Measuring the Atmospheres of (the best!) Earth-sized Planets with JWST
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1 Measuring the Atmospheres of (the best!) Earth-sized Planets with JWST Caroline Morley Sagan Fellow, Harvard University Laura Kreidberg Zafar Rustamkulov Ty Robinson Photo by C. Morley Top of Mt Whitney, California, on Planet Earth
2 Terrestrial planet atmospheres in the solar system are diverse and controlled by many physical processes Venus Earth Titan Mars 100 bar CO 2 sulfuric acid clouds no oceans surface is hellscape 1 bar N 2 /O 2 oceans & hydro cycle surface is nice 1 bar N 2 methane lakes and hydro cycle surface is (really) cold 6 mbar CO 2 former liquid water surface is cold volatile delivery interior composition planet mass atm loss (ocean loss) UV flux (photochemistry)
3 How do terrestrial atmospheres form and evolve in planetary systems? Two big problems: 1. very small sample size 2. all around the same star
4 For the first time ever, we have discovered temperate, terrestrial planets for which we have a fighting shot of characterizing their atmospheres + GJ 1132b LHS 1140b all small planets around some of the smallest nearby stars Gillon et al Berta-Thompson et al Dittmann et al. 2017
5 Outline generating a diverse set of model planet spectra (transmission and emission) simulating observations with JWST +
6 Good experimental setup: these planets span sizes from 0.7 to 1.4 R Earth and T eq from ~150 to 500+ K. albedo=0.0 (dark) albedo=0.3 (Earth) albedo=0.7 (Venus)
7 Some masses appear to be Earth-like (rock/iron); others may be low density? Earth-like mass-radius relationship measured
8 We construct a grid with a range of plausible compositions/surface pressures Compositions Surface pressures Venus Earth & Titan Mars Pluto ( bar)
9 We construct atmospheres with simple temperature structures and chemistry isothermal upper atmosphere 0.1 bar tropopause (Robinson & Catling 2014) adiabatic deep atmosphere
10 We model the molecular compositions assuming chemical equilibrium elemental abundances molecular abundances 1 bar
11 Earth-based models are dominated by H 2 O, plus CO 2, O 2. Titan-based models are dominated by CH 4, plus NH 3, CO, H 2 O. Venus-based models are dominated by CO 2, plus SO 2, H 2 O.
12 Surface temperature increases with surface pressure; depends on composition and assumed albedo.
13 Planet composition strongly effects the emergent spectrum, including where bright/faint windows are. (surface pressure = 1 bar)
14 Transmission spectra of the different compositions show a variety of spectral features (CO 2, H 2 O, CH 4 )
15 Transmission spectra for all 9 planets; uncertainties in the planet s mass strongly affect the feature amplitude. mass using rock/iron composition measured mass
16 For bar atmospheres, thermal emission spectra are much more sensitive to surface pressure than transmission spectra emission transmission
17 All ~400 models (including emission spectra, transmission spectra, and MIRI eclipse depths) are publicly available online!
18 Outline generating a diverse set of model planet spectra (transmission and emission) simulating observations with JWST +
19 We (Laura Kreidberg) simulate JWST observations with PandExo for near-ir (NIRSpec) and mid-ir (MIRI). rock/iron composition (measured mass)
20 We (Laura Kreidberg) simulate JWST observations with PandExo for near-ir (NIRSpec) and mid-ir (MIRI). 1. A number of these planets may be good transmission spectroscopy targets: TRAPPIST-1b, d, e, f, g, h? GJ 1132b rock/iron composition (measured mass)
21 We (Laura Kreidberg) simulate JWST observations with PandExo for near-ir (NIRSpec) and mid-ir (MIRI). 2. We have at least 2 great thermal emission spectroscopy targets (TRAPPIST-1b and GJ 1132b) rock/iron composition (measured mass)
22 We (Laura Kreidberg) simulate JWST observations with PandExo for near-ir (NIRSpec) and mid-ir (MIRI). 3. We need more precise constraints on planet s masses to plan JWST observations of rocky planets rock/iron composition (measured mass)
23 For the best targets, we can detect spectral features and discern compositions 6 transits TRAPPIST-1b 9 eclipses
24 Conclusions With dedicated JWST observations of the best systems, we can detect the atmospheres of terrestrial planets for the first time We generated a diverse set of model transmission & emission spectra based on solar system planet compositions that are published as a community resource JWST simulations show that this will be a significant investment of resources, but we can (potentially) measure differences in compositions, temperatures, and surface pressures +
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Meteorites. A Variety of Meteorite Types. Ages and Compositions of Meteorites. Meteorite Classification
Meteorites A meteor that survives its fall through the atmosphere is called a meteorite Hundreds fall on the Earth every year Meteorites do not come from comets First documented case in modern times was