Kepler-102
Kepler-102 is a star in the constellation of Lyra. It has five known exoplanets. Kepler-102 is less luminous than the Sun.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h 45m 55.8553s[1] |
| Declination | +47° 12′ 28.859″[1] |
| Apparent magnitude (V) | 12.07[2] |
| Astrometry | |
| Proper motion (μ) | RA: −40.603±1.244[1] mas/yr Dec.: −44.144±0.889[1] mas/yr |
| Parallax (π) | 9.62 ± 0.34[1] mas |
| Distance | 340 ± 10 ly (104 ± 4 pc) |
| Details | |
| Mass | 0.8[3] M☉ |
| Radius | 0.74[3] R☉ |
| Temperature | 4903[3] K |
| Metallicity [Fe/H] | +0.08[3] dex |
| Rotation | 26.572±0.153 d[4] |
| Other designations | |
| Database references | |
| SIMBAD | data |
Planetary system
On January 2014, a system of five planets around the star was announced, three of them being smaller than Earth. While 3 of the transit signals were discovered during the first year of the Kepler mission, their small size made them hard to confirm as possibilities of these being false positives were needed to be removed. Later, two other signals were detected. Follow-up radial velocity data helped to determine the mass of the largest planet.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | — | 0.055 | 5.28696 | — | 85.37° | 0.47 R⊕ |
| c | — | 0.067 | 7.07142 | — | 87.09° | 0.58 R⊕ |
| d | — | 0.086 | 10.3117 | — | 87.09° | 1.18 R⊕ |
| e | 8.9 ± 2.0 M⊕ | 0.116 | 16.1457 | — | 87.66° | 2.22 R⊕ |
| f | — | 0.165 | 27.4536 | — | 88.24° | 0.88 R⊕ |
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gollark: Yes, inasmuch as far as I know you need various more advanced calculus things to do much of that, as well as large quantities of other maths you don't appear to know.
gollark: One basic use is that you can calculate the rate of change of things, because that's basically what the derivative is. For example, velocity is rate of change of displacement, so you can go from displacement to velocity (to acceleration, which is rate of change of velocity, and so on), or integrate to go the other way.
gollark: Having vaguely looked at how they work, I don't think you can do that unless you know the frequency of sound in question.
References
- Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.Gaia Data Release 1 catalog entry
- "KOI-82". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 January 2018.
- "How many exoplanets has Kepler discovered?". 2015-04-09.
- 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.
- Masses, radii, and orbits of small Kepler planets: the transition from gaseous to rocky planets accessdate=8 January 2014
- "Geoffrey Marcy – Personal Website" (PDF).
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