Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Lyra |
Right ascension | 18h 52m 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° |
Observed separation (projected) | 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 | |
Kepler-410A: Gaia EDR3 2106904148451706752 | |
Kepler-410B: Gaia EDR3 2106904148449360000 | |
Database references | |
SIMBAD | data |
B |
HD 175289 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±75 K. [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-410 Ab , 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🜨 |
(unconfirmed) | 0.165 M🜨 | — | 26.5 | — | — | — |
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−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.
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−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.
HATS-3 is a F-type main-sequence star. Its surface temperature is 6351±76 K. HATS-3 is relatively depleted in its concentration of heavy elements, with a metallicity Fe/H index of −0.157±0.07, but is slightly younger than the Sun at an age of 3.2+0.6
−0.4 billion years.
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