| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus [1] |
| Right ascension | 19h 53m 23.6018s [2] |
| Declination | +47° 29′ 28.437″ [2] |
| Apparent magnitude (V) | 15.456±0.025 [3] |
| Characteristics | |
| Spectral type | G5V [4] |
| Astrometry | |
| Proper motion (μ) |
RA: 6.487(29)
mas/
yr
[2] Dec.: 16.183(24) mas/ yr [2] |
| Parallax (π) | 1.1276 ± 0.0229 mas [2] |
| Distance | 2,890 ± 60
ly (890 ± 20 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 23.6018s, Declination +47° 29′ 28.437″. [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 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 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, 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.
- ^ "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
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus [1] |
| Right ascension | 19h 53m 23.6018s [2] |
| Declination | +47° 29′ 28.437″ [2] |
| Apparent magnitude (V) | 15.456±0.025 [3] |
| Characteristics | |
| Spectral type | G5V [4] |
| Astrometry | |
| Proper motion (μ) |
RA: 6.487(29)
mas/
yr
[2] Dec.: 16.183(24) mas/ yr [2] |
| Parallax (π) | 1.1276 ± 0.0229 mas [2] |
| Distance | 2,890 ± 60
ly (890 ± 20 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 23.6018s, Declination +47° 29′ 28.437″. [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 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 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, 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.
- ^ "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