사용자:Ta183ta/연습장

외계행성 편집

지난 20년 동안 외계행성 수천 개가 발견되었다. 이들 (系)와, 이 계들을 구성하는 행성들의 궤도는 태양계와 확연하게 다르다. 이 외계행성들 중에는 뜨거운 목성, 따뜻한 목성, 슈퍼지구, 빽빽하게 모여 있는 내행성들 등이 포함되어 있다.

뜨거운 목성 및 따뜻한 목성들은 태어나는 과정 혹은 태어난 후 현재의 궤도로 이동해 온 것으로 생각된다. 이 이동에 대해 여러 가지 가능한 메커니즘이 제안되었다. I형 또는 II형 이동은 행성 궤도의 긴반지름을 서서히 감소시켜 뜨겁거나 따뜻한 목성을 형성하게 만들 수 있다. Gravitational scattering by other planets onto eccentric orbits with a perihelion near the star followed by the circularization of its orbit due to tidal interactions with the star can leave a planet on a close orbit. If a massive companion planet or star on an inclined orbit was present an exchange of inclination for eccentricity via the Kozai mechanism raising eccentricities and lowering perihelion followed by circularization can also result in a close orbit. Many of the Jupiter-sized planets have eccentric orbits which may indicate that gravitational encounters occurred between the planets, although migration while in resonance can also excite eccentricities.[1] The in situ growth of hot Jupiters from closely orbiting super Earths has also been proposed. The cores in this hypothesis could have formed locally or at a greater distance and migrated close to the star.[2]

Super-Earths and other closely orbiting planets are thought to have either formed in situ or ex situ, that is, to have migrated inward from their initial locations.[3] The in situ formation of closely orbiting super-Earths would require a massive disk, the migration of planetary embryos followed by collisions and mergers, or the radial drift of small solids from farther out in the disk. The migration of the super-Earths, or the embryos that collided to form them, is likely to have been Type I due to their smaller mass. The resonant orbits of some of the exoplanet systems indicates that some migration occurred in these systems, while the spacing of the orbits in many of the other systems not in resonance indicates that an instability likely occurred in those systems after the dissipation of the gas disk. The absence of Super-Earths and closely orbiting planets in the Solar System may be due to the previous formation of Jupiter blocking their inward migration.[4]

The amount of gas a super-Earth that formed in situ acquires may depend on when the planetary embryos merged due to giant impacts relative to the dissipation of the gas disk. If the mergers happen after the gas disk dissipates terrestrial planets can form, if in a transition disk a super-Earth with a gas envelope containing a few percent of its mass may form. If the mergers happen too early runaway gas accretion may occur leading to the formation of a gas giant. The mergers begin when the dynamical friction due to the gas disk becomes insufficient to prevent collisions, a process that will begin earlier in a higher metallicity disk.[5] Alternatively gas accretion may be limited due to the envelopes not being in hydrostatic equilibrium, instead gas may flow through the envelope slowing its growth and delaying the onset of runaway gas accretion until the mass of the core reaches 15 Earth masses.[6]

  1. Baruteau, C.; Crida, A.; Paardekooper, S.-J.; Masset, F.; Guilet, J.; Bitsch, B.; Nelson, R.; Kley, W.; Papaloizou, J. (2014). 《Protostars and Planets VI, Chapter: Planet-Disk Interactions and Early Evolution of Planetary Systems》. 《Protostars and Planets Vi》. 667–689쪽. arXiv:1312.4293. Bibcode:2014prpl.conf..667B. doi:10.2458/azu_uapress_9780816531240-ch029. ISBN 9780816531240. S2CID 67790867. 
  2. Batygin, Konstantin; Bodenheimer, Peter H.; Laughlin, Gregory P. (2016). “In Situ Formation and Dynamical Evolution of Hot Jupiter Systems”. 《The Astrophysical Journal》 829 (2): 114. arXiv:1511.09157. Bibcode:2016ApJ...829..114B. doi:10.3847/0004-637X/829/2/114. S2CID 25105765. 
  3. D'Angelo, G.; Bodenheimer, P. (2016). “In Situ and Ex Situ Formation Models of Kepler 11 Planets”. 《The Astrophysical Journal》 828 (1): id. 33 (32 pp.). arXiv:1606.08088. Bibcode:2016ApJ...828...33D. doi:10.3847/0004-637X/828/1/33. S2CID 119203398. 
  4. Morbidelli, Alessandro; Raymond, Sean (2016). “Challenges in planet formation”. 《Journal of Geophysical Research: Planets》 121 (10): 1962–1980. arXiv:1610.07202. Bibcode:2016JGRE..121.1962M. doi:10.1002/2016JE005088. S2CID 119122001. 
  5. Lee, Eve J.; Chiang, Eugene (2016). “Breeding Super-Earths and Birthing Super-puffs in Transitional Disks”. 《The Astrophysical Journal》 817 (2): 90. arXiv:1510.08855. Bibcode:2016ApJ...817...90L. doi:10.3847/0004-637X/817/2/90. S2CID 118456061. 
  6. Lambrechts, Michiel; Lega, Elana (2017). “Reduced gas accretion on super-Earths and ice giants”. 《Astronomy and Astrophysics》 606: A146. arXiv:1708.00767. Bibcode:2017A&A...606A.146L. doi:10.1051/0004-6361/201731014. S2CID 118979289.