Kepler-1513
Main-sequence star in the constellation Lyra
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Kepler-1513 is a main-sequence star about 1,150 light-years (350 parsecs) away in the constellation Lyra. It has a late-G[4] or early-K[3] spectral type, and it hosts at least one, and likely two, exoplanets.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra[1] |
| Right ascension | 19h 19m 09.99418s[2] |
| Declination | +39° 17′ 06.9287″[2] |
| Apparent magnitude (V) | 12.888±0.100 (Kepler band) |
| Characteristics | |
| Evolutionary stage | Main sequence[2] |
| Spectral type | K0V[3] or late G[4] |
| Apparent magnitude (G) | 12.946±0.003[2] |
| Apparent magnitude (J) | 11.758±0.027[5] |
| Apparent magnitude (H) | 11.397±0.030[5] |
| Apparent magnitude (K) | 11.309±0.020[5] |
| Astrometry | |
| Radial velocity (Rv) | −0.42±1.41[2] km/s |
| Proper motion (μ) | RA: 20.439 mas/yr[2] Dec.: 1.745 mas/yr[2] |
| Parallax (π) | 2.8446±0.0134 mas[2] |
| Distance | 1,147 ± 5 ly (352 ± 2 pc) |
| Details[6] | |
| Mass | 0.943±0.037 M☉ |
| Radius | 0.950+0.077 −0.055 R☉ |
| Luminosity (bolometric) | 0.743+0.148 −0.100 L☉ |
| Surface gravity (log g) | 4.46±0.10 cgs |
| Temperature | 5491±100 K |
| Metallicity | 0.17±0.06 [M/H] |
| Age | 7.0+4.0 −4.2 Gyr |
| Other designations | |
| Kepler-1513, KOI-3678, KIC 4150804, TIC 394177315, 2MASS J19190999+3917070[5] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
Planetary system
Kepler-1513b (KOI-3678.01) was confirmed in 2016 as part of a study statistically validating hundreds of Kepler planets.[7] In November 2022, an exomoon candidate was reported around Kepler-1513b based on transit-timing variations (TTVs). Unlike previous giant exomoon candidates in the Kepler-1625 and Kepler-1708 systems, this exomoon would have been terrestrial-mass, ranging from 0.76 Lunar masses to 0.34 Earth masses depending on the planet's mass and the moon's orbital period.[4]
In October 2023, a follow-up study by the same team of astronomers using additional observations found that the observed TTVs cannot be explained by an exomoon, but can be explained by a second, outer planet, Kepler-1513c, with a mass comparable to Saturn.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.152+0.104 −0.061 MJ |
0.53+0.04 −0.03 |
160.8842+0.0011 −0.0028 |
0.306+0.093 −0.097 |
— | 8.05+0.58 −0.40 R🜨 |
| c | 0.266+0.098 −0.063 MJ |
1.7106[8] | 841.4+8.1 −5.3 |
0.125+0.018 −0.019 |
— | — |