Kepler-63
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus[1] |
| Right ascension | 19h 16m 54.2861s[2] |
| Declination | 49° 32′ 53.451″[2] |
| Apparent magnitude (V) | 12.02[3] |
| Characteristics | |
| Evolutionary stage | Main sequence[2] |
| Spectral type | G2V[4] |
| Astrometry | |
| Radial velocity (Rv) | −21.7±0.8[2] km/s |
| Proper motion (μ) | RA: 14.375[2] mas/yr Dec.: 23.336[2] mas/yr |
| Parallax (π) | 5.1157±0.0096 mas[2] |
| Distance | 638 ± 1 ly (195.5 ± 0.4 pc) |
| Details[5] | |
| Mass | 0.984+0.035 −0.040 M☉ |
| Radius | 0.901+0.027 −0.021 R☉ |
| Luminosity | 0.696+0.076 −0.059[3] L☉ |
| Surface gravity (log g) | 4.52±0.02 cgs |
| Temperature | 5576±50 K |
| Metallicity [Fe/H] | 0.05±0.08[3] dex |
| Rotation | 5.4±0.009 days |
| Rotational velocity (v sin i) | 5.6±0.8[3] km/s |
| Age | 0.21±0.045 Gyr |
| Other designations | |
| KOI-63, TYC 3550-458-1, 2MASS J19165428+4932535[6] | |
| Database references | |
| SIMBAD | data |
Kepler-63 is a G-type main-sequence star about 638 light-years away. The star is much younger than the Sun, at 0.21 billion years. Kepler-63 is similar to the Sun in its concentration of heavy elements.
The star is exhibiting strong starspot activity, with relatively cold (4700±300 K) starspots concentrated in two mid-latitude bands similar to the Sun,[5] changing their position in a cycle with a period of 1.27±0.16 years.[7] Due to high magnetic activity associated with its young age, Kepler-63 has a very hot corona heated to 8 million degrees, and produces over ten times the solar amount of x-rays than the Sun.[8]
Multiplicity surveys did not detect any stellar companions to Kepler-63 by 2016.[9]
Planetary system
[edit]In 2013 a transiting hot Jupiter planet b was detected on a tight orbit. The orbit is nearly polar to the equatorial plane of the star.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | < 0.377[8] MJ | 0.080±0.002[8] | 9.4341505±0.000001[5] | <0.45[3] | 87.806+0.018 −0.019[5]° |
0.54±0.02[8] RJ |
References
[edit]- ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ^ a b c d e f g 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 e f Sanchis-Ojeda, Roberto; Winn, Joshua N.; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard; Johnson, John Asher; Torres, Guillermo; Albrecht, Simon; Campante, Tiago L.; Chaplin, William J.; Davies, Guy R.; Lund, Mikkel N.; Carter, Joshua A.; Dawson, Rebekah I.; Buchhave, Lars A.; Everett, Mark E.; Fischer, Debra A.; Geary, John C.; Gilliland, Ronald L.; Horch, Elliott P.; Howell, Steve B.; Latham, David W. (2013), "KEPLER-63b: A GIANT PLANET IN a POLAR ORBIT AROUND a YOUNG SUN-LIKE STAR", The Astrophysical Journal, 775 (1): 54, arXiv:1307.8128, Bibcode:2013ApJ...775...54S, doi:10.1088/0004-637X/775/1/54, S2CID 36615256
- ^ Frasca, A.; Molenda-Żakowicz, J.; Alonso-Santiago, J.; Catanzaro, G.; De Cat, P.; Fu, J. N.; Zong, W.; Wang, J. X.; Cang, T.; Wang, J. T. (2022). "Characterization of Kepler targets based on medium-resolution LAMOST spectra analyzed with ROTFIT". Astronomy and Astrophysics. 664: A78. arXiv:2205.04757. Bibcode:2022A&A...664A..78F. doi:10.1051/0004-6361/202243268.
- ^ a b c d Netto, Y.; Valio, A. (2020), "Stellar magnetic activity and the butterfly diagram of Kepler-63", Astronomy & Astrophysics, 635: A78, arXiv:1911.08661, Bibcode:2020A&A...635A..78N, doi:10.1051/0004-6361/201936219, S2CID 208176115
- ^ "Kepler-63", SIMBAD, Centre de données astronomiques de Strasbourg
- ^ Estrela, Raissa; Valio, Adriana (2016), Stellar magnetic cycles in the solar-like stars Kepler-17 and Kepler-63, arXiv:1608.07322
- ^ a b c d Lalitha, Sairam; Schmitt, J H M M.; Dash, Spandan (2018), "Atmospheric mass-loss of extrasolar planets orbiting magnetically active host stars", Monthly Notices of the Royal Astronomical Society, 477: 808–815, arXiv:1803.08684, doi:10.1093/mnras/sty732
- ^ Furlan, E.; Ciardi, D. R.; Everett, M. E.; Saylors, M.; Teske, J. K.; Horch, E. P.; Howell, S. B.; Van Belle, G. T.; Hirsch, L. A.; Gautier, T. N.; Adams, E. R.; Barrado, D.; Cartier, K. M. S.; Dressing, C. D.; Dupree, A. K.; Gilliland, R. L.; Lillo-Box, J.; Lucas, P. W.; Wang, J. (2016), "Thekeplerfollow-Up Observation Program. I. A Catalog of Companions Tokeplerstars from High-Resolution Imaging", The Astronomical Journal, 153 (2): 71, arXiv:1612.02392, doi:10.3847/1538-3881/153/2/71, S2CID 38339900