Kepler-45

Today, Kepler-45 continues to be a topic of great relevance and interest in society. With the advancement of technology and globalization, Kepler-45 has become an increasingly frequent topic of discussion in different areas, from politics to popular culture. Its impact and scope cover a wide spectrum of aspects of daily life, making it a topic of constant study and reflection. In this article, we will explore different perspectives and approaches related to Kepler-45, with the aim of better understanding its influence today and its projection in the future.

Kepler-45
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus[1]
Right ascension 19h 31m 29.4966s[2]
Declination +41° 03′ 51.356″[2]
Apparent magnitude (V) 16.88[3]
Characteristics
Spectral type M1 V[4]
Astrometry
Proper motion (μ) RA: 4.646(36) mas/yr[2]
Dec.: −21.589(36) mas/yr[2]
Parallax (π)2.5984±0.0331 mas[2]
Distance1,260 ± 20 ly
(385 ± 5 pc)
Details
Mass0.59 ± 0.06[5] M☉
Radius0.55 ± 0.11[5] R☉
Temperature3820 ± 90[5] K
Metallicity 0.13 ± 0.13[5] dex
Other designations
Gaia DR2 2053562475706063744, Kepler-45, KOI-254, KIC 5794240, 2MASS J19312949+4103513
Database references
SIMBADdata
KICdata
Kepler-45

Kepler-45, formerly known as KOI-254, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: right ascension 19h 31m 29.495s, declination +41° 03′ 51.37″.[6] With an apparent visual magnitude of 16.88,[4] this star is too faint to be seen with the naked eye.

The star is exhibiting strong starspot activity, with 4.1±2.5% of its surface covered by starspots.[7]

Planetary system

The Kepler-45 planetary system[8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 0.5505 MJ 0.030 2.455239 — — 11 R🜨

The "Hot Jupiter" class planet Kepler-45b,[9] discovered in February 2011,[10] is unusually massive for the M-class parent star.[11] Its orbit is aligned within 11 degrees of rotational axis of the star.[12]

The planet is strongly suspected to have optically thick rings, because its planetary shadow appears to be elongated.[13]

See also

References

  1. ^ "Cygnus – constellation boundary", The Constellations, International Astronomical Union, retrieved 2011-12-15
  2. ^ 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.
  3. ^ "Kepler-45". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 January 2018.
  4. ^ a b Muirhead, Philip S.; Hamren, Katherine; Schlawin, Everett; Rojas-Ayala, Bárbara; Covey, Kevin R.; et al. (May 2012). "Characterizing the Cool Kepler Objects of Interests. New Effective Temperatures, Metallicities, Masses, and Radii of Low-mass Kepler Planet-candidate Host Stars". The Astrophysical Journal Letters. 750 (2). L37. arXiv:1109.1819. Bibcode:2012ApJ...750L..37M. doi:10.1088/2041-8205/750/2/L37. S2CID 27131741.
  5. ^ a b c d Kepler-45b, NASA Ames Research Center, archived from the original on 2015-09-19, retrieved 2011-12-06
  6. ^ "Kepler Discoveries". 2011-12-05. Archived from the original on 2010-05-27.
  7. ^ Activity and differential rotation of the early M dwarf Kepler-45 from transit mapping
  8. ^ Schneider, Jean, "Star: Kepler-45", Extrasolar Planets Encyclopaedia, archived from the original on 2014-03-04, retrieved 2011-12-06
  9. ^ Kepler-45 b at exoplanet.eu
  10. ^ Ford, Eric B.; Rowe, Jason F.; Fabrycky, Daniel C.; Carter, Joshua A.; Holman, Matthew J.; Lissauer, Jack J.; Ragozzine, Darin; Steffen, Jason H.; Batalha, Natalie M.; Borucki, William J.; Bryson, Steve; Caldwell, Douglas A.; Dunham, Edward W.; Gautier, Thomas N.; Jenkins, Jon M.; Koch, David G.; Li, Jie; Lucas, Philip; Marcy, Geoffrey W.; McCauliff, Sean; Mullally, Fergal R.; Quintana, Elisa; Still, Martin; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D. (2011), "Transit Timing Observations from Kepler : I. Statistical Analysis of the First Four Months", The Astrophysical Journal Supplement Series, 197 (1): 2, arXiv:1102.0544, Bibcode:2011ApJS..197....2F, doi:10.1088/0067-0049/197/1/2, S2CID 118472942
  11. ^ Gaidos, E.; Mann, A. W.; Kraus, A. L.; Ireland, M. (2016). "They are small worlds after all: Revised properties of Kepler M dwarf stars and their planets". Monthly Notices of the Royal Astronomical Society. 457 (3): 2877–2899. arXiv:1512.04437. Bibcode:2016MNRAS.457.2877G. doi:10.1093/mnras/stw097. S2CID 53705225.
  12. ^ Dai, Fei; Winn, Joshua N.; Berta-Thompson, Zachory; Sanchis-Ojeda, Roberto; Albrecht, Simon (2018). "Stellar Obliquity and Magnetic Activity of Planet-hosting Stars and Eclipsing Binaries Based on Transit Chord Correlation". The Astronomical Journal. 155 (4): 177. arXiv:1803.05000. Bibcode:2018AJ....155..177D. doi:10.3847/1538-3881/aab618. S2CID 59454470.
  13. ^ Revealing peculiar exoplanetary shadows from transit light curves