Astronomy:Kepler-32

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Short description: M-type main sequence star in the constellation Cygnus
Kepler-32
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cygnus
Right ascension  19h 51m 22.1742s[1]
Declination +46° 34′ 27.390″[1]
Apparent magnitude (V) 16.0[2]
Characteristics
Spectral type M1V[3]
Astrometry
Proper motion (μ) RA: −13.618±0.058[1] mas/yr
Dec.: 19.646±0.068[1] mas/yr
Parallax (π)3.0595 ± 0.0322[1] mas
Distance1,070 ± 10 ly
(327 ± 3 pc)
Details
Mass0.58±0.05[2] M☉
Radius0.53±0.04[2] R☉
Surface gravity (log g)4.64[3] cgs
Temperature3900±200[2] K
Metallicity [Fe/H]0.00 dex
Rotation36.220±0.256 days[4]
Other designations
KIC 9787239, KOI-952, 2MASS J19512217+4634273, Gaia DR2 2080287892525359872[3]
Database references
SIMBADdata
KICdata

Kepler-32 is an M-type main sequence star located about 1070 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]

Planetary system

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]

The Kepler-32 planetary system[13]
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

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 "Notes on Kepler-32 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/kepler_32_b--1069/. 
  3. ↑ 3.0 3.1 3.2 "KOI-952". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=KOI-952. 
  4. ↑ 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. doi:10.1088/2041-8205/775/1/L11. Bibcode: 2013ApJ...775L..11M. 
  5. ↑ NBC. "100 billion alien planets fill our galaxy: study". NBC News. http://www.nbcnews.com/id/50348563/ns/technology_and_science-space/#.US-dW4Z8wVB. 
  6. ↑ 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. doi:10.1088/0004-637X/764/1/105. Bibcode: 2013ApJ...764..105S. 
  7. ↑ Lissauer, Jack J.; Ragozzine, Darin; Fabrycky, Daniel C.; Steffen, Jason H.; Ford, Eric B.; Jenkins, Jon M.; Shporer, Avi; Holman, Matthew J. et al. (2011), "Architecture and Dynamics of Kepler 'S Candidate Multiple Transiting Planet Systems", The Astrophysical Journal Supplement Series 197 (1): 8, doi:10.1088/0067-0049/197/1/8, Bibcode: 2011ApJS..197....8L 
  8. ↑ The Extrasolar Planet Encyclopedia. "Kepler-32". Exoplanet.eu. http://voparis-exoplanet-new.obspm.fr/catalog/?f=%27Kepler-32%27+in+name. 
  9. ↑ Fabrycky, Daniel C. (2012). "Transit Timing Observations from Kepler: IV. Confirmation of 4 Multiple Planet Systems by Simple Physical Models". The Astrophysical Journal 750 (2): 114. doi:10.1088/0004-637X/750/2/114. Bibcode: 2012ApJ...750..114F. 
  10. ↑ T. O. Hands, R. D. Alexander, W. Dehnen, "Understanding the assembly of Kepler's compact planetary systems", 2014
  11. ↑ 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, doi:10.1093/mnras/stv2897, Bibcode: 2016MNRAS.456.4121H 
  12. ↑ 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, doi:10.1093/mnras/stx461, Bibcode: 2017MNRAS.468..549B 
  13. ↑ NASA Exoplanet Archive--Planet Host Overview page:Kepler-32
  14. ↑ 14.0 14.1 Characterizing the Cool KOIs. IV. Kepler-32 as a Prototype for the Formation of Compact Planetary Systems throughout the Galaxy

Coordinates: Sky map 19h 51m 22s, +46° 34′ 27″




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