614 research outputs found
Water On -and In- Terrestrial Planets
Earth has a unique surface character among Solar System worlds. Not only does
it harbor liquid water, but also large continents. An exoplanet with a similar
appearance would remind us of home, but it is not obvious whether such a planet
is more likely to bear life than an entirely ocean-covered waterworld---after
all, surface liquid water defines the canonical habitable zone. In this
proceeding, I argue that 1) Earth's bimodal surface character is critical to
its long-term climate stability and hence is a signpost of habitability, and 2)
we will be able to constrain the surface character of terrestrial exoplanets
with next-generation space missions.Comment: 4 pages, 1 figure; to appear in the proceedings of the Comparative
Climates of Terrestrial Planets II conferenc
A Model for Thermal Phase Variations of Circular and Eccentric Exoplanets
We present a semi-analytic model atmosphere for close-in exoplanets that
captures the essential physics of phase curves: orbital and viewing geometry,
advection, and re-radiation. We calibrate the model with the well-characterized
transiting planet, HD 189733b, then compute light curves for seven of the most
eccentric transiting planets. We present phase variations for a variety of
different radiative times and wind speeds. In the limit of instant
re-radiation, the light curve morphology is entirely dictated by the planet's
eccentricity and argument of pericenter: the light curve maximum leads or
trails the eclipse depending on whether the planet is receding from or
approaching the star at superior conjunction, respectively. For a planet with
non-zero radiative timescales, the phase peak occurs early for super- rotating
winds, and late for sub-rotating winds. We find that for a circular orbit, the
timing of the phase variation maximum with respect to superior conjunction
indicates the direction of the dominant winds, but cannot break the degeneracy
between wind speed and radiative time. For circular planets the phase minimum
occurs half an orbit away from the phase maximum -despite the fact that the
coolest longitudes are always near the dawn terminator- and therefore does not
convey any additional information. In general, increasing the advective
frequency or the radiative time has the effect of reducing the peak-to-trough
amplitude of phase variations, but there are interesting exceptions to these
trends. Lastly, eccentric planets with orbital periods significantly longer
than their radiative time exhibit "ringing" whereby the hot spot generated at
periastron rotates in and out of view. The existence of ringing makes it
possible to directly measure the wind speed (the frequency of the ringing) and
the radiative time constant (the damping of the ringing).Comment: 13 pages, 13 figures, accepted for publication in Ap
Revisiting the Energy Budget of WASP-43b: Enhanced day-night heat transport
The large day--night temperature contrast of WASP-43b has so far eluded
explanation. We revisit the energy budget of this planet by considering the
impact of reflected light on dayside measurements, and the physicality of
implied nightside temperatures. Previous analyses of the infrared eclipses of
WASP-43b have assumed reflected light from the planet is negligible and can be
ignored. We develop a phenomenological eclipse model including reflected light,
thermal emission, and water absorption, and use it to fit published Hubble and
Spitzer eclipse data. We infer a near-infrared geometric albedo of 27
and a cooler dayside temperature of K. Additionally, we perform
lightcurve inversion on the three published orbital phase curves of WASP-43b
and find that each requires unphysical, negative flux on the nightside. By
requiring non-negative brightnesses at all longitudes, we correct the
unphysical parts of the maps and obtain a much hotter nightside effective
temperature of K. The cooler dayside and hotter nightside
suggests a heat recirculation efficiency of for WASP-43b, essentially
the same as for HD 209458b, another hot Jupiter with nearly the same
temperature. Our analysis therefore reaffirms the trend that planets with lower
irradiation temperatures have more efficient day-night heat transport.
Moreover, we note that 1) reflected light may be significant for many near-IR
eclipse measurements of hot Jupiters, and 2) phase curves should be fit with
physically possible longitudinal brightness profiles --- it is insufficient to
only require that the disk-integrated lightcurve be non-negative.Comment: Accepted for publication in ApJL. 7 pages, 4 figure
Knot a Bad Idea: Testing BLISS Mapping for Spitzer Space Telescope Photometry
Much of transiting exoplanet science relies on high-precision photometry. The
current generation of instruments can exhibit sensitivity variations greater
than the astrophysical signals. For the InfraRed Array Camera (IRAC) on the
Spitzer Space Telescope, a popular way to handle this is
BiLinearly-Interpolated Subpixel Sensitivity (BLISS) mapping. As part of a
Markov Chain Monte Carlo (MCMC), BLISS mapping estimates the sensitivity at
many locations (knots) on the pixel, then interpolates to the target star's
centroids. We show that such embedded optimization schemes can misfit or bias
parameters. Thus, we construct a model of eclipse light
curves to test the accuracy and precision of BLISS mapping. We compare standard
BLISS mapping to a variant where the knots are fit during the MCMC, as well as
to a polynomial model. Both types of BLISS mapping give similar eclipse depths,
and we find that standard knots behave like real parameters. Standard BLISS
mapping is therefore a reasonable shortcut to fitting for knots in an MCMC.
BLISS maps become inaccurate when the photon noise is low, but typically
approximate the real sensitivity well. We also find there is no perfect method
for choosing the ideal number of BLISS knots to use on given data. BLISS
mapping gives fits that are usually more accurate than precise (i.e. they are
overly conservative), and the routine is more precise than polynomial models
for significant eclipses or pixels with more varied sensitivities. BLISS
mapping has better predictive power for most of these particular synthetic
data, depending on how one treats time-correlated residuals. Overall, we
conclude that BLISS mapping can be a reasonable sensitivity model for IRAC
photometry.Comment: 32 pages, 13 figures; Accepted by PASP 9/26/16. Major updates: higher
amplitude for main detector signals, estimating good number of BLISS knots
for given data, more/better synthetic light curves, trying projected
sensitivity along pixel axes, uncertainties in Figures 10-13. Most edits in
Abstract, Sections 4-6. New findings but main conclusion same (i.e. BLISS
Mapping can be acceptable
The Feeding Zones of Terrestrial Planets and Insights into Moon Formation
[Abridged] We present an extensive suite of terrestrial planet formation
simulations that allows quantitative analysis of the stochastic late stages of
planet formation. We quantify the feeding zone width, Delta a, as the
mass-weighted standard deviation of the initial semi-major axes of the
planetary embryos and planetesimals that make up the final planet. The size of
a planet's feeding zone in our simulations does not correlate with its final
mass or semi-major axis, suggesting there is no systematic trend between a
planet's mass and its volatile inventory. Instead, we find that the feeding
zone of any planet more massive than 0.1M_Earth is roughly proportional to the
radial extent of the initial disk from which it formed: Delta
a~0.25(a_max-a_min), where a_min and a_max are the inner and outer edge of the
initial planetesimal disk. These wide stochastic feeding zones have significant
consequences for the origin of the Moon, since the canonical scenario predicts
the Moon should be primarily composed of material from Earth's last major
impactor (Theia), yet its isotopic composition is indistinguishable from Earth.
In particular, we find that the feeding zones of Theia analogs are
significantly more stochastic than the planetary analogs. Depending on our
assumed initial distribution of oxygen isotopes within the planetesimal disk,
we find a ~5% or less probability that the Earth and Theia will form with an
isotopic difference equal to or smaller than the Earth and Moon's. In fact we
predict that every planetary mass body should be expected to have a unique
isotopic signature. In addition, we find paucities of massive Theia analogs and
high velocity moon-forming collisions, two recently proposed explanations for
the Moon's isotopic composition. Our work suggests that there is still no
scenario for the Moon's origin that explains its isotopic composition with a
high probability event.Comment: 16 pages, 22 figures, accepted for publication in Icarus; fixed typo
Wavelength Does Not Equal Pressure: Vertical Contribution Functions and their Implications for Mapping Hot Jupiters
Multi-band phase variations in principle allow us to infer the longitudinal
temperature distributions of planets as a function of height in their
atmospheres. For example, 3.6 micron emission originates from deeper layers of
the atmosphere than 4.5 micron due to greater water vapor absorption at the
longer wavelength. Since heat transport efficiency increases with pressure, we
expect thermal phase curves at 3.6 micron to exhibit smaller amplitudes and
greater phase offsets than at 4.5 micron; this trend is not observed. Of the
seven hot Jupiters with full-orbit phase curves at 3.6 and 4.5 micron, all have
greater phase amplitude at 3.6 micron than at 4.5 micron, while four of seven
exhibit a greater phase offset at 3.6 micron. We use a 3D
radiative-hydrodynamic model to calculate theoretical phase curves of HD
189733b, assuming thermo-chemical equilibrium. The model exhibits temperature,
pressure, and wavelength dependent opacity, primarily driven by carbon
chemistry: CO is energetically favored on the dayside, while CH4 is favored on
the cooler nightside. Infrared opacity therefore changes by orders of magnitude
between day and night, producing dramatic vertical shifts in the
wavelength-specific photospheres, which would complicate eclipse or phase
mapping with spectral data. The model predicts greater relative phase amplitude
and greater phase offset at 3.6 micron than at 4.5 micron, in agreement with
the data. Our model qualitatively explains the observed phase curves, but is in
tension with current thermo-chemical kinetics models that predict zonally
uniform atmospheric composition due to transport of CO from the hot regions of
the atmosphere.Comment: 9 pages, 5 figures, accepted for publications in ApJ Letter
Water Cycling Between Ocean and Mantle: Super-Earths Need Not be Waterworlds
Large terrestrial planets are expected to have muted topography and deep
oceans, implying that most super-Earths should be entirely covered in water,
so-called waterworlds. This is important because waterworlds lack a silicate
weathering thermostat so their climate is predicted to be less stable than that
of planets with exposed continents. In other words, the continuously habitable
zone for waterworlds is much narrower than for Earth-like planets. A planet's
water is partitioned, however, between a surface reservoir, the ocean, and an
interior reservoir, the mantle. Plate tectonics transports water between these
reservoirs on geological timescales. Degassing of melt at mid-ocean ridges and
serpentinization of oceanic crust depend negatively and positively on seafloor
pressure, respectively, providing a stabilizing feedback on long-term ocean
volume. Motivated by Earth's approximately steady-state deep water cycle, we
develop a two-box model of the hydrosphere and derive steady-state solutions to
the water partitioning on terrestrial planets. Critically, hydrostatic seafloor
pressure is proportional to surface gravity, so super-Earths with a deep water
cycle will tend to store more water in the mantle. We conclude that a
tectonically active terrestrial planet of any mass can maintain exposed
continents if its water mass fraction is less than ~0.2%, dramatically
increasing the odds that super-Earths are habitable. The greatest source of
uncertainty in our study is Earth's current mantle water inventory: the greater
its value, the more robust planets are to inundation. Lastly, we discuss how
future missions can test our hypothesis by mapping the oceans and continents of
massive terrestrial planets.Comment: 8 pages, 2 figures, ApJ in pres
Eccentricity is Not Responsible for Odd Harmonics in HAT-P-7 and Kepler-13A
The exquisite photometry of Kepler has revealed reflected light from
exoplanets, tidal distortion of host stars and Doppler beaming of a star's
light due to its motion (Borucki 2016; Demory et al. 2012; Welsh et al. 2010;
Bloemen et al. 2012). Esteves et al. (2013, 2015) and Shporer et al. (2014)
reported additional odd harmonics in the light curves of two hot Jupiters:
HAT-P-7b and Kepler-13Ab. They measured non-zero power at three times the
orbital frequency that persisted while the planet was eclipsed and hence must
originate in the star (Esteves et al. 2015). Penoyre & Sandford (2018) showed
that orbital eccentricity could result in time-dependent tidal deformation of
the star that manifests itself at three times the orbital frequency and
suggested this could be the origin of the measured odd modes. In this Research
Note, we show that the small orbital eccentricities of HAT-P-7b and Kepler-13Ab
cannot generate the odd harmonics observed in these systems. Esteves et al.
(2015) hypothesized that the odd modes could be due to tidal distortion of the
star if its spin is misaligned with the system's orbital motion, as is the case
in both of these systems (Benomar et al. 2014; Herman et al. 2018), but this
mechanism has yet to be verified theoretically or numerically.Comment: 2 pages, 1 figure, RNAAS in pres
Brief Follow-up on Recent Studies of Theia's Accretion
Kaib & Cowan (2015) recently used terrestrial planet formation simulations to
conclude that the moon-forming impactor (Theia) had only a ~5% or less chance
of having the same oxygen isotope composition as Earth, while
Mastrobuono-Battisti et al. (2015) used seemingly similar simulations and
methods to arrive at a higher value of ~20% or more. Here we derive the results
of both papers from a single set of simulations. Compared to Kaib & Cowan
(2015), the analysis of Mastrobuono-Battisti et al. (2015) systematically
yields more massive Theia analogs and imposes flatter isotopic gradients across
the original protoplanetary disk. Both of these effects diminish isotopic
differences between Earth and Theia analogs. While it is notoriously difficult
to produce systems resembling our actual terrestrial planets, the analysis of
Kaib & Cowan (2015) more often selects and analyzes Earth and Mars analogs at
orbital locations near the real planets. Given this, we conclude that the
greater isotopic differences between Earth and Theia found in Kaib & Cowan
(2015) better reflect the predictions of terrestrial planet formation models.
Finally, although simulation uncertainties and a terrestrial contribution to
Moon formation enhance the fraction of Theia analogs consistent with the
canonical giant impact hypothesis, this fraction still remains in the 5-8%
range.Comment: 5 pages, 4 figures, accepted to Icaru
Increased Heat Transport in Ultra-Hot Jupiter Atmospheres Through H Dissociation/Recombination
A new class of exoplanets is beginning to emerge: planets whose dayside
atmospheres more closely resemble stellar atmospheres as most of their
molecular constituents dissociate. The effects of the dissociation of these
species will be varied and must be carefully accounted for. Here we take the
first steps towards understanding the consequences of dissociation and
recombination of molecular hydrogen (H) on atmospheric heat recirculation.
Using a simple energy balance model with eastward winds, we demonstrate that
H dissociation/recombination can significantly increase the daynight
heat transport on ultra-hot Jupiters (UHJs): gas giant exoplanets where
significant H dissociation occurs. The atomic hydrogen from the highly
irradiated daysides of UHJs will transport some of the energy deposited on the
dayside towards the nightside of the planet where the H atoms recombine into
H; this mechanism bears similarities to latent heat. Given a fixed wind
speed, this will act to increase the heat recirculation efficiency;
alternatively, a measured heat recirculation efficiency will require slower
wind speeds after accounting for H dissociation/recombination.Comment: 8 pages, 5 figures, accepted for publication in ApJ
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