 Artist's impression of the Kepler-452 andKepler-186 systems compared to the inner Solar System, with their respective habitable zones shown. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 44m 00.8861s[1] |
| Declination | +44° 16′ 39.171″[1] |
| Apparent magnitude (V) | 13.426[2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | G2V[3] |
| Astrometry | |
| Proper motion (μ) | RA: 9.987(13)mas/yr[1] Dec.: 8.943(14)mas/yr[1] |
| Parallax (π) | 1.8053±0.0103 mas[1] |
| Distance | 1,810 ± 10 ly (554 ± 3 pc) |
| Details | |
| Mass | 1.037+0.054 −0.047 M☉ |
| Radius | 1.11+0.15 −0.09 R☉ |
| Luminosity | 1.2 L☉ |
| Surface gravity (log g) | 4.32 ± 0.09 cgs |
| Temperature | 5757 ± 85 K |
| Metallicity [Fe/H] | 0.21 ± 0.09 dex |
| Age | 6 ± 2 Gyr |
| Other designations | |
| Gaia DR2 2079597124345617280,KOI-7016,KIC 8311864,GSC 3148-814,2MASS J19440088+4416392[4] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| KIC | data |
| Extrasolar Planets Encyclopaedia | data |
Kepler-452 is aG-type main-sequence star located about 1,810light-years away fromEarth[1] in theCygnus constellation.[5] Although similar in temperature to theSun, it is 20% brighter, 3.7% more massive and 11% larger.[6][7] Alongside this, the star is approximately six billion years old and possesses a highmetallicity.[3]
Prior to Kepler observation, Kepler-452 had the2MASS catalogue number 2MASS 19440088+4416392. In the Kepler Input Catalog, it has the designation of KIC 8311864. When it was found to have a transiting planet candidate, it was given theKepler object of interest number of KOI-7016.
Planetary candidates were detected around the star byNASA'sKepler Mission, a mission tasked with discovering planets intransit around their stars. The transit method that Kepler uses involves detecting dips in brightness of stars. These dips in brightness can be interpreted as planets whose orbits pass in front of their stars from the perspective ofEarth, although other phenomena can also be responsible which is why the term "planetary candidate" is used.[8]
Following the acceptance of the discovery paper, the Kepler team referred to the star as Kepler-452, which is the normal procedure for naming exoplanets discovered by the spacecraft.[9][3] Hence, this is the name usually used by the public to refer to the star and its planet.
Candidate planets that are associated with stars studied by the Kepler Mission are assigned the designations ".01", ".02", and so on, after the star's name, in the order of discovery.[2] If planet candidates are detected simultaneously, then the ordering follows the order of orbital periods from shortest to longest.[2] Following these rules, there was only one candidate planet detected, with an orbital period of 384.843 days. The name Kepler-452 derives directly from the fact that the star is the catalogued 452nd star discovered byKepler to have confirmed planets.
The designationb, derives from the order of discovery. The designation ofb is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet.[10] In the case of Kepler-452, there was only one planet, so only the letterb is used.
Kepler-452 is aG-type star that is approximately 104% the mass of and 111% the radius of theSun. It has a temperature of 5757K and is roughly 6 billion years old. In comparison, the Sun is about 4.6 billion years old[11] and has a temperature of 5778 K.[12]
The star is metal-rich, with ametallicity (Fe/H) of about 0.21, or about 162% of the amount of iron and other heavier metals found in the Sun.[3] The star's luminosity is somewhat normal for a star like Kepler-452, with a luminosity of around 120% of that of the solar luminosity.
The star'sapparent magnitude, or how bright it appears from Earth's perspective, is 13.426. Therefore, it is too dim to be seen with the naked eye.
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b(unconfirmed[14][15]) | 5 ± 2[16]M🜨 | 1.046+0.019 −0.015 | 384.843+0.007 −0.012 | — | 89.806+0.134 −0.049° | 1.5+0.32 −0.22 R🜨 |
The star hosts one unconfirmedexoplanet,Kepler-452b, discovered in July 2015 by theKepler spacecraft. This planet is mostly known for its characteristics similar to Earth, most notably its size, orbit and stellar flux. It is the first potentially rockysuper-Earth[17] planet discovered orbiting within thehabitable zone and theabiogenesis zone of a star very similar to theSun.[6][18] It may even have a surface temperature similar to that of Earth (the planet has anequilibrium temperature of approximately 265 K (−8 °C; 17 °F) (Earth's equilibrium temperature is only 10K cooler than this). However, its star is 6 billion years old (roughly 1.5 billion years older than the Sun). Due to this, Kepler-452b is receiving roughly 10% more stellar radiation than the Earth does today. If Kepler-452b is a rocky planet, it might be subject to arunaway greenhouse effect. However, because of its mass (estimated to be about 5ME), it may be able to prevent succumbing to the runaway greenhouse for a limited amount of time (at most about 500 million years). Nevertheless, the planet is one of the most Earth-like planets discovered so far by theKepler team. Both the Earth and Kepler-452b are at just the right distances from their stars so that water can be liquid, at a temperature between 0 °C and 100 °C.[19]
This table compares the Sun to Kepler-452.
| Identifier | J2000 Coordinates | Distance (ly) | Stellar Class | Temperature (K) | Metallicity (dex) | Age (Gyr) | Notes | |
|---|---|---|---|---|---|---|---|---|
| Right ascension | Declination | |||||||
| Sun | — | — | 0.00 | G2V | 5,778 | +0.00 | 4.6 | [20] |
| Kepler-452 [21] | 19h 44m 00.89s | +44° 16′ 39.2″ | 1,800 | G2V | 5,757 | +0.21 | 6.0 | [22] |