Kepler-25
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra[1] |
| Right ascension | 19h 06m 33.2141s[2] |
| Declination | +39° 29′ 16.359″[2] |
| Apparent magnitude (V) | 10.623±0.053[3] |
| Characteristics | |
| Spectral type | F[4] |
| Apparent magnitude (B) | 11.337±0.016[3] |
| Variable type | Planetary transit variable |
| Astrometry | |
| Proper motion (μ) | RA: −0.303(14) mas/yr[2] Dec.: 6.109(13) mas/yr[2] |
| Parallax (π) | 4.1456 ± 0.0113 mas[2] |
| Distance | 787 ± 2 ly (241.2 ± 0.7 pc) |
| Details | |
| Mass | 1.159+0.040 −0.051[5] M☉ |
| Radius | 1.297±0.015[5] R☉ |
| Luminosity | 2.406+0.126 −0.128[5] L☉ |
| Surface gravity (log g) | 4.275+0.007 −0.008[5] cgs |
| Temperature | 6270±79[6] K |
| Metallicity [Fe/H] | −0.05±0.10[6] dex |
| Rotation | 23.147±0.039 days[7] |
| Rotational velocity (v sin i) | 9.5[8] km/s |
| Age | 3.45+0.81 −0.72[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-25 is a star in the northern constellation of Lyra.[1] It is slightly larger and more massive than the Sun, with a luminosity 21⁄2 times that of the Sun.[5] With an apparent visual magnitude of 10.6,[3] this star is too faint to be seen with the naked eye.
Planetary system
[edit]In 2011, two candidate planets were found transiting this star by the Kepler space telescope.[10] These planets are very close to yet not lie in the 1:2 orbital resonance to each other, indicating the absence of other planetary objects in the inner part of the planetary systems.[11] These planets were confirmed through transit-timing variation method.[12] A third planet was discovered through follow-up radial velocity measurements and was confirmed in January 2014.[8]
The plane of planetary orbits is well aligned with the equatorial plane of the star, misalignment angle equal to 7±8°[13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 8.7+2.5 −2.3 M🜨 |
0.068 | 6.238297±0.000017 | 0.0029+0.0023 −0.0017 |
92.827+0.084 −0.083° |
2.748+0.038 −0.035 R🜨 |
| c | 15.2+1.3 −1.6 M🜨 |
0.11 | 12.7207±0.0001 | 0.0061+0.0049 −0.0041 |
92.764+0.042 −0.039° |
5.217+0.070 −0.065 R🜨 |
| d | 71.9±9.8 M🜨 | — | 122.4+0.0 −0.7 |
0.13+0.13 −0.09 |
— | — |
References
[edit]- ^ a b Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Vizier query form
- ^ 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.
- ^ a b c 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
- ^ a b Schneider, Jean, "Star: Kepler-25", Extrasolar Planets Encyclopaedia, archived from the original on 2012-06-16, retrieved 2013-12-18
- ^ a b c d e f Silva Aguirre, V.; et al. (2015). "Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology". Monthly Notices of the Royal Astronomical Society. 452 (2): 2127–2148. arXiv:1504.07992. Bibcode:2015MNRAS.452.2127S. doi:10.1093/mnras/stv1388.
- ^ a b Huber, Daniel; et al. (2013). "Fundamental Properties of Kepler Planet-candidate Host Stars using Asteroseismology". The Astrophysical Journal. 767 (2). 127. arXiv:1302.2624. Bibcode:2013ApJ...767..127H. doi:10.1088/0004-637X/767/2/127.
- ^ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1). L11. arXiv:1308.1845. Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11.
- ^ a b Marcy, Geoffrey W.; et al. (2014). "Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets". The Astrophysical Journal Supplement Series. 210 (2). 20. arXiv:1401.4195. Bibcode:2014ApJS..210...20M. doi:10.1088/0067-0049/210/2/20.
- ^ "Kepler-25". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-02.
- ^ 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.
- ^ Migaszewski, Cezary; Gozdziewski, Krzysztof (2018), "A periodic configuration of the Kepler-25 planetary system?", Monthly Notices of the Royal Astronomical Society, 480 (2): 1767–1777, arXiv:1803.10285, doi:10.1093/mnras/sty1972, S2CID 55395774
- ^ Steffen, Jason H.; et al. (2012). "Transit timing observations from Kepler - III. Confirmation of four multiple planet systems by a Fourier-domain study of anticorrelated transit timing variations". Monthly Notices of the Royal Astronomical Society. 421 (3): 2342–2354. arXiv:1201.5412. Bibcode:2012MNRAS.421.2342S. doi:10.1111/j.1365-2966.2012.20467.x.
- ^ Albrecht, Simon; Winn, Joshua N.; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard; Johnson, John A. (2013), "Low Stellar Obliquities in Compact Multiplanet Systems", The Astrophysical Journal, 771 (1): 11, arXiv:1302.4443, Bibcode:2013ApJ...771...11A, doi:10.1088/0004-637X/771/1/11, S2CID 17247029
- ^ Mills, Sean M.; et al. (2019). "Long-period Giant Companions to Three Compact, Multiplanet Systems". The Astronomical Journal. 157 (4). 145. arXiv:1903.07186. Bibcode:2019AJ....157..145M. doi:10.3847/1538-3881/ab0899.
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