Kepler-29
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus[1] |
| Right ascension | 19h 53m 23.6020s[2] |
| Declination | +47° 29′ 28.436″[2] |
| Apparent magnitude (V) | 15.456±0.025[3] |
| Characteristics | |
| Spectral type | G5V[4] |
| Astrometry | |
| Proper motion (μ) | RA: 6.326±0.069[2] mas/yr Dec.: 16.226±0.049[2] mas/yr |
| Parallax (π) | 1.1739 ± 0.0377 mas[2] |
| Distance | 2,780 ± 90 ly (850 ± 30 pc) |
| Details | |
| Mass | 0.761+0.024 −0.028[5] M☉ |
| Radius | 0.732+0.033 −0.031[5] R☉ |
| Surface gravity (log g) | 4.6±0.1[5] cgs |
| Temperature | 5378±60[5] K |
| Metallicity [Fe/H] | −0.44±0.04[5] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-29 is a Sun-like star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 53m 23.6020s, Declination +47° 29′ 28.436″.[2] With an apparent visual magnitude of 15.456,[3] this star is too faint to be seen with the naked eye. It is a solar analog, having a close mass, radius, and temperature as the Sun. Currently the age of the star has not been determined due to its 2780 light-year (850 parsecs) distance. As of 2016 no Jovian exoplanets of 0.9–1.4 MJ have been found at a distance of 5 AU. [7]
Planetary system
In 2011 an analysis of the first four months of data from the Kepler space telescope detected 1235 planetary candidates two of which orbited this star.[8] Later study of the transit-timing variations of the system lead to the confirmation of both planets.[9] The planetary orbits are lying in Orbital resonance to each other, with orbital period ratio being exactly 7:9.[10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 5.0+1.5 −1.3 M🜨 |
0.09 | 10.33966+0.00015 −0.00017 |
— | — | 2.55±0.12 R🜨 |
| c | 4.5±1.1 M🜨 | 0.11 | 13.28633+0.00031 −0.00027 |
— | — | 2.34+0.12 −0.11 R🜨 |
References
- ^ "Cygnus – constellation boundary", The Constellations, International Astronomical Union, retrieved 2011-12-15
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b Henden, A. A.; et al. (2016). "VizieR Online Data Catalog: AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016)". VizieR On-line Data Catalog: II/336. Originally Published in: 2015AAS...22533616H. 2336. Bibcode:2016yCat.2336....0H.Vizier catalog entry
- ^ Schneider, Jean, "Star: Kepler-29", Extrasolar Planets Encyclopaedia, Paris Observatory, archived from the original on 2012-04-26, retrieved 2011-12-06
- ^ a b c d e f Vissapragada, Shreyas; et al. (2020). "Diffuser-assisted Infrared Transit Photometry for Four Dynamically Interacting Kepler Systems". The Astronomical Journal. 159 (3). 108. arXiv:1907.04445. Bibcode:2020AJ....159..108V. doi:10.3847/1538-3881/ab65c8. S2CID 195874295.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ "Kepler-29". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-06.
- ^ Open Exoplanet Catalogue, Kepler-29
- ^ Borucki, William J.; et al. (2011). "Characteristics of Planetary Candidates Observed by Kepler. II. Analysis of the First Four Months of Data". The Astrophysical Journal. 736 (1). 19. arXiv:1102.0541. Bibcode:2011ApJ...736...19B. doi:10.1088/0004-637X/736/1/19.
- ^ a b Fabrycky, Daniel C.; et al. (2012). "Transit Timing Observations from Kepler. IV. Confirmation of Four 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.
- ^ Panichi, Federico; Goździewski, Krzyszof; Turchetti, Giorgio (2017), "The Reversibility Error Method (REM): a new,dynamical fast indicator for planetary dynamics", Monthly Notices of the Royal Astronomical Society, 468: 469–491, arXiv:1703.10596, doi:10.1093/mnras/stx374, S2CID 119391438
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