The atmospheres of short-period terrestrial exoplanets

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vendredi 10 septembre 2010 HZ: Selsis, Kasting et al, 2007
Habitability around M stars • Strong tidal interaction with the star. Slow rotation. Fast tidal locking if circular orbit. The atmosphere can freeze out on the dark hemisphere if heat redistribution (circulation, greenhouse effect) not efficient enough. (A dense atmosphere can prevent synchronization, see Correia et al., 2008). • Planets in the HZ are subjected to high and long-lasting X-EUV radiations, strong stellar winds (Scalo et al., 2007), frequent CMEs (Kodatchenko et al., 2007) and flares Fast atmospheric escape Do terrestrial planets in the HZ of M stars have an atmosphere ? vendredi 10 septembre 2010
Page 1: The atmospheres of short-period ter
Page 5 and 6: stellar photon noise only instrumen
Page 7 and 8: vendredi 10 septembre 2010 Belu et
Page 9 and 10: The detection and basic characteriz
Page 11 and 12: Animation made with the data from t
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Page 19 and 20: IR light phase curve curve and clim
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Page 23 and 24: Eccentric planets max max vendredi
Page 25 and 26: IR Earth Vis Palle et al., 2008 ven
Page 27 and 28: Test case for a non-transiting hot
Page 29 and 30: no atmosphere 3.6 µm 4.3 µm 5.9
Page 31 and 32: 1 bar (CO2) 3.6 µm 4.3 µm 5.9 µm
Page 33 and 34: 8.7 µm no atmosphere 0.1 bar (CO2)
Page 35 and 36: 0.1 bar CO2 1 bar CO2 10 bar CO2 ve
Page 37 and 38: Altitude 10 bar (CO2) color = gas t
Page 39 and 40: dayside low-res spectrum of the pla
Page 41 and 42: 0.1 bar CO2 1 bar CO2 10 bar CO2 SN
Page 43 and 44: ideal SNR with a 6m telescope integ
Page 45: - SNR calculations for phasecurve d

The atmospheres of short-period terrestrial exoplanets

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