Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cygnus |
Right ascension | 19h 51m 22.1744s [1] |
Declination | +46° 34′ 27.391″ [1] |
Apparent magnitude (V) | 16.0 [2] |
Characteristics | |
Spectral type | M1V [3] |
Astrometry | |
Proper motion (μ) |
RA: −13.762(31)
mas/
yr
[1] Dec.: 19.586(32) mas/ yr [1] |
Parallax (π) | 3.0960 ± 0.0276 mas [1] |
Distance | 1,053 ± 9
ly (323 ± 3 pc) |
Details | |
Mass | 0.58±0.05 [2] M☉ |
Radius | 0.53±0.04 [2] R☉ |
Surface gravity (log g) | 4.64 [3] cgs |
Temperature | 3900±200 [2] K |
Metallicity [Fe/H] | 0.00 dex |
Rotation | 36.220±0.256 days [4] |
Other designations | |
Database references | |
SIMBAD | data |
KIC | data |
Kepler-32 is an M-type main sequence star located about 1053 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, [5] it shows a 0.58 ± 0.05 solar mass ( M☉), a 0.53 ± 0.04 solar radius ( R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity. [6]
In 2011, 2 planets orbiting around it, were discovered, and two more suspected. [7] The smaller Kepler-32b, orbiting its parent star every 5.90124 days, and Kepler-32c with an orbital period of 8.7522 days. [8] In April 2013, transit-timing variation analysis confirmed 3 other planets to be in the system. However, only very loose constraints of the maximum mass of the planets could be determined. [9] In 2014, the dynamical simulation shown what the Kepler-32 planetary system have likely undergone a substantial inward migration in the past, producing an observed pattern of lower-mass planets on tightest orbits. [10] Additional yet unobserved gas giant planets on wider orbit are likely necessary for migration of smaller planets to proceed that far inward, [11] although current planetary systems would be unstable if additional planets are located closer than 8.7 AU from the parent star. [12]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
f | — | 0.013 | 0.742956 | — | — | 0.81±0.05 R🜨 |
e | — | 0.033 | 2.896009 | — | — | 1.5±0.1 R🜨 |
b | 0.011 [14] MJ | 0.05 | 5.90124 | — | — | 2.2±0.2 R🜨 |
c | 0.012 [14] MJ | 0.09 | 8.7522 | — | — | 2.0±0.2 R🜨 |
d | — | 0.129 | 22.780806 | — | — | 2.7±0.1 R🜨 |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cygnus |
Right ascension | 19h 51m 22.1744s [1] |
Declination | +46° 34′ 27.391″ [1] |
Apparent magnitude (V) | 16.0 [2] |
Characteristics | |
Spectral type | M1V [3] |
Astrometry | |
Proper motion (μ) |
RA: −13.762(31)
mas/
yr
[1] Dec.: 19.586(32) mas/ yr [1] |
Parallax (π) | 3.0960 ± 0.0276 mas [1] |
Distance | 1,053 ± 9
ly (323 ± 3 pc) |
Details | |
Mass | 0.58±0.05 [2] M☉ |
Radius | 0.53±0.04 [2] R☉ |
Surface gravity (log g) | 4.64 [3] cgs |
Temperature | 3900±200 [2] K |
Metallicity [Fe/H] | 0.00 dex |
Rotation | 36.220±0.256 days [4] |
Other designations | |
Database references | |
SIMBAD | data |
KIC | data |
Kepler-32 is an M-type main sequence star located about 1053 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, [5] it shows a 0.58 ± 0.05 solar mass ( M☉), a 0.53 ± 0.04 solar radius ( R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity. [6]
In 2011, 2 planets orbiting around it, were discovered, and two more suspected. [7] The smaller Kepler-32b, orbiting its parent star every 5.90124 days, and Kepler-32c with an orbital period of 8.7522 days. [8] In April 2013, transit-timing variation analysis confirmed 3 other planets to be in the system. However, only very loose constraints of the maximum mass of the planets could be determined. [9] In 2014, the dynamical simulation shown what the Kepler-32 planetary system have likely undergone a substantial inward migration in the past, producing an observed pattern of lower-mass planets on tightest orbits. [10] Additional yet unobserved gas giant planets on wider orbit are likely necessary for migration of smaller planets to proceed that far inward, [11] although current planetary systems would be unstable if additional planets are located closer than 8.7 AU from the parent star. [12]
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
f | — | 0.013 | 0.742956 | — | — | 0.81±0.05 R🜨 |
e | — | 0.033 | 2.896009 | — | — | 1.5±0.1 R🜨 |
b | 0.011 [14] MJ | 0.05 | 5.90124 | — | — | 2.2±0.2 R🜨 |
c | 0.012 [14] MJ | 0.09 | 8.7522 | — | — | 2.0±0.2 R🜨 |
d | — | 0.129 | 22.780806 | — | — | 2.7±0.1 R🜨 |