Astronomy:KELT-3
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Leo |
| Right ascension | 09h 54m 34.39s[1] |
| Declination | +40° 23′ 16.98″[1] |
| Apparent magnitude (V) | 9.82 ± 0.03[2]
|
| Characteristics | |
| Evolutionary stage | main sequence star |
| Spectral type | F6V |
| Variable type | planetary transit |
| Astrometry | |
| Proper motion (μ) | RA: -28.328 ± 0.198[1] mas/yr Dec.: -24.411 ± 0.227[1] mas/yr |
| Parallax (π) | 4.7315 ± 0.1213[1] mas |
| Distance | 690 ± 20 ly (211 ± 5 pc) |
| Details[3] | |
| Mass | 1.301±0.046 M☉ |
| Radius | 1.583±0.036 R☉ |
| Luminosity | 3.04[4] L☉ |
| Surface gravity (log g) | 4.153±0.024 cgs |
| Temperature | 6306+36−35 K |
| Metallicity [Fe/H] | 0.030+0.072−0.066 dex |
| Age | 3.0 ± 0.2[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
KELT-3 is a star in the zodiac constellation Leo. With an apparent magnitude of 9.82, it is too faint to be seen with the naked eye, but can be detected using a telescope. It is currently located around 690 light years away, based on parallax measurements.
Properties
KELT-3 is an early F-type main-sequence star with 27.7% more mass than the Sun, and is slightly larger than the latter. It is radiating 3 times the Sun's luminosity, and has a metallicity similar to the latter. It has an effective temperature of 6,304 K, which gives KELT-3 a yellow-white hue. It's also slightly younger than the Sun, with an age of 3 billion years. There is uncertainty about the star's age, it being an evolved star or not.[4]
Since 2015, the star is suspected to have a stellar companion, at angular separation of 3.762±0.009 arcseconds.[5]
Planetary system
In 2013, KELT discovered an eccentric hot Jupiter transiting the star. In the research paper, it is stated as one of the brightest transiting hosts. The light curves of the star have been observed during transits.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.94±0.33[6] MJ | 0.04120 ± 0.00067 | 2.7033902 | 0.202 | 84.25° | 1.458+0.042−0.041[3] RJ |
See also
References
 |  |
- ↑ 1.0 1.1 1.2 1.3 Gaia Collaboration (2018-04-01). "VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018)". VizieR Online Data Catalog 1345. doi:10.26093/cds/vizier.1345. Bibcode: 2018yCat.1345....0G. http://adsabs.harvard.edu/abs/2018yCat.1345....0G.
- ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000-03-01). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. http://adsabs.harvard.edu/abs/2000A%26A...355L..27H.
- ↑ 3.0 3.1 Wang, Xian-Yu; Wang, Yong-Hao; Wang, Songhu; Wu, Zhen-Yu; Rice, Malena; Zhou, Xu; Hinse, Tobias C.; Liu, Hui-Gen et al. (2021), "Transiting Exoplanet Monitoring Project (TEMP). VI. The Homogeneous Refinement of System Parameters for 39 Transiting Hot Jupiters with 127 New Light Curves", The Astrophysical Journal Supplement Series 255 (1): 15, doi:10.3847/1538-4365/ac0835, Bibcode: 2021ApJS..255...15W
- ↑ 4.0 4.1 4.2 4.3 Pepper, Joshua; Siverd, Robert J.; Beatty, Thomas G.; Gaudi, B. Scott; Stassun, Keivan G.; Eastman, Jason; Collins, Karen; Latham, David W. et al. (2013-08-01). "KELT-3b: A Hot Jupiter Transiting a V = 9.8 Late-F Star". The Astrophysical Journal 773 (1): 64. doi:10.1088/0004-637X/773/1/64. ISSN 0004-637X. Bibcode: 2013ApJ...773...64P. http://adsabs.harvard.edu/abs/2013ApJ...773...64P.
- ↑ Wöllert, Maria; Brandner, Wolfgang (2015), "A Lucky Imaging search for stellar sources near 74 transit hosts", Astronomy & Astrophysics 579: A129, doi:10.1051/0004-6361/201526525, Bibcode: 2015A&A...579A.129W
- ↑ Stassun, Keivan G.; Collins, Karen A.; Gaudi, B. Scott (2016), "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes", The Astronomical Journal 153 (3): 136, doi:10.3847/1538-3881/aa5df3, Bibcode: 2017AJ....153..136S
