Kepler-51
From Wikipedia the free encyclopedia
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 45m 55.14s[1] |
| Declination | +49° 56′ 15.65″[1] |
| Characteristics | |
| Spectral type | G[2] |
| Astrometry | |
| Radial velocity (Rv) | −4.3[3] km/s |
| Proper motion (μ) | RA: 0.075±0.020[1] mas/yr Dec.: −7.451±0.019[1] mas/yr |
| Parallax (π) | 1.2457 ± 0.0165 mas[1] |
| Distance | 2,620 ± 30 ly (800 ± 10 pc) |
| Details[4][2] | |
| Mass | 0.985±0.012 M☉ |
| Radius | 0.881±0.011 R☉ |
| Luminosity | 0.66[5] L☉ |
| Surface gravity (log g) | 4.51+0.03 −0.04 cgs |
| Temperature | 5,662+64 −65 K |
| Metallicity [Fe/H] | +0.04±0.04 dex |
| Rotational velocity (v sin i) | 5.5±1.0[3] km/s |
| Age | 500±250[2] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kepler-51 is a Sun-like star that is about 500 million years old.[2] It is orbited by four planets—Kepler-51b, c, d and e—first three of which are super-puffs and have the lowest known densities of any known exoplanet. The transiting planets in the system (b, c and d) are similar in radius to gas giants like Jupiter, but have unusually small masses for their size, only a few times greater than Earth’s.[2]
Properties
[edit]Kepler-51 is a small G-type star, with a slightly lower radius, mass and effective temperature than the Sun. It is a young star, less than one billion years old, and hence is highly active compared to the Sun. Around 4 to 6% of the star's surface is covered by starspots. Its EUV and X-ray fluxes are likely influencing the chemistry, dynamics and atmospheric mass loss of its planets.[7][2]
Planetary system
[edit]| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 3.69+1.86 −1.59 M🜨 | 0.2514±0.0097 | 45.15405±0.00039 | 0.026±0.010 | 89.78+0.15 −0.17° | 6.83±0.13 R🜨 |
| c | 5.65±0.81 M🜨 | 0.384±0.015 | 85.3139±0.0020 | 0.063±0.020 | — | 6.4±1.4 R🜨 |
| d | 5.6±1.2 M🜨 | 0.509±0.020 | 130.182±0.0024 | 0.01±0.01 | 89.91+0.06 −0.08° | 9.32±0.18 R🜨 |
| e | 1.8–8.5 M🜨 or <1 MJ | — | 256.860±0.631 or <3650 | 0.08±0.032 | — | — |
Kepler-51 has four planets, discovered between 2013 and 2024. The first planets discovered in the system were Kepler-51 b, c and d, detected by the transit method.[2] The radius of these planets were measured using transit data, yielding values of 7.1, 9.0 and 9.7 R🜨 respectively. Their masses were measured using transit-timing variations, giving masses of 2.1, 4.0 and 7.6 ME respectively. These estimates imply very low densities, less than 0.05 g/cm3, one of the lowest of any exoplanets,[7] or 14 times less than Saturn. The low masses were later confirmed in 2020[2] and 2024, and the densities have been improved to less than 0.14 g/cm3.[7]
Kepler-51 b, c and d are called super-puffs, planets with masses a bit larger than that of Earth, but radii larger than Neptune.[2] The reason for the low density of these planets remains elusive, and many hypotheses have been proposed for explain the nature of these planets, all of which have flaws.[7][2]
In 2024, the Kepler-51 system was revealed to have a new planet, detected using transit timing variations by the James Webb Space Telescope. This new planet, named Kepler-51e, has an orbital period around 260 days and a mass estimated to be between 1.3 and 5.4 Earth masses.[7]
Kepler-51b
[edit]The innermost planet, Kepler-51b, has an orbital period of 45 days. It is 6.8 times larger than Earth and 319 times more voluminous, but its mass is only 3.5 times that of Earth. This translates to a very low density of 0.06 g/cm3, much lower than that of any planet in the Solar System.[7] Given the planet's proximity to its host star, its equilibrium temperature is of 543 K.[7]
Transmission spectroscopy with the James Webb Space Telescope revealed that Kepler-51b has a featureless spectrum, implying that its extended atmosphere has a high photochemical haze layer. Over time, the planet will contract, lose part of its atmosphere and become a sub-Neptune.[2]
Kepler-51c
[edit]Kepler-51c takes 85 days to complete an orbit around its host star, about the same as the planet Mercury. It has 6.4 times Earth's radius (40,770 km) and is 262 times more voluminous, while its mass is only around 5.65 Earth masses. This implies a low density of 0.14 g/cm3.[7]
Kepler-51d
[edit]Kepler-51d is the puffiest planet in the system, with an density of just 0.0381 g/cm3. It is also the largest planet orbiting Kepler-51d, with 9.32 times Earth's radius (59,400 km), almost the same size as Saturn. Its mass, however, is only 3.8 times that of Earth.[7]
Transmission spectroscopy with the James Webb Space Telescope revealed that Kepler-51d has a featureless spectrum, implying that its extended atmosphere has a high photochemical haze layer. Over time, the planet will contract and lose part of its atmosphere, but will still have a low density.[2]
The rotation of the planet has been measured to be larger or equal than 40 hours.[9]
References
[edit]- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d e f g h i j k l m Libby-Roberts, Jessica E.; et al. (2020). "The Featureless Transmission Spectra of Two Super-puff Planets". The Astronomical Journal. 159 (2): 57. arXiv:1910.12988. Bibcode:2020AJ....159...57L. doi:10.3847/1538-3881/ab5d36. S2CID 204950000.
- ^ a b Petigura, Erik A.; et al. (September 2017). "The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets". The Astronomical Journal. 154 (3): 20. arXiv:1703.10400. Bibcode:2017AJ....154..107P. doi:10.3847/1538-3881/aa80de. S2CID 55183141. 107.
- ^ Johnson, John Asher; et al. (September 2017). "The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars". The Astronomical Journal. 154 (3): 9. arXiv:1703.10402. Bibcode:2017AJ....154..108J. doi:10.3847/1538-3881/aa80e7. S2CID 119241581. 108.
- ^ 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.
- ^ "KOI-620". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-01-08.
- ^ a b c d e f g h i j Masuda, Kento; Libby-Roberts, Jessica E.; Livingston, John H.; Stevenson, Kevin B.; Gao, Peter; Vissapragada, Shreyas; Fu, Guangwei; Han, Te; Greklek-McKeon, Michael (2024-10-02), A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations, doi:10.48550/arXiv.2410.01625, retrieved 2024-10-05
- ^ Masuda, Kento (2014). "Very Low Density Planets Around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event". The Astrophysical Journal. 783 (1): 53. arXiv:1401.2885. Bibcode:2014ApJ...783...53M. doi:10.1088/0004-637X/783/1/53. S2CID 119106865.
- ^ Lammers, Caleb; Winn, Joshua N. (2024-09-10). "Slow Rotation for the Super-Puff Planet Kepler-51d". arXiv:2409.06697.
Further reading
[edit]- Kepler-51 is Home to Three Super-Puff Exoplanets, Sci-News, Dec 20, 2019 by Natali Anderson
 | This main-sequence-star-related article is a stub. You can help Wikipedia by expanding it. |