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]
| 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 |
Planetary system
editIn 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🜨 |
References
edit- ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d "Notes on Kepler-32 b". Extrasolar Planets Encyclopaedia. Retrieved 21 January 2017.
- ^ a b c "KOI-952". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 January 2017.
- ^ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1). L11. arXiv:1308.1845. Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID 118557681.
- ^ NBC (3 January 2013). "100 billion alien planets fill our galaxy: study". NBC News. Retrieved 28 February 2013.
- ^ Swift, Jonathan J. (2012). "Characterizing the Cool KOIs IV: Kepler-32 as a prototype for the formation of compact planetary systems throughout the Galaxy". The Astrophysical Journal. 764 (1): 105. arXiv:1301.0023. Bibcode:2013ApJ...764..105S. doi:10.1088/0004-637X/764/1/105. S2CID 43750666.
- ^ Lissauer, Jack J.; Ragozzine, Darin; Fabrycky, Daniel C.; Steffen, Jason H.; Ford, Eric B.; Jenkins, Jon M.; Shporer, Avi; Holman, Matthew J.; Rowe, Jason F.; Quintana, Elisa V.; Batalha, Natalie M.; Borucki, William J.; Bryson, Stephen T.; Caldwell, Douglas A.; Carter, Joshua A.; Ciardi, David; Dunham, Edward W.; Fortney, Jonathan J.; Gautier, Iii, Thomas N.; Howell, Steve B.; Koch, David G.; Latham, David W.; Marcy, Geoffrey W.; Morehead, Robert C.; Sasselov, Dimitar (2011), "Architecture and Dynamics of Kepler 'S Candidate Multiple Transiting Planet Systems", The Astrophysical Journal Supplement Series, 197 (1): 8, arXiv:1102.0543, Bibcode:2011ApJS..197....8L, doi:10.1088/0067-0049/197/1/8, S2CID 43095783
- ^ The Extrasolar Planet Encyclopedia. "Kepler-32". Exoplanet.eu. Archived from the original on 3 February 2014. Retrieved 28 February 2013.
- ^ Fabrycky, Daniel C.; et al. (2012). "Transit Timing Observations from Kepler: IV. Confirmation of 4 Multiple Planet Systems by Simple Physical Models". The Astrophysical Journal. 750 (2): 114. arXiv:1201.5415. Bibcode:2012ApJ...750..114F. doi:10.1088/0004-637X/750/2/114. S2CID 9075167.
- ^ T. O. Hands, R. D. Alexander, W. Dehnen, "Understanding the assembly of Kepler's compact planetary systems", 2014
- ^ Hands, T. O.; Alexander, R. D. (2015), "There might be giants: unseen Jupiter-mass planets as sculptors of tightly-packed planetary systems", Monthly Notices of the Royal Astronomical Society, 456 (4): 4121–4127, arXiv:1512.02649, Bibcode:2016MNRAS.456.4121H, doi:10.1093/mnras/stv2897, S2CID 55175754
- ^ Becker, Juliette C.; Adams, Fred C. (2017), "Effects of Unseen Additional Planetary Perturbers on Compact Extrasolar Planetary Systems", Monthly Notices of the Royal Astronomical Society, 468 (1): 549–563, arXiv:1702.07714, Bibcode:2017MNRAS.468..549B, doi:10.1093/mnras/stx461, S2CID 119325005
- ^ NASA Exoplanet Archive--Planet Host Overview page:Kepler-32
- ^ a b Characterizing the Cool KOIs. IV. Kepler-32 as a Prototype for the Formation of Compact Planetary Systems throughout the Galaxy
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