Astronomy:Kepler-71
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 37m 57.7155s |
| Declination | 46° 17′ 08.9428″ |
| Apparent magnitude (V) | 15.06 |
| Characteristics | |
| Evolutionary stage | main sequence star |
| Spectral type | G8V |
| V−R color index | -0.29 |
| R−I color index | 0.46 |
| J−H color index | 0.377 |
| J−K color index | 0.457 |
| Variable type | ROT[1] |
| Astrometry | |
| Radial velocity (Rv) | 0±7 km/s |
| Proper motion (μ) | RA: -2.343±0.039 mas/yr Dec.: -1.073±0.041 mas/yr |
| Parallax (π) | 1.0647 ± 0.0204 mas |
| Distance | 3,060 ± 60 ly (940 ± 20 pc) |
| Details[2][3][4] | |
| Mass | 0.923 M☉ |
| Radius | 0.816 R☉ |
| Surface gravity (log g) | 4.54±0.01 cgs |
| Temperature | 5545 K |
| Metallicity [Fe/H] | 0.22 dex |
| Rotation | period 20 days |
| Age | 2.5-4 Gyr |
| Other designations | |
KOI-217, BOKS 40959, KIC 9595827, 2MASS J19392772+4617090, Gaia DR2 2080095679848047872[5] | |
| Database references | |
| SIMBAD | data |
Kepler-71 is a yellow main sequence star in the constellation of Cygnus.
Star characteristics
Kepler-71 is enriched by heavy elements at 170% of Sun metallicity, young and has a very prominent starspot activity. Starspots are covering about 40% of star surface at transit latitudes, each planetary transit passing over an average six starspots.[2] The bright facula regions are even more extensive.[6] Unlike Sun, the photosphere of Kepler-71 rotates nearly like rigid body, with differential rotation not exceeding 2%.[4]
Planetary system
The "Hot Jupiter" class planet Kepler-71b was discovered around Kepler-71 in 2010.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.05029+0.00002−0.00006 | 3.905079476+0.000008−0.000009 | 0 | 89.8+0.2−0.4° | 1.1987±0.0044 RJ |
References
- ↑ "VARIABLE STAR TYPE DESIGNATIONS IN VSX". https://www.aavso.org/vsx/index.php?view=about.vartypes. Retrieved 2020-05-23.]
- ↑ 2.0 2.1 2.2 Gusmão, Eber A.; Selhorst, Caius L.; Oliveira, Alexandre S. (2016). "Analysis of Kepler-71 Activity Through Planetary Transit". Proceedings of the International Astronomical Union 12: 140–142. doi:10.1017/S1743921317004057.
- ↑ 3.0 3.1 Howell, Steve B.; Rowe, Jason F.; Sherry, William; von Braun, Kaspar; Ciardi, David R.; Bryson, Stephen T.; Feldmeier, John J.; Horch, Elliott et al. (2010). "Keplerobservations of Three Pre-Launch Exoplanet Candidates: Discovery of Two Eclipsing Binaries and a New Exoplanet". The Astrophysical Journal 725 (2): 1633–1643. doi:10.1088/0004-637X/725/2/1633. Bibcode: 2010ApJ...725.1633H.
- ↑ 4.0 4.1 4.2 Zaleski, S. M.; Valio, A.; Marsden, S. C.; Carter, B. D. (2019). "Differential rotation of Kepler-71 via transit photometry mapping of faculae and starspots". Monthly Notices of the Royal Astronomical Society 484 (1): 618–630. doi:10.1093/mnras/sty3474. Bibcode: 2019MNRAS.484..618Z. http://eprints.usq.edu.au/37370/2/Zaleski_pub_2019.pdf.
- ↑ KOI-217 -- Rotationally variable Star
- ↑ Schrijver, Carolus J. (2020). "Testing the Solar Activity Paradigm in the Context of Exoplanet Transits". The Astrophysical Journal 890 (2): 121. doi:10.3847/1538-4357/ab67c1. Bibcode: 2020ApJ...890..121S.
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