| Observation data EpochJ2000 EquinoxJ2000 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 07h 37m 09.23325s[1] |
| Declination | −13° 54′ 23.9569″[1] |
| Apparent magnitude (V) | 10.04[2] |
| Characteristics | |
| Spectral type | G5IV-V/K2III[2] |
| Astrometry | |
| Radial velocity (Rv) | 18.23±0.15[1] km/s |
| Proper motion (μ) | RA: -0.601mas/yr[1] Dec.: -3.625mas/yr[1] |
| Parallax (π) | 1.0746±0.0140 mas[1] |
| Distance | 3,040 ± 40 ly (930 ± 10 pc) |
| Absolute magnitude (MV) | 0.03[citation needed] |
| Details[3] | |
| Mass | 2.03±0.14 M☉ |
| Radius | 17.71±1.04 R☉ |
| Luminosity | 131.8 L☉ |
| Surface gravity (log g) | 2.23±0.04 cgs |
| Temperature | 4534±12 K |
| Metallicity [Fe/H] | −0.08±0.01 dex |
| Rotational velocity (v sin i) | 2.19 km/s |
| Age | 1.02 Gyr |
| Other designations | |
| BD−13 2130,TIC 288474555,TYC 5409-2156-1,GSC 05409-02156,2MASS J07370922-1354239,NGC 2423 3, NGC 2423 MMU 3, NGC 2423 SN 4[2] | |
| Database references | |
| SIMBAD | data |
NGC 2423-3 is ared giantstar approximately 3,040light-years away in theconstellation ofPuppis. The star is part of theNGC 2423open cluster (hence the nameNGC 2423-3). The star has anapparent magnitude of 10 and anabsolute magnitude of zero, with a mass of 2.4 times theSun. In 2007, it was proposed that anexoplanet orbits the star, but this is now doubtful.
NGC 2423-3 b is anexoplanet 10.6 times more massive thanJupiter. Only theminimum mass is known since theorbital inclination is not known, so it is likely to be abrown dwarf instead. The planet orbits at 2.1AU, taking 1.956 years to orbit eccentrically around the star. Its eccentricity is about the same asMercury, but less thanPluto. The planet has asemi-amplitude of 71.5m/s.[4]
This planet was discovered byChristophe Lovis andMichel Mayor in July 2007 by theradial velocity method.[4] Lovis had also found threeNeptune-mass planets orbitingHD 69830 in May 2006, also in Puppis.
However, a 2018 study with the same C. Lovis as an author found evidence that the radial velocity signal corresponding to the proposed planetary companion could be caused by stellar activity orstellar pulsations, and so the planet may not exist.[5] Another study by the same team in 2023 confirms evidence for a stellar origin of the signal.[3]
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b(dubious) | >10.6MJ | 2.10 | 714.3 ± 5.3 | 0.21 ± 0.07 | — | — |
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