Kepler-46 b (2MASS J19170449 + 4236150 b, KIC 7109675 b, KOI-872 b) is an exoplanet discovered in 2011 by the star Kepler-46 in the constellation Cygnus .
| Kepler-46 b | |
|---|---|
| Exoplanet | |
| Parent star | |
| Star | Kepler-46 |
| Constellation | Swan |
| Right Ascension ( α ) | 19 h 17 m 04,499 s [1] |
| Declination ( δ ) | + 42 ° 36 ′ 15.03 ″ [1] |
| Visible magnitude ( m V ) | 13.347 (± 0.028) [1] |
| Distance | St. years old (2,795 (± 226) light years (855 (± 67) pc ) [1] pc ) |
| Spectral class | K1V [1] |
| Weight ( m ) | 0.902 +0.040 −0.038 [1] M ☉ |
| Radius ( r ) | 0.938 +0.038 −0.039 [1] R ☉ |
| Temperature ( T ) | 5155 (± 105) [1] K |
| Metallicity ([Fe / H]) | 0.41 (± 0.10) [1] |
| Age | 9.9 +3.1 −3.1 [2] billion years |
| Elements of the orbit | |
| Era of orbit | J2000.0 [1] |
| Semimajor axis ( a ) | 0.1968 +0.0029 −0.0028 [1] a. e. |
| Eccentricity ( e ) | 0.01 (± 0.01) [1] |
| Orbital Period ( P ) | 33,60134 +0,00021 −0,00020 [1] d. |
| physical characteristics | |
| Weight ( m ) | <6 [1] M J (<1907 [1] M ⊕ ) |
| Radius ( r ) | 0.808 +0.042 −0.043 [1] R J (9,057 +0,471 −0.482 [1] R ⊕ ) |
| Density ( ρ ) | <14 [1] g / cm 3 |
| Temperature ( T ) | 543 (± 16) [1] K |
| Discovery Information | |
| opening date | 2011 |
| Detection method | Transit |
| Opening place | Kepler telescope |
| Opening status | Published |
| Other designations | |
| 2MASS J19170449 + 4236150 b, KIC 7109675 b, KOI-872 b [1] | |
The Kepler-46 b exoplanet was discovered by the Kepler space telescope in 2011 using the transit photometry method based on observations of the passage of an exoplanet against a star background.
Content
Native Star
Kepler-46 is a star , an orange dwarf , of the K1 spectral class of main sequence stars, with a surface temperature of about 5155 K. The radius and mass of the star is only 0.94 and 0.9 of the solar. Located in the constellation Cygnus . At least two exoplanets, Kepler-46 b and Kepler-46 s , and one candidate for exoplanets, Kepler-46 d , circulate around the star.
Interesting fact
Orange dwarfs are of interest in the search for extraterrestrial civilizations ( SETI ), since they are stable on the main sequence of 15-30 billion years (1.5-3 longer than the Sun ). The reason for this is a more complete consumption of hydrogen than on the Sun , as well as lower luminosity . These factors contribute to maintaining constant conditions in the formation of planets and life on the planets. After the main sequence, the orange dwarfs also expand to the red giant and drop shells to form a white dwarf , but these processes occur noticeably slower than on the Sun. In addition, given the age of the universe (13 billion years), not a single orange dwarf has yet managed to become a red giant .
See also
- Kepler-12
- List of exoplanets discovered in 2011
- Hot jupiter
Notes
- ↑ 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 NASA Exoplanet Archive .
- ↑ Exoplanet.eu .
Articles
Directories
- 2MASS = 19170449 + 4236150 (English) . VizieR Catalog Service .
- KOI-872 SIMBAD
- Kepler-46 b Ames Research Center.
- Kepler-46b (English) . NASA Exoplanet Archive.
- KOI-872 (English) (unavailable link) . Open Exoplanet Catalog. Archived October 17, 2013.
- Exoplanet Kepler-46 b (English) . Exoplanets Findthedata.
- Planet Kepler-46 b (English) . Exoplanet.eu.