Kepler-13 or KOI-13 is a stellar triple star system consisting of Kepler-13A, around which an orbiting hot Jupiter exoplanet was discovered with the Kepler space telescope in 2011, and Kepler-13B a common proper motion companion star which has an additional star orbiting it.[8]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra[1] |
| Kepler-13 A | |
| Right ascension | 19h 07m 53.1397s[2] |
| Declination | 46° 52′ 05.922″[2] |
| Apparent magnitude (V) | 9.95[3] |
| Kepler-13 B | |
| Right ascension | 19h 07m 53.0281s[4] |
| Declination | 46° 52′ 06.126″[4] |
| Apparent magnitude (V) | 10.33[5] |
| Characteristics | |
| Spectral type | A4 |
| Variable type | Planetary transit variable[6] |
| Astrometry | |
| Kepler-13 A | |
| Proper motion (μ) | RA: −4.411(42) mas/yr[2] Dec.: −15.220(50) mas/yr[2] |
| Parallax (π) | 2.0319 ± 0.0344 mas[2] |
| Distance | 1,610 ± 30 ly (492 ± 8 pc) |
| Kepler-13 B | |
| Proper motion (μ) | RA: −4.060(33) mas/yr[4] Dec.: −15.512(40) mas/yr[4] |
| Parallax (π) | 2.0912 ± 0.0263 mas[4] |
| Distance | 1,560 ± 20 ly (478 ± 6 pc) |
| Details[7] | |
| Kepler-13A | |
| Mass | 1.72±0.10 M☉ |
| Radius | 1.71±0.04 R☉ |
| Surface gravity (log g) | 4.2±0.5 cgs |
| Temperature | 7650±250 K |
| Metallicity [Fe/H] | 0.2±0.2 dex |
| Rotational velocity (v sin i) | 78±15 km/s |
| Age | 0.5±0.1 Gyr |
| Kepler-13B | |
| Mass | 1.68±0.10 M☉ |
| Radius | 1.68±0.04 R☉ |
| Surface gravity (log g) | 4.2±0.5 cgs |
| Temperature | 7530±250 K |
| Metallicity [Fe/H] | 0.2±0.2 dex |
| Rotational velocity (v sin i) | 69±13 km/s |
| Age | 0.5±0.1 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Stellar system
editThe multiple nature of the system was discovered in 1904 by Robert Grant Aitken at Lick Observatory. He measured a separation between the A and B components of approximately one arc second and position angle of 281.3° with the 36" James Lick telescope.[9] The position of the two visual components of the system relative to each other has remained constant since 1904.[10] Radial velocity measurements taken with the SOPHIE échelle spectrograph at the Haute-Provence Observatory revealed an additional companion orbiting Kepler-13B. This companion has a mass of between 0.4 and 1 times that of the Sun and orbits with a period of 65.831 days with an eccentricity of 0.52[8]
Planetary system
editKepler-13 was identified as one of 1235 planetary candidates with transit-like signatures in the first four months of Kepler data.[11] It was confirmed as a planet by measuring the Doppler beaming effect on the Kepler light curve.[6] The planet that has been confirmed, having a radius of between 1.5 and 2.6 RJ, is also one of the largest known exoplanets.
The planet is likely to be tidally locked to the parent star. In 2015, the planetary nightside temperature was estimated to be equal to 2394±251 K.[12]
The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is mildly misaligned with the equatorial plane of the star, misalignment equal to 24±4°.[13]
The planetary transits are changing in duration over time which is likely caused by the interaction of the planet with its host star.[14][15]
In 2017, Hubble observations by a team of astronomers led by Thomas Beatty revealed that titanium monoxide molecules in the dayside might be carried to the nightside of the planet, where they form clouds and precipitate.[16]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 9.28(16) MJ | 0.03641(87) | 1.763588(1) | 0.00064+0.00012 −0.00016 |
86.770+0.048 −0.052° |
2.216(87) RJ |
References
edit- ^ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. 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 "Kepler-13". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-01-07.
- ^ 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.
- ^ Howarth, Ian D.; Morello, Giuseppe (2017). "Rapid rotators revisited: Absolute dimensions of KOI-13". Monthly Notices of the Royal Astronomical Society. 470 (1): 932–939. arXiv:1705.07302. Bibcode:2017MNRAS.470..932H. doi:10.1093/mnras/stx1260. S2CID 31123194.
- ^ a b Shporer, Avi; et al. (2011). "Detection of Koi-13.01 Using the Photometric Orbit". The Astronomical Journal. 142 (6) 195. arXiv:1110.3510. Bibcode:2011AJ....142..195S. doi:10.1088/0004-6256/142/6/195.
- ^ Shporer, Avi; et al. (2014). "Atmospheric Characterization of the Hot Jupiter Kepler-13Ab". The Astrophysical Journal. 788 (1) 92. arXiv:1403.6831. Bibcode:2014ApJ...788...92S. doi:10.1088/0004-637X/788/1/92.
- ^ a b Santerne, A.; et al. (2012). "SOPHIE velocimetry of Kepler transit candidates. VI. An additional companion in the KOI-13 system". Astronomy and Astrophysics. 544 L12. arXiv:1207.1715. Bibcode:2012A&A...544L..12S. doi:10.1051/0004-6361/201219899. S2CID 118482346.
- ^ Aitken, Robert Grant (1904). "Measures of one hundred fifty-five new double stars". Lick Observatory Bulletin. 3: 6–18. Bibcode:1904LicOB...3....6A. doi:10.5479/ADS/bib/1904LicOB.3.6A.
- ^ Szabó, Gy. M.; et al. (2011). "Asymmetric Transit Curves As Indication of Orbital Obliquity: Clues from the Late-Type Dwarf Companion in Koi-13". The Astrophysical Journal Letters. 736 (1) L4. arXiv:1105.2524. Bibcode:2011ApJ...736L...4S. doi:10.1088/2041-8205/736/1/L4.
- ^ 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.
- ^ Angerhausen, Daniel; et al. (2015). "A Comprehensive Study of Kepler Phase Curves and Secondary Eclipses: Temperatures and Albedos of Confirmed Kepler Giant Planets". Publications of the Astronomical Society of the Pacific. 127 (957): 1113–1130. arXiv:1404.4348. Bibcode:2015PASP..127.1113A. doi:10.1086/683797.
- ^ Albrecht, Simon; et al. (2012). "Obliquities of Hot Jupiter host stars: Evidence for tidal interactions and primordial misalignments". The Astrophysical Journal. 757 (1) 18. arXiv:1206.6105. Bibcode:2012ApJ...757...18A. doi:10.1088/0004-637X/757/1/18.
- ^ Szabó, Gy. M.; et al. (2011). "Spin-orbit resonance, transit duration variation and possible secular perturbations in KOI-13". MNRAS. 421 (1) L122. arXiv:1110.4231. Bibcode:2012MNRAS.421L.122S. doi:10.1111/j.1745-3933.2012.01219.x.
- ^ Shahaf, Sahar; et al. (12 May 2021). "Systematic search for long-term transit duration changes in Kepler transiting planets". Monthly Notices of the Royal Astronomical Society. 505 (1): 1293–1310. arXiv:2105.04318. Bibcode:2021MNRAS.505.1293S. doi:10.1093/mnras/stab1359.
- ^ "Hubble Observes Exoplanet that Snows Sunscreen - NASA Science". science.nasa.gov. Retrieved 2024-01-06.
- ^ Esteves, Lisa J.; Mooij, Ernst J. W. De; Jayawardhana, Ray (2015). "Changing Phases of Alien Worlds: Probing Atmospheres Of Kepler planets with High-Precision Photometry". The Astrophysical Journal. 804 (2) 150. arXiv:1407.2245. Bibcode:2015ApJ...804..150E. doi:10.1088/0004-637X/804/2/150.