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• Part 1: NASA’s Kepler Mission and the parameter Earth
• Part 2: Update on the habitable zone and speculations on where Earth lies within it– Some of this is our work
• Part 3: How can we look for Earth-like planets and life in the not-too-distant future?– This is what we’d like to do eventually, with NASA’s
help. We can help them interpret the results
Kepler Mission
http://www.nmm.ac.uk/uploads/jpg/kepler.jpg
• This space-based telescope will point at a patch of the Milky Way and monitor the brightness of ~160,000 stars, looking for transits of Earth- sized (and other) planets• 105 precision photometry• 0.95-m aperture capable of detecting Earths• Launched: March 5, 2009• Died (mostly): April, 2013
Transit method• The light from the star
dims if a planet passes in front of it
• Jupiter’s diameter is 1/10th that of the Sun, so a Jupiter transit would diminish the sunlight by 1%
• Earth’s diameter is 1% that of the Sun, so an Earth transit decreases sunlight by 1 part in 104
• The plane of the planetary system must be favorably oriented– Transit probability is R*/a,
where R* is the star’s radius and a is the planet’s orbital distance
– Transit probability for our own Earth is 0.5%
Image from Wikipedia
Kepler target field: The stars in this field range from a fewhundred to a few thousand light years in distance
December 2011 Kepler data
Candidate label
Candidate size (RE)
Number of candidates
Earth-size Rp < 1.25 207
Super-Earths 1.25 < Rp < 2.0
680
Neptune-size 2.0 < Rp < 6.0
1181
Jupiter-size 6.0 < Rp < 15 203
Very-large-size
15 < Rp < 22.4
55
TOTAL 2326
• Classically, planets bigger than about 2 Earth radii (~10 Earth masses) were expected to capture gas during their formation and turn into gas or ice giants• We now suspect, based on planets whose masses have been determined, that the upper radius for rocky planets is more like 1.4 REarth
• We don’t just care about the sizes of the planets, though. We also care how far they are from their parent star
The (liquid water) habitable zone
http://www.dlr.de/en/desktopdefault.aspx/tabid-5170/8702_read-15322/8702_page-2/
• What our group is most interested in is planets that lie within the habitable zone, where liquid water can exist on a planet’s surface• The blue strip represents the zero-age-main-sequence HZ (which then moves outward as the stars age)
Definition of Earth
• Earth—the fraction of stars that have at least one rocky planet in their habitable zone– This is what we need to
know in order to design a space telescope to look for such planets around nearby stars
– We should be conservative when calculating Earth for this purpose, because we don’t want to undersize the telescope
Published Earth estimates• In November, 2013,
Petigura et al. published an estimate of Earth for K stars and (one)
late-G star• They got 0.22, but they
assumed a habitable zone of 0.5-2.0 AU, which is too wide, so a conservative estimate might be ~0.1
• By comparison, published estimates of Earth for M stars are of the order of 0.4-0.6 (Kasting et al., PNAS, 2014, and refs. therein)
Petigura et al., PNAS (2013)
AU
0.5 1.0 2.0
Conservative HZ
• The estimates for Earth are still changing, however, as new analyses are performed on the Kepler data
• Just this January, astronomers announced 8 new small (and maybe rocky) planets within the HZ
NewPreviouslyknown
Habitable zone updates• Within the past two
years, our group has recalculated HZ boundaries using updated 1-D climate models
• The main thing that has changed is the development of a new HITEMP database for H2O absorption coefficients (replacing the older HITRAN database)– The new database gives
more absorption of incoming sunlight at visible/near-IR wavelengths, thereby lowering a planet’s albedo
Goldblatt et al., Nature Geosciences (2013)
• We derived new correlated k-coefficients for CO2 and H2O and put them into our existing 1-D climate model
• The theoretical runaway greenhouse limit on the HZ inner edge moved farther out as a result
• But there is significant uncertainty about the location of the inner edge because the empirical ‘recent Venus’ limit is much closer in
Kopparapu et al., Ap. J. (2013)
3-D modeling of habitable zone boundaries
• Our 1-D models are almost certainly too pessimistic near the HZ inner edge because we assume that the troposphere is fully saturated and we neglect cloud feedback (but not the clouds themselves)
• 3-D climate models predict that the runaway greenhouse threshold is significantly higher because of the ‘radiator-fin’ behavior of the tropical Hadley cells
Leconte et al., Nature (2013)
Outgoing IR radiation
Most recent habitable zone
• Note the change in the x-axis from distance units to stellar flux units. This makes it easier to compare where different objects lie
Credit: Sonny Harman
Most recent habitable zone
• Also note that there is still a lot of uncertainty regarding the location of the inner edge
Conservative HZ
Credit: Sonny Harman
Most recent habitable zone
Optimistic HZ
Credit: Sonny Harman
• Also note that there is still a lot of uncertainty regarding the location of the inner edge
Identifying habitable planets
• We can speculate until we’re blue in the face about whether of the Kepler planets are habitable, but we won’t know anything until we are able to look at them (or at their somewhat closer analogs)– The average distance to
a Kepler target star is > 600 light years, so the planets found by Kepler will be difficult or impossible to characterize
JWST and TESS• NASA’s James Webb Space
Telescope, scheduled for launch in 2018, could in principle characterize Earth-size planets using transit spectroscopy– NASA’s TESS mission will look for
transiting habitable zone planets around nearby K and M stars in hopes of providing targets for JWST
• In practice, however, this is considered to be a scientific long-shot
• We want instead to look for non-transiting planets using direct imaging..
NASA’s James Webb Space Telescope
6.5 m
• Direct imaging means looking for the light reflected or emitted by a planet when it is beside its parent star (which is hard to do because stars are very bright, and planets are dim)• Such missions have been studied previously under the name of TPF (Terrestrial Planet Finder)• With such a telescope, we could also look for spectroscopic biomarkers (O2, O3, CH4) and try to infer whether life is present on such planets
TPF-I/Darwin
TPF-C
TPF-O
Terrestrial Planet Finder (TPF)
Visible or thermal-IR?
• Contrast ratio: 1010 in the visible 107 in the thermal-IR• Resolution: /D• Required aperture: ~8 m in the visible 80 m in the IR• NASA’s current plan is to do the visible mission first, maybe by the early 2030’s
≈ 1010
TPF-CTPF-I
≈ 107
Courtesy: Chas Beichman, JPL
Looking for life via the by-products of metabolism
• Green plants and algae (and cyanobacteria) produce oxgyen from photosynthesis: CO2 + H2O CH2O + O2
• Methanogenic bacteria produce methane CO2 + 4 H2 CH4 + 2 H2O
• CH4 and O2 are out of thermodynamic equilibrium by 20 orders of magnitude!* Hence, their simultaneous presence is strong evidence for life
O2
CH4
*As first pointed out by James Lovelock (Nature, 1965)
Visible spectrum of Earth
Integrated light of Earth, reflected from dark side of moon: Rayleigh
scattering, chlorophyll, O2, O3, H2O
Ref.: Woolf, Smith, Traub, & Jucks, ApJ 2002; also Arnold et al. 2002
Visible spectrum of Earth
• Note that one can see O2 but not CH4 or N2O. So, this leads to an interesting question
Ref.: Woolf, Smith, Traub, & Jucks, ApJ 2002; also Arnold et al. 2002
‘’False positives’ for life• Can high atmospheric O2
concentrations build up abiotically on an exoplanet?
• Recent calculations (at right) suggest that this might be especially easy on a planet orbiting an M star– Lower near-UV flux less
photolysis of H2O less catalytic recombination of CO and O
• Photochemical model calculations are underway to determine if and when one needs to worry about this problem
Sun M star
F. Tian et al., EPSL (2014)
Conclusions• The Kepler dataset is a veritable gold mine and
has clearly shown that Earth-sized planets exist in the habitable zones of many main sequence stars– Earth is still being evaluated for different types of
stars, but is very unlikely to be below 0.1• Calculations of habitable zone boundaries
using 3-D climate models are currently underway and are improving. More work to be done..
• Ultimately, we need to fly some kind of TPF mission to directly image Earth-sized planets, to characterize their atmospheres, and to look for evidence of life