18h52m36.1606s, +45° 08′ 23.3432″| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h52m 36.1606s[1] |
| Declination | +45° 08′ 23.343″[1] |
| Apparent magnitude (V) | 9.50[1] |
| Characteristics | |
| Kepler-410A | |
| Evolutionary stage | Subgiant |
| Spectral type | F6IV[2] |
| Kepler-410B | |
| Spectral type | K2[3] |
| Astrometry | |
| A | |
| Radial velocity (Rv) | −40.6±0.7[4] km/s |
| Proper motion (μ) | RA: 61.683[4] mas/yr Dec.: 61.673[4] mas/yr |
| Parallax (π) | 6.7933 ± 0.0109 mas[4] |
| Distance | 480.1 ± 0.8 ly (147.2 ± 0.2 pc) |
| B | |
| Proper motion (μ) | RA: 61.679[4] mas/yr Dec.: 60.937[5] mas/yr |
| Parallax (π) | 6.8007 ± 0.0260 mas[5] |
| Distance | 480 ± 2 ly (147.0 ± 0.6 pc) |
| Position (relative to Kepler-410A)[6] | |
| Component | Kepler-410B |
| Angular distance | 1.6672±0.0015″ |
| Position angle | 35.975±0.052° |
| Projected separation | 245 AU |
| Details | |
| Kepler-410A | |
| Mass | 1.223±0.054[7] M☉ |
| Radius | 1.357±0.022[7] R☉ |
| Luminosity | 2.66±0.16[7] L☉ |
| Surface gravity (log g) | 4.28±0.02[8] cgs |
| Temperature | 6325±75[8] K |
| Metallicity [Fe/H] | 0.01±0.10[8] dex |
| Rotation | 20.3+2.2 −1.3 d[9] |
| Age | 1.81±0.27[7] Gyr |
| Kepler-410B | |
| Mass | 0.728[3] M☉ |
| Radius | 0.89+0.09 −0.03[3] R☉ |
| Other designations | |
BD+44 3008, Kepler-410, KOI-42, KIC 8866102, TYC 3540-760-1, GSC 03540-00760, 2MASS J18523616+4508233[1] | |
| Kepler-410A: Gaia EDR3 2106904148451706752 | |
| Kepler-410B: Gaia EDR3 2106904148449360000 | |
| Database references | |
| SIMBAD | data |
| B | |
Kepler-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.[6]
The primary star's surface temperature is 6325±75K.[8] HD 175289 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.01±0.10,[8] but is much younger at an age of 1.81±0.27 billion years.[7]
In 2013, one planet, named Kepler-410Ab, was discovered using the transit method.[10] It is not known if the planet is orbiting the primary or secondary star.[10] If orbiting the secondary, the planetary radius must be doubled.[11] Immediately, a second non-transiting planet was suspected due to transit-timing variations, and a 2019 study also found evidence for such a planet, though it has not yet been confirmed or given any designation.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.14±0.01 | 17.833682±0.000012 | 0.17 | 90° | 2.48±0.07 R🜨 |
| c (unconfirmed) | 0.165 M🜨 | — | 26.5 | — | — | — |
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