Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Lyra [1] |
Right ascension | 19h 09m 33.4137s [2] |
Declination | +46° 59′ 04.108″ [2] |
Apparent magnitude (V) | 14.69 (var.) [3] |
Characteristics | |
Evolutionary stage | Subdwarf B star |
Spectral type | sdB [4] |
Apparent magnitude (J) | 16.36±0.10 [4] |
Variable type | V361 Hya [3] |
Astrometry | |
Proper motion (μ) | RA: 1.133 [2] mas/yr Dec.: −5.907 [2] mas/yr |
Parallax (π) | 0.5573 ± 0.0372 mas [2] |
Distance | 5,900 ± 400 ly (1,800 ± 100 pc) |
Details | |
Mass | 0.47 [5] M☉ |
Radius | 0.24 [5] R☉ |
Luminosity | 3.54 [6] L☉ |
Surface gravity (log g) | 5.35 [6] cgs |
Temperature | 27,500 [5] K |
Metallicity [Fe/H] | 0.0 [5] dex |
Other designations | |
Database references | |
SIMBAD | data |
Exoplanet Archive | data |
Kepler-429 (KIC 10001893) is a variable subdwarf B star in the constellation Lyra, about 5,900 light years away.
The brightness of Kepler-429 changes unpredictably by up to 0.13 magnitudes. [3] It has been classified as a V361 Hydrae variable, but also as a V1093 Herculis variable, which typically has slower variations and a cooler temperature. Over 100 pulsation modes were identified with periods from 256 seconds to over three hours. [7]
Kepler-429 has been reported to have three possible exoplanets, [8] though their existence is questioned. [9] They were detected by orbital brightness modulation. [10]
Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b(unconfirmed) | — | 0.005541 | 0.21970 | 0 [12] | — | — |
c(unconfirmed) | — | 0.007197 | 0.32528 | 0 [13] | — | — |
d(unconfirmed) | — | 0.01324 | 0.81161 | 0 [14] | — | — |
V391 Pegasi, also catalogued as HS 2201+2610, is a blue-white subdwarf star approximately 4,000 light-years away in the constellation of Pegasus. The star is classified as an "extreme horizontal branch star". It is small, with only half the mass and a bit less than one quarter the diameter of the Sun. It has luminosity 34 times that of the Sun. It could be quite old, perhaps in excess of 10 Gyr. It is a pulsating variable star of the V361 Hydrae type. It is believed that the star's mass when it was still on the main sequence was between 0.8 and 0.9 times that of the Sun.
A B-type subdwarf (sdB) is a kind of subdwarf star with spectral type B. They differ from the typical subdwarf by being much hotter and brighter. They are situated at the "extreme horizontal branch" of the Hertzsprung–Russell diagram. Masses of these stars are around 0.5 solar masses, and they contain only about 1% hydrogen, with the rest being helium. Their radius is from 0.15 to 0.25 solar radii, and their temperature is from 20,000 to 40,000 K.
GSC 03549-02811 is a yellow main-sequence star similar to the Sun. This star is located approximately 704 light-years away in the constellation of Draco. The apparent magnitude of this star is 11.41, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night. The age of this star is about 5 billion years.
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Kepler-69 is a G-type main-sequence star similar to the Sun in the constellation Cygnus, located about 2,430 ly (750 pc) from Earth. On April 18, 2013 it was announced that the star has two planets. Although initial estimates indicated that the terrestrial planet Kepler-69c might be within the star's habitable zone, further analysis showed that the planet very likely is interior to the habitable zone and is far more analogous to Venus than to Earth and thus completely inhospitable.
K2-3, also known as EPIC 201367065, is a red dwarf star with three known planets. It is on the borderline of being a late orange dwarf/K-type star, but because of its temperature, it is classified as a red dwarf.
2MASS J19383260+4603591 is a binary star system with at least one known planet, Kepler-451b. The system comprises two stars, a pulsating subdwarf B star as well as a small red dwarf star.
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