Kepler-296e

In today's world, Kepler-296e has become a widely debated and researched topic, generating constant discussions and analysis. From its origins to its impact on today's society, Kepler-296e has captured the attention of researchers, experts and enthusiasts alike. With a rich and complex history, Kepler-296e has evolved over time, influencing various areas of daily life. In this article, we will explore in depth the various aspects related to Kepler-296e, from its origins to its impact on the world today, providing a comprehensive and detailed view on this exciting topic.

Kepler-296e
Discovery
Discovery siteKepler Space Observatory
Discovery date2014
Transit
Orbital characteristics
0.17400 AU (26,030,000 km)
Eccentricity<0.33
34.14234700 d
Inclination89.950
StarKepler-296
Physical characteristics
Mean radius
1.530 R🜨
Temperature267 K (−6 Â°C; 21 Â°F)

Kepler-296e (also known by its Kepler Object of Interest designation KOI-1422.05) is a confirmed super-Earth exoplanet orbiting within the habitable zone of Kepler-296. The planet was discovered by NASA's Kepler spacecraft using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. NASA announced the discovery of the exoplanet on 26 February 2014.

Characteristics

Kepler-296e was assumed to be a super-Earth with a radius 1.75 times that of Earth. A more revised estimate puts the planet at 1.53 Earth-radii. The planet orbits Kepler-296 once every 34.1 days at a semimajor axis distance of 0.169 AU. It would have a mass of 4.52 Earth masses, with the higher-than-Earth density suggested by exoplanetkyoto. With an Earth-like density, the mass would be 3.58 Earth masses. The planet's equilibrium temperature is 267 K (–6 °C; 21 °F), much higher than that of Earth.

Habitability

Main articles: Habitability of K-type main-sequence star systems and Habitability of red dwarf systems

The planet was announced as being located within the habitable zone of Kepler-296. In this region, liquid water could exist on the surface of the planet. It is likely rocky, with its relatively low radius, in contrast to f, which is larger. As of 2017, with an ESI of 0.85, it is the fifth-most Earth-like planet after Kepler-438b, TRAPPIST-1 d, and two Gliese-designated planets, GJ 3323 b and Gliese 273 b (Luyten b) which were both discovered in 2017. The planet receives 1.4 times the Earth's solar flux, putting it well within the habitable zone and just barely beyond the runaway G line. According to Kopparapu et. al (2013), the planet is within the most conservative boundaries of the habitable zone. However, it has an eccentric orbit, with a maximum eccentricity of 0.33 to a confidence of 3-sigma. The planet's equilibrium temperature varies depending on its albedo: for a non-tidally locked planet with an Earth-like albedo of 0.3, it is 234 K (–39 °C; –38 °F), and for a Venus-like albedo of 0.7, it is 189 K (–84 °C; -119 °F). For a tidally locked planet with an Earth-like albedo of 0.3, the equilibrium temperature is 278 K (5 °C; 41 °F).

Tidal locking

According to, an Earth-size planet with eccentricity <0.1, no moons, and no obliquity orbiting at the Earth boundary within the habitable zone is tidally locked around a star with a mass of <0.42 solar masses (~M2 or later). When the Solar System is used as a yardstick, then the limit is 0.72 solar masses (~K3-4 or later). However, the orbit of planet e, is likely more eccentric than the modeled fictional planet, so the planet may not have had enough time to tidally lock.

See also

References

  1. ^ a b Staff (26 February 2014). "715 Newly Verified Planets More Than Triples the Number of Confirmed Kepler Planets". NASA. Archived from the original on 4 March 2014. Retrieved 8 January 2015.
  2. ^ Lissauer, Jack J.; et al. (25 February 2014). "Validation of Kepler's Multiple Planet Candidates. II: Refined Statistical Framework and Descriptions of Systems of Special Interest". The Astrophysical Journal. 784 (1): 44. arXiv:1402.6352. Bibcode:2014ApJ...784...44L. doi:10.1088/0004-637X/784/1/44. S2CID 119108651.
  3. ^ Rowe, Jason F. (2014). "Validation of Kepler's Multiple Planet Candidates. III: Light Curve Analysis & Announcement of Hundreds of New Multi-planet Systems". The Astrophysical Journal. 784 (1): 45. arXiv:1402.6534. Bibcode:2014ApJ...784...45R. doi:10.1088/0004-637X/784/1/45. S2CID 119118620.
  4. ^ a b c d e f g Barclay, Thomas; Quintana, Elisa V; Adams, Fred C; Ciardi, David R; Huber, Daniel; Foreman-Mackey, Daniel; Montet, Benjamin T; Caldwell, Douglas (4 August 2015). "The Five Planets in the Kepler-296 Binary System all orbit the Primary: A Statistical and Analytical Analysis". The Astrophysical Journal. 809 (1): 7. arXiv:1505.01845. Bibcode:2015ApJ...809....7B. doi:10.1088/0004-637X/809/1/7. S2CID 37742564.
  5. ^ a b "Kepler-296 e". www.exoplanetkyoto.org. Retrieved 27 November 2023.
  6. ^ a b "New Study Reassesses Habitability of Exoplanets Around Multiple Star Systems - AmericaSpace". www.americaspace.com. 25 May 2015. Retrieved 27 November 2023.
  7. ^ a b "PHL @ UPR Arecibo – the Habitable Exoplanets Catalog". Archived from the original on 10 February 2022. Retrieved 20 March 2022.
  8. ^ "The Five Planets in the Kepler-296 Binary System All Orbit the Primary: A Statistical and Analytical Analysis". IPAC. Retrieved 27 November 2023.
  9. ^ "Kepler-296 e". www.exoplanetkyoto.org. Retrieved 27 November 2023.
  10. ^ a b Huffman, Darrell. "Gravity Simulator | Kepler-296 - System With 5 Exoplanets". gravitysimulator.org. Retrieved 27 November 2023.
  11. ^ Barnes, Rory (1 December 2017). "Tidal locking of habitable exoplanets". Celestial Mechanics and Dynamical Astronomy. 129 (4): 509–536. arXiv:1708.02981. Bibcode:2017CeMDA.129..509B. doi:10.1007/s10569-017-9783-7. ISSN 1572-9478.

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