477 research outputs found
On the Emergent Spectra of Hot Protoplanet Collision Afterglows
We explore the appearance of terrestrial planets in formation by studying the
emergent spectra of hot molten protoplanets during their collisional formation.
While such collisions are rare, the surfaces of these bodies may remain hot at
temperatures of 1000-3000 K for up to millions of years during the epoch of
their formation. These object are luminous enough in the thermal infrared to be
observable with current and next generation optical/IR telescopes, provided
that the atmosphere of the forming planet permits astronomers to observe
brightness temperatures approaching that of the molten surface. Detectability
of a collisional afterglow depends on properties of the planet's atmosphere --
primarily on the mass of the atmosphere. A planet with a thin atmosphere is
more readily detected, because there is little atmosphere to obscure the hot
surface. Paradoxically, a more massive atmosphere prevents one from easily
seeing the hot surface, but also keeps the planet hot for a longer time. In
terms of planetary mass, more massive planets are also easier to detect than
smaller ones because of their larger emitting surface areas. We present
preliminary calculations assuming a range of protoplanet masses (1-10
M_\earth), surface pressures (1-1000 bar), and atmospheric compositions, for
molten planets with surface temperatures ranging from 1000 to 1800 K, in order
to explore the diversity of emergent spectra that are detectable. While current
8- to 10-m class ground-based telescopes may detect hot protoplanets at wide
orbital separations beyond 30 AU (if they exist), we will likely have to wait
for next-generation extremely large telescopes or improved diffraction
suppression techniques to find terrestrial planets in formation within several
AU of their host stars.Comment: 28 pages, 6 figures, ApJ manuscript format, accepted into the Ap
A Search for a Sub-Earth Sized Companion to GJ 436 and a Novel Method to Calibrate Warm Spitzer IRAC Observations
We discovered evidence for a possible additional 0.75 R_Earth transiting
planet in the NASA EPOXI observations of the known M dwarf exoplanetary system
GJ 436. Based on an ephemeris determined from the EPOXI data, we predicted a
transit event in an extant Spitzer Space Telescope 8 micron data set of this
star. Our subsequent analysis of those Spitzer data confirmed the signal of the
predicted depth and at the predicted time, but we found that the transit depth
was dependent on the aperture used to perform the photometry. Based on these
suggestive findings, we gathered new Warm Spitzer Observations of GJ 436 at 4.5
microns spanning a time of transit predicted from the EPOXI and Spitzer 8
micron candidate events. The 4.5 micron data permit us to rule out a transit at
high confidence, and we conclude that the earlier candidate transit signals
resulted from correlated noise in the EPOXI and Spitzer 8 micron observations.
In the course of this investigation, we developed a novel method for correcting
the intrapixel sensitivity variations of the 3.6 and 4.5 micron channels of the
Infrared Array Camera (IRAC) instrument. We demonstrate the sensitivity of Warm
Spitzer observations of M dwarfs to confirm sub-Earth sized planets. Our
analysis will inform similar work that will be undertaken to use Warm Spitzer
observations to confirm rocky planets discovered by the Kepler mission.Comment: 22 pages, 8 figures, accepted for publication in PAS
Detection of Thermal Emission from a Super-Earth
We report on the detection of infrared light from the super-Earth 55 Cnc e,
based on four occultations obtained with Warm Spitzer at 4.5 microns. Our data
analysis consists of a two-part process. In a first step, we perform individual
analyses of each dataset and compare several baseline models to optimally
account for the systematics affecting each lightcurve. We apply independent
photometric correction techniques, including polynomial detrending and
pixel-mapping, that yield consistent results at the 1-sigma level. In a second
step, we perform a global MCMC analysis including all four datasets, that
yields an occultation depth of 131+-28ppm, translating to a brightness
temperature of 2360+-300 K in the IRAC-4.5 micron channel. This occultation
depth suggests a low Bond albedo coupled to an inefficient heat transport from
the planetary dayside to the nightside, or else possibly that the 4.5-micron
observations probe atmospheric layers that are hotter than the maximum
equilibrium temperature (i.e., a thermal inversion layer or a deep hot layer).
The measured occultation phase and duration are consistent with a circular
orbit and improves the 3-sigma upper limit on 55 Cnc e's orbital eccentricity
from 0.25 to 0.06.Comment: Accepted to ApJL on April, 6th 201
A Precise Water Abundance Measurement for the Hot Jupiter WASP-43b
The water abundance in a planetary atmosphere provides a key constraint on
the planet's primordial origins because water ice is expected to play an
important role in the core accretion model of planet formation. However, the
water content of the Solar System giant planets is not well known because water
is sequestered in clouds deep in their atmospheres. By contrast, short-period
exoplanets have such high temperatures that their atmospheres have water in the
gas phase, making it possible to measure the water abundance for these objects.
We present a precise determination of the water abundance in the atmosphere of
the 2 short-period exoplanet WASP-43b based on thermal
emission and transmission spectroscopy measurements obtained with the Hubble
Space Telescope. We find the water content is consistent with the value
expected in a solar composition gas at planetary temperatures (0.4-3.5x solar
at 1 confidence). The metallicity of WASP-43b's atmosphere suggested
by this result extends the trend observed in the Solar System of lower metal
enrichment for higher planet masses.Comment: Accepted to ApJL; this version contains three supplemental figures
that are not included in the published paper. See also our companion paper
"Thermal structure of an exoplanet atmosphere from phase-resolved emission
spectroscopy" by Stevenson et a
The EXPLORE Project I: A Deep Search for Transiting Extrasolar Planets
(Abridged) We discuss the design considerations of the EXPLORE (EXtra-solar
PLanet Occultation REsearch) project, a series of transiting planet searches
using 4-m-class telescopes to continuously monitor a single field of stars in
the Galactic Plane in each ~2 week observing campaign. We discuss the general
factors which determine the efficiency and the number of planets found by a
transit search, including time sampling strategy and field selection. The
primary goal is to select the most promising planet candidates for radial
velocity follow-up observations. We show that with very high photometric
precision light curves that have frequent time sampling and at least two
detected transits, it is possible to uniquely solve for the main parameters of
the eclipsing system (including planet radius) based on several important
assumptions about the central star. Together with a measured spectral type for
the star, this unique solution for orbital parameters provides a powerful
method for ruling out most contaminants to transiting planet candidates. For
the EXPLORE project, radial velocity follow-up observations for companion mass
determination of the best candidates are done on 8-m-class telescopes within
two or three months of the photometric campaigns. This same-season follow-up is
made possible by the use of efficient pipelines to produce high quality light
curves within weeks of the observations. We conclude by presenting early
results from our first search, EXPLORE I, in which we reached <1% rms
photometric precision (measured over a full night) on ~37,000 stars to I <=
18.2.Comment: accepted by ApJ. Main points unchanged but more thorough discussion
of some issues. 36 pages, including 14 figure
Thermodynamic Limits on Magnetodynamos in Rocky Exoplanets
To ascertain whether magnetic dynamos operate in rocky exoplanets more
massive or hotter than the Earth, we developed a parametric model of a
differentiated rocky planet and its thermal evolution. Our model reproduces the
established properties of Earth's interior and magnetic field at the present
time. When applied to Venus, assuming that planet lacks plate tectonics and has
a dehydrated mantle with an elevated viscosity, the model shows that the dynamo
shuts down or never operated. Our model predicts that at a fixed planet mass,
dynamo history is sensitive to core size, but not to the initial inventory of
long-lived, heat-producing radionuclides. It predicts that rocky planets larger
than 2.5 Earth masses will not develop inner cores because the
temperature-pressure slope of the iron solidus becomes flatter than that of the
core adiabat. Instead, iron "snow" will condense near or at the top of these
cores, and the net transfer of latent heat upwards will suppress convection and
a dynamo. More massive planets can have anemic dynamos due to core cooling, but
only if they have mobile lids (plate tectonics). The lifetime of these dynamos
is shorter with increasing planet mass but longer with higher surface
temperature. Massive Venus-like planets with stagnant lids and more viscous
mantles will lack dynamos altogether. We identify two alternative sources of
magnetic fields on rocky planets: eddy currents induced in the hot or molten
upper layers of planets on very short period orbits, and dynamos in the ionic
conducting layers of "ocean" planets with ~10% mass in an upper mantle of water
(ice).Comment: Accepted to The Astrophysical Journa
Vegetation and floristics of a lowland tropical rainforest in northeast Australia
Background: Full floristic data, tree demography, and biomass estimates incorporating non-tree life forms are seldom collected and reported for forest plots in the tropics. Established research stations serve as important repositories of such biodiversity and ecological data. With a canopy crane setup within a tropical lowland rainforest estate, the 42-ha Daintree Rainforest Observatory (DRO) in Cape Tribulation, northern Australia is a research facility of international significance. We obtained an estimate of the vascular plant species richness for the site, by surveying all vascular plant species from various mature-phase, remnant and open vegetation patches within the site. We also integrate and report the demography and basal areas of trees ≥ 10 cm diameter at breast height (dbh) in a new 1- ha core plot, an extension to the pre-existing forest 1-ha plot under the canopy crane. In addition, we report for the canopy crane plot new demography and basal areas for smaller size shrubs and treelets subsampled from nine 20 m quadrats, and liana basal area and abundance from the whole plot. The DRO site has an estimated total vascular plant species richness of 441 species, of which 172 species (39%) are endemic to Australia, and 4 species are endemics to the Daintree region. The 2 x 1-ha plots contains a total of 262 vascular plant species of which 116 (1531 individuals) are tree species ≥ 10 cm dbh. We estimate a stem basal area of 34.9 m ha, of which small stems (tree saplings and shrubs <10cm dbh) and lianas collectively contribute c.4.2%. Comparing the stem density-diversity patterns of the DRO forest with other tropical rainforests globally, our meta-analysis shows that DRO forests has a comparatively high stem density and moderate species diversity, due to the influence of cyclones. These data will provide an important foundation for ecological and conservation studies in lowland tropical forest.
New information: We present a floristic checklist, a life form breakdown, and demography data from two 1-ha rainforest plots from a lowland tropical rainforest study site. We also present a meta-analysis of stem densities and species diversity from comparable-sized plots across the tropics
Mapping the integrative field: taking stock of socio-technical collaborations
Responsible innovation requires that scientific and other expert practices be responsive to society. We take stock of a variety of collaborative approaches to socio-technical integration that seek to broaden the societal contexts technical experts take into account during their routine activities. Part of a larger family of engaged scholarship that includes inter- and trans-disciplinarity as well as stakeholder and public engagement, we distinguish collaborative socio-technical integration in terms of its proximity to and transformation of expert practices. We survey a variety of approaches that differ widely in terms of their integrative methods, conceptions of societal context, roles, and aspirations for intervention. Taking a handful of “communities of integration” as exemplars, we then provide a framework for comparing the forms, means, and ends of collaborative integration. We conclude by reflecting on some of the main features of, and tensions within, this developing arena of practical inquiry and engagement and what this suggests for integrative efforts aimed at responsible innovation
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