Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Columba |
Right ascension | 06h 17m 46.75s [1] |
Declination | −35° 42′ 23.05″ [1] |
Apparent magnitude (V) | 14.67±0.01 [2] |
Characteristics | |
Spectral type | G6 V + K1 V |
B−V color index | +0.77 [2] |
R−I color index | +0.36 [2] |
Astrometry | |
Radial velocity (Rv) | 8.57±0.05 [3] km/s |
Proper motion (μ) | RA: -8.838 [1] mas/yr Dec.: +8.771 [1] mas/yr |
Parallax (π) | 1.3153 ± 0.0193 mas [1] |
Distance | 2,480 ± 40 ly (760 ± 10 pc) |
Details [3] | |
A | |
Mass | 1.02±0.09 M☉ |
Radius | 0.93±0.23 R☉ |
Luminosity | 0.72±0.03 [1] L☉ |
Surface gravity (log g) | 4.45 [4] cgs |
Temperature | 5,600±150 K |
Metallicity [Fe/H] | 0.12±0.15 dex |
Rotational velocity (v sin i) | 1.0±0.7 km/s |
Other designations | |
Gaia DR2 2885350546895266432 | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Extrasolar Planets Encyclopaedia | data |
NGTS-3 is a star located in the southern constellation Columba. With an apparent magnitude of 14.67, it requires a powerful telescope to observe. However, NGTS-3 is actually an unresolved spectroscopic binary. The system is located 2,480 light years away based on parallax, but is drifting away with a radial velocity of 8.57 km/s.
The system contains two main sequence stars of classes G6 and K1 respectively; only the primary properties is known. NGTS-3A has a similar mass to the Sun, but is 7% smaller. It radiates at 72% the Sun's luminosity from its photosphere at an effective temperature of 5,600 K , which gives it a typical yellow hue of a G-type star.
In 2018, the NGTS survey discovered an inflated hot Jupiter orbiting NGTS-3A despite the components being visually unresolved. [3]
Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 2.38 ± 0.26 MJ | 0.023+0.007 −0.005 | 1.6753728 ± 0.0000030 | 0? | 89.56+0.31 −0.48 ° | 1.48 ± 0.37 RJ |
The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.
Gliese 317 is a small red dwarf star with two exoplanetary companions in the southern constellation of Pyxis. It is located at a distance of 49.6 light-years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +87.8 km/s. This star is too faint to be viewed with the naked eye, having an apparent visual magnitude of 11.98 and an absolute magnitude of 11.06.
Gliese 445 is an M-type main sequence star in the northern part of the constellation Camelopardalis.
V1057 Cygni is a suspected binary star system in the northern constellation of Cygnus. It is a variable star of the FU Orionis-type, and was the second FU Orionis-type variable to be discovered. The system is located at a distance of approximately 3,000 light years from the Sun, in the North America Nebula. It has an apparent visual magnitude of around 12.4.
HAT-P-24 is an F8 dwarf star about 400 parsecs away. A planet was discovered with the transit method by the HATNet Project in 2010. HAT-P-24b, is a typical hot Jupiter orbiting in only 3 days.
HD 97413 is a binary star located in the southern constellation Centaurus. The system has a combined magnitude of 6.27, placing it near the limit for naked eye visibility. Based on parallax measurements from the Gaia spacecraft, the system is located 320 light years away from the Solar System.
WR 21a is an eclipsing binary star in the constellation Carina. It includes one of the most massive known stars and is one of the most massive binaries.
TYC 9486-927-1 is the primary of a possible trinary star system located at a distance of 26.7 parsecs from Earth in the southern direction in the constellation of Octans. It is a BY Draconis variable, with large starspots causing it to change brightness as it rotates every 13 hours.
NGTS-3Ab is a gas giant exoplanet that orbits a G-type star. Its mass is 2.38 Jupiters, it takes 1.7 days to complete one orbit of its star, and is 0.023 AU from its star. Its discovery was announced in 2018. The Jupiter-like planet is discovered by 39 astronomers, mainly Max Günther, Didier Queloz, Edward Gillen, Laetitia Delrez, and Francois Bouchy.
KELT-10, also known as CD−47°12635, is a sun-like star in the southern constellation Telescopium. It has an apparent magnitude of 10.62, making it readily visible in telescopes, but not to the naked eye. Parallax measurements from the Gaia spacecraft place the star at a distance of 617 light years; it is currently receding with a radial velocity of 31.6 km/s.
NGTS-1 is a solitary red dwarf located in the constellation Columba. With an apparent magnitude of 15.52, it requires a powerful telescope to be seen. The star is located 716 light years away from the Solar System, and is drifting away with a high radial velocity of 97.2 km/s (60.4 mi/s).
KIC 11145123, is a white hued star located in the northern constellation Cygnus, the swan. It has an apparent magnitude of 13.12, making it readily visible in large telescopes, but not to the naked eye. The object is located relatively far at a distance of approximately 3,910 light years, but is rapidly approaching the Solar System with a radial velocity of −136 km/s.
HAT-P-65 is a faint star located in the equatorial constellation Equuleus. With an apparent magnitude of 13.16, it requires a telescope to be seen. The star is located 2,460 light-years (750 pc) away from Earth, but is drifting close with a radial velocity of -48 km/s.
L 98-59 is a bright M dwarf star, located in the constellation of Volans, at a distance of 10.608 parsecs, as measured by Gaia.
CoRoT-16 is a solitary star located in the equatorial constellation Scutum. With an apparent magnitude of 16, it requires a powerful telescope to be seen, and is located 2,400 light years away based on parallax.
HD 46588 is a star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.44, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of only 59 light years but is receding with a heliocentric radial velocity of 15 km/s.
HD 222806 is a suspected astrometric binary in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.74, allowing it to be faintly seen with the naked eye. Parallax measurements place the system at a distance of 565 light years and it is currently receding with a heliocentric radial velocity of 21 km/s.
HD 193373 is a solitary red hued star located in the equatorial constellation Delphinus. It has an apparent magnitude of 6.21, placing it near the limit for naked eye visibility. Parallax measurements place it 846 light years distant and it is currently receding with a heliocentric radial velocity of 22.7 km/s.
HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.