HAT-P-11b

Coordenadas: Sky map 19h 50m 50.25s, +48° 04′ 51.1″

HAT-P-11b
Exoplaneta Estrelas com exoplanetas

Comparação de tamanho de HAT-P-11b (cinza) com Netuno.
Estrela mãe
Estrela HAT-P-11
Constelação Cygnus
Ascensão reta 19h 50m 50.25s[1]
Declinação +48° 04′ 51.1″[1]
Magnitude aparente 9.59[2]
Distância 122 ± 4[1] anos-luz
37 ± 1[1] pc
Tipo espectral K4[2]
Elementos orbitais
Semieixo maior 0.053+0.0002
−0.0008 UA
Periastro 0.043 UA
Apoastro 0.063 UA
Excentricidade 0.198 ± 0.046
Período orbital 4.8878045 ± 0.0000043[3] d
Velocidade orbital 118 km/s
Inclinação 88.5 ± 0.6°
Argumento do periastro 355.2 ± 17.3°
Características físicas
Massa 0.081 ± 0.009 MJ
26 ± 3 M🜨
Raio 0.422 ± 0.014 RJ
4.58 ± 0.15 R🜨
Densidade 1440 g/cm³
Gravidade superficial 1.20 m/s²
Temperatura 878 ± 15 K
Descoberta
Data da descoberta 2 de janeiro de 2009
Descobridores Bakos et al.
Método de detecção Por trânsito (HATNet)
Estado da descoberta Publicado

HAT-P-11b (ou Kepler-3b) é um exoplaneta que orbita a estrela HAT-P-11. Este planeta foi descoberto pelo método de trânsito e submetido à publicação em 2 de janeiro de 2009.

Este planeta está localizado a aproximadamente 122 anos-luz de distância da Terra[1] na constelação de Cygnus, orbitando a estrela HAT-P-11 de magnitude 9 de classe K. Este planeta foi o menor planeta em trânsito conhecido quando descoberto pela primeira vez, com um raio de cerca de 5 vezes o da Terra; mas é mais massivo do que Gliese 436 bque tem uma massa de 26 vezes o da Terra. Este planeta orbita sobre a mesma distância da estrela 51 Pegasi b, como é de 51 Pegasi, típico de planetas em trânsito. No entanto, a órbita deste planeta é excêntrico, em torno de 0.198, excepcionalmente alta para Netunos quentes. A órbita de HAT-P-11b é também altamente inclinado, com uma inclinação de cerca de 103° em relação à rotação de sua estrela.[4][5]

O sistema de HAT-P-11 esta dentro do campo de visão da sonda espacial Kepler.[2]

Sua velocidade radial está à deriva e isso pode ser resultado de um planeta ainda não descoberto no sistema.[2]

O planeta se encaixa aos modelos em 90% elementos pesados​​. Temperatura esperada é de 878 ± 15 K.[2] Temperatura atual prevista a espera de cálculos de trânsito secundário.

Referências

  1. ↑ a b c d e van Leeuwen, F. (2007). «Validation of the new Hipparcos reduction». Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752Acessível livremente. doi:10.1051/0004-6361:20078357  Vizier catalog entry
  2. ↑ a b c d e Bakos, G. Á.; et al. (2010). «HAT-P-11b: A Super-Neptune Planet Transiting a Bright K Star in the Kepler Field». The Astrophysical Journal. 710 (2): 1724–1745. Bibcode:2010ApJ...710.1724B. arXiv:0901.0282Acessível livremente. doi:10.1088/0004-637X/710/2/1724 
  3. ↑ Dittmann, Jason A.; Close, Laird M.; Green, Elizabeth M.; Scuderi, Louis J.; Males, Jared R. (2009). «Follow-up Observations of the Neptune Mass Transiting Extrasolar Planet HAT-P-11b». The Astrophysical Journal. 699: L48–L51. Bibcode:2009ApJ...699L..48D. arXiv:0905.1114v2Acessível livremente. doi:10.1088/0004-637X/699/1/L48 
  4. ↑ «Inclined Orbits Prevail in Exoplanetary Systems». 12 de janeiro de 2011 
  5. ↑ Roberto Sanchis-Ojeda, Josh N. Winn, Daniel C. Fabrycky (2012). «Starspots and spin-orbit alignment for Kepler cool host stars». Bibcode:2013AN....334..180S. arXiv:1211.2002Acessível livremente. doi:10.1002/asna.201211765 

Ligações externas

Media relacionados com HAT-P-11b no Wikimedia Commons

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