Planets of the solar system

terrestrial planets: Mercury, Venus, Earth, Mars)high density: 4 – 5 g/cm3, no He,H-gas, Mg,Si,O mantle + Fe core

giant planets (Jupiter, Saturn, Uranus, Neptune)low density: 0.7 – 1.3 g/cm3, H, He atmosphere + rocky core

ice giants (Uranus and Neptune)density: 1.5-2 g/cm3, H, He atmosphere + C,O-rich core1

Astrophysics I, Lecture Slides – Chapter 3, ETH Zurich

Motion of the sun as seen from 10 pc

2

51 Peg b detection by Mayor and Queloz

3

Multiplanet system HD40307

Mayor et al. 2009, A&A 493, 639

4

HAT-P-7 b transit light curve observed by KEPLER satellite

5

KEPLER transits: period-radius diagram

RJ

RN

(from Batalha et al. 2013, ApJS 204, 24) 6

Transit timing variations for KOI-872

- transit model (lines) and - data points of 14 transits

- timing variations are ±1 hr

Periods of planets:- 33.6 days for transiting planet- 57 days for unseen planet

(Nesvorny et al. 2012, Science 336, 1133)

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MP-RP and MP-ρ diagrams for exoplanets

50% high, 50% low incident flux, borderline = 800 times incident flux on Earth

(from Weiss et al. 2013, ApJ 768,14)8

Direct imaging of HR 8799 system

2008

2010Slide 6.1W.M. Keck Observatory 9

Spectral flux of solar system planets and the sun

from S. SeagerExoplanets atmospheres

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Secondary eclipse spectra

Secondary eclipse observations compared with models• HD 189733b data points (spectroscopy – black, photometry – red) • Solid lines – models from Burrows et al. 2007, 2008.

from Grillmair et al. 2008

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