636±44 K . [4] The dayside temperature measured in 2014 is much higher at 2386 K, indicating a very poor heat redistribution across the planet. [9] A re-measurement of the dayside planetary temperature in 2020 resulted in a lower value of 1870+130
−120 K. [10]
In 2017, a search for transit-timing variations of WASP-46b yielded zero results, thus ruling out existence of additional gas giants in the system. The orbital decay of WASP-46b was also not detected. [11]
Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 1.91±0.11 MJ | 0.02335±0.00063 | 1.43036763(93) | <0.022 [3] | 82.80±0.17 ° | 1.174±0.033 RJ |
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-5 is a magnitude 12 yellow dwarf star located about 910 light-years away in the Phoenix constellation. The star is likely older than Sun, slightly enriched in heavy elements and is rotating rapidly, being spun up by the tides raised by the giant planet on the close orbit.
WASP-45 is a K-type main-sequence star about 690 light-years away. The star age cannot be well constrained, but it is probably older than Sun. Yet, WASP-45 is enriched in heavy elements compared to Sun, having 240% of solar abundance.
WASP-35 is a G-type main-sequence star about 660 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. WASP-35 is similar in concentration of heavy elements compared to the Sun.
Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.
WASP-78, is a single F-type main-sequence star about 2500 light-years away. It is likely to be younger than the Sun at 3.4+1.5
−0.8 billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.
BD-07 436, also known as WASP-77 since 2012, is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares.
WASP-72 is the primary of a binary star system. It is an F7 class dwarf star, with an internal structure just on the verge of the Kraft break. It is orbited by a planet WASP-72b. The age of WASP-72 is younger than the Sun at 3.55±0.82 billion years.
BD+00 316, also known as WASP-71 since 2019, is an F-class main sequence star about 1200 light-years away. The star is younger than the Sun at approximately 3.6 billion years, yet is already close to leaving the main sequence. BD+00 316 is enriched in heavy elements, having 140% of the solar abundance of iron.
WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.
WASP-62, formally named Naledi, is a single star about 573 light-years away. It is an F class main-sequence star, orbited by a planet, WASP-62b. The age of WASP-62 is much younger than the Sun at 0.8±0.6 billion years, and it has a metal abundance similar to the Sun.
WASP-63 or Kosjenka, also known as CD-38 2551, is a single star with an exoplanetary companion in the southern constellation of Columba. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 11.1. The distance to this system is approximately 942 light-years based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.
WASP-61 is a single F-type main-sequence star about 1560 light-years away. The star age is much likely younger than the Sun's 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.
WASP-59 is a K-type main-sequence star about 379 light-years away. The star's age is essentially unconstrained by observations. WASP-59 is slightly depleted in heavy elements, having 70% of the solar abundance of iron. The star produces extremely low levels of ultraviolet light, indicating an absence of flare activity.
WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.
WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.
WASP-75 is a F-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 2.9±0.2 billion years. WASP-75 is similar to the Sun in its concentration of heavy elements.
WASP-88 is a F-type main-sequence star. Its surface temperature is 6450±61 K. WASP-88 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.03±0.04, and is younger at an age of 3.0±1.3 billion years.
WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.
WASP-103 is an F-type main-sequence star located 1,800 ± 100 light-years away in the constellation Hercules. Its surface temperature is 6,110±160 kelvins (K). The star's concentration of heavy elements is similar to that of the Sun. WASP-103 is slightly younger than the Sun at 4±1 billion years. The chromospheric activity of the star is elevated due to interaction with the giant planet on a close-in orbit.