| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 48m 06.77346s[1] |
| Declination | +48° 12′ 30.9642″[1] |
| Apparent magnitude (V) | 12.70 |
| Characteristics | |
| Spectral type | G2V[2] |
| Apparent magnitude (B) | 13.34[2] |
| Apparent magnitude (V) | 12.70[2] |
| Apparent magnitude (J) | 11.39[2] |
| Apparent magnitude (K) | 11.06[2] |
| Astrometry | |
| Radial velocity (Rv) | 5.64423 ± 4.5 × 10–4[2] km/s |
| Proper motion (μ) | RA: −9.393 mas/yr[1] Dec.: 0.158 mas/yr[1] |
| Parallax (π) | 1.9259 ± 0.0092 mas[1] |
| Distance | 1,694 ± 8 ly (519 ± 2 pc) |
| Details | |
| Mass | 1.238±0.029[2] M☉ |
| Radius | 1.447±0.014[2] R☉ |
| Surface gravity (log g) | (Spectroscopic) 4.28 ± 0.10 cgs (Asteroseismic) 4.210 ± 0.013[2] cgs |
| Temperature | 5854±61[2] K |
| Metallicity [Fe/H] | 0.321±0.065[2] dex |
| Rotational velocity (v sin i) | 3.6±0.5[2] km/s |
| Age | 4.29+0.70 −0.56[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kepler-107 is a star about 1,694 light-years (519 parsecs) away in the constellation Cygnus. It is a spectral type G2 star. An imaging survey in 2016 failed to find any stellar companions to it.[4]
Planetary system
[edit]Kepler-107 has four known planets discovered in 2014.[5][6][7][8] A giant impact is the likely origin of two planets in the system.[2] Kepler-107 c is more than twice as dense (about 12.6 g cm−3) as the innermost exoplanet Kepler-107 b (about 5.3 g cm−3).[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 3.8+1.8 −1.7 M🜨 |
0.04544±0.00036 | 3.1800218±0.0000029 | <0.10 | 89.05±0.67° | 1.536±0.025 R🜨 |
| c | 10.0±2.0 M🜨 | 0.06064±0.00048 | 4.901452±0.0 | <0.080 | 89.49+0.34 −0.44° |
1.597±0.026 R🜨 |
| d | <7.7 M🜨 | 0.08377±0.00065 | 7.95839±0.00012 | <0.11 | 87.55+0.64 −0.48° |
0.860±0.060 R🜨 |
| e | 14.1±3.3 M🜨 | 0.12638±0.00099 | 14.749143±0.000019 | <0.10 | 89.67±0.22° | 2.903±0.035 R🜨 |
References
[edit]- ^ 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 d e f g h i j k l m n o Bonomo, Aldo S.; Zeng, Li; Damasso, Mario; Leinhardt, Zoë M.; Justesen, Anders B.; Lopez, Eric; Lund, Mikkel N.; Malavolta, Luca; Silva Aguirre, Victor; Buchhave, Lars A.; Corsaro, Enrico; Denman, Thomas; Lopez-Morales, Mercedes; Mills, Sean M.; Mortier, Annelies; Rice, Ken; Sozzetti, Alessandro; Vanderburg, Andrew; Affer, Laura; Arentoft, Torben; Benbakoura, Mansour; Bouchy, François; Christensen-Dalsgaard, Jørgen; Collier Cameron, Andrew; Cosentino, Rosario; Dressing, Courtney D.; Dumusque, Xavier; Figueira, Pedro; Fiorenzano, Aldo F. M.; García, Rafael A.; Handberg, Rasmus; Harutyunyan, Avet; Johnson, John A.; Kjeldsen, Hans; Latham, David W.; Lovis, Christophe; Lundkvist, Mia S.; Mathur, Savita; Mayor, Michel; Micela, Giusi; Molinari, Emilio; Motalebi, Fatemeh; Nascimbeni, Valerio; Nava, Chantanelle; Pepe, Francesco; Phillips, David F.; Piotto, Giampaolo; Poretti, Ennio; Sasselov, Dimitar; Ségransan, Damien; Udry, Stéphane; Watson, Chris (May 2019). "A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system". Nature Astronomy. 3 (5): 416–423. arXiv:1902.01316. Bibcode:2019NatAs...3..416B. doi:10.1038/s41550-018-0684-9. S2CID 89604609.
- ^ Kepler-107 -- Rotationally variable Star
- ^ Kraus, Adam L.; Ireland, Michael J.; Huber, Daniel; Mann, Andrew W.; Dupuy, Trent J. (2016), "The Impact of Stellar Multiplicity on Planetary Systems. I. The Ruinous Influence of Close Binary Companions", The Astronomical Journal, 152 (1): 8, arXiv:1604.05744, Bibcode:2016AJ....152....8K, doi:10.3847/0004-6256/152/1/8, S2CID 119110229
- ^ "Exoplanets Data Explorer | Exoplanets - Detail View". exoplanets.org. Retrieved 5 May 2017.
- ^ "Exoplanets Data Explorer | Exoplanets - Detail View". exoplanets.org. Retrieved 5 May 2017.
- ^ "Exoplanets Data Explorer | Exoplanets - Detail View". exoplanets.org. Retrieved 5 May 2017.
- ^ "Exoplanets Data Explorer | Exoplanets - Detail View". exoplanets.org. Retrieved 5 May 2017.
- ^ Bonomo, A. S.; Dumusque, X.; et al. (April 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems". Astronomy & Astrophysics. arXiv:2304.05773. Bibcode:2023A&A...677A..33B. doi:10.1051/0004-6361/202346211. S2CID 258078829.
Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction