109 research outputs found
The Signature of Primordial Grain Growth in the Polarized Light of the AU Mic Debris Disk
We have used the Hubble Space Telescope/ACS coronagraph to make polarization
maps of the AU Mic debris disk. The fractional linear polarization rises
monotonically from about 0.05 to 0.4 between 20 and 80 AU. The polarization is
perpendicular to the disk, indicating that the scattered light originates from
micron sized grains in an optically thin disk. Disk models, which
simultaneously fit the surface brightness and polarization, show that the inner
disk (< 40-50 AU) is depleted of micron-sized dust by a factor of more than
300, which means that the disk is collision dominated. The grains have high
maximum linear polarization and strong forward scattering. Spherical grains
composed of conventional materials cannot reproduce these optical properties. A
Mie/Maxwell-Garnett analysis implicates highly porous (91-94%) particles. In
the inner Solar System, porous particles form in cometary dust, where the
sublimation of ices leaves a "bird's nest" of refractory organic and silicate
material. In AU Mic, the grain porosity may be primordial, because the dust
"birth ring" lies beyond the ice sublimation point. The observed porosities
span the range of values implied by laboratory studies of particle coagulation
by ballistic cluster-cluster aggregation. To avoid compactification, the upper
size limit for the parent bodies is in the decimeter range, in agreement with
theoretical predictions based on collisional lifetime arguments. Consequently,
AU Mic may exhibit the signature of the primordial agglomeration process
whereby interstellar grains first assembled to form macroscopic objects.Comment: 12 pages, 8 figures, ApJ, in pres
Searching for sub-stellar companion into the LkCa15 proto-planetary disk
Recent sub-millimetric observations at the Plateau de Bure interferometer
evidenced a cavity at ~ 46 AU in radius into the proto-planetary disk around
the T Tauri star LkCa15 (V1079 Tau), located in the Taurus molecular cloud.
Additional Spitzer observations have corroborated this result possibly
explained by the presence of a massive (>= 5 MJup) planetary mass, a brown
dwarf or a low mass star companion at about 30 AU from the star. We used the
most recent developments of high angular resolution and high contrast imaging
to search directly for the existence of this putative companion, and to bring
new constraints on its physical and orbital properties. The NACO adaptive
optics instrument at VLT was used to observe LkCa15 using a four quadrant phase
mask coronagraph to access small angular separations at relatively high
contrast. A reference star at the same parallactic angle was carefully observed
to optimize the quasi-static speckles subtraction (limiting our sensitivity at
less than 1.0). Although we do not report any positive detection of a faint
companion that would be responsible for the observed gap in LkCa15's disk
(25-30 AU), our detection limits start constraining its probable mass,
semi-major axis and eccentricity. Using evolutionary model predictions, Monte
Carlo simulations exclude the presence of low eccentric companions with masses
M >= 6 M Jup and orbiting at a >= 100 AU with significant level of confidence.
For closer orbits, brown dwarf companions can be rejected with a detection
probability of 90% down to 80 AU (at 80% down to 60 AU). Our detection limits
do not access the star environment close enough to fully exclude the presence
of a brown dwarf or a massive planet within the disk inner activity (i.e at
less than 30 AU). Only, further and higher contrast observations should unveil
the existence of this putative companion inside the LkCa15 disk.Comment: 6 pages, 4 figures, accepted for publication in A&
Orbital characterization of the \beta Pictoris b giant planet
In June 2010, we confirmed the existence of a giant planet in the disk of the
young star Beta Pictoris, located between 8 AU and 15 AU from the star. This
young planet offers the rare opportunity to monitor a large fraction of the
orbit using the imaging technique over a reasonably short timescale. Using the
NAOS-CONICA adaptive-optics instrument (NACO) at the Very Large Telescope
(VLT), we obtained repeated follow-up images of the Bpic system in the Ks and
L' filters at four new epochs in 2010 and 2011. Complementing these data with
previous measurements, we conduct a homogeneous analysis, which covers more
than eight yrs, to accurately monitor the Bpic b position relative to the star.
On the basis of the evolution of the planet's relative position with time, we
derive the best-fit orbital solutions for our measurements. More reliable
results are found with a Markov-chain Monte Carlo approach. The solutions favor
a low-eccentricity orbit e < 0.17, with semi-major axis in the range 8--9 AU
corresponding to orbital periods of 17--21 yrs. Our solutions favor a highly
inclined solution with a peak around i=88.5+-1.7 deg, and a longitude of
ascending node tightly constrained at Omega = -147.5+-1.5 deg. These results
indicate that the orbital plane of the planet is likely to be above the
midplane of the main disk, and compatible with the warp component of the disk
being tilted between 3.5 deg and 4.0 deg. This suggests that the planet plays a
key role in the origin of the inner warped-disk morphology of the Bpic disk.
Finally, these orbital parameters are consistent with the hypothesis that the
planet is responsible for the transit-like event observed in November 1981, and
also linked to the cometary activity observed in the Bpic system.Comment: 10 pages, 12 figures, accepted to A&
ANYCaRE: a role-playing game to investigate crisis decision-making and communication challenges in weather-related hazards
This study proposes a role-playing experiment to explore the value of modern
impact-based weather forecasts on the decision-making process to (i) issue
warnings and manage the official emergency response under uncertainty and
(ii) communicate and trigger protective action at different levels of the
warning system across Europe. Here, flood or strong-wind game simulations
seek to represent the players' realistic uncertainties and dilemmas
embedded in the real-time forecasting-warning processes. The game was first
tested in two scientific workshops in Finland and France, where European
researchers, developers, forecasters and civil protection representatives
played the simulations. Two other game sessions were organized afterwards
(i) with undergraduate university students in France and (ii) with Finnish
stakeholders involved in the management of hazardous weather emergencies.
First results indicate that multi-model developments and crowdsourcing tools
increase the level of confidence in the decision-making under pressure. We
found that the role-playing approach facilitates interdisciplinary
cooperation and argumentation on emergency response in a fun and interactive
manner. The ANYCaRE experiment was proposed, therefore, as a valuable learning
tool to enhance participants' understanding of the complexities and
challenges met by various actors in weather-related emergency management.</p
Exoplanet Characterization and the Search for Life
Over 300 extrasolar planets (exoplanets) have been detected orbiting nearby
stars. We now hope to conduct a census of all planets around nearby stars and
to characterize their atmospheres and surfaces with spectroscopy. Rocky planets
within their star's habitable zones have the highest priority, as these have
the potential to harbor life. Our science goal is to find and characterize all
nearby exoplanets; this requires that we measure the mass, orbit, and
spectroscopic signature of each one at visible and infrared wavelengths. The
techniques for doing this are at hand today. Within the decade we could answer
long-standing questions about the evolution and nature of other planetary
systems, and we could search for clues as to whether life exists elsewhere in
our galactic neighborhood.Comment: 7 pages, 2 figures, submitted to Astro2010 Decadal Revie
The EMBRACE web service collection
The EMBRACE (European Model for Bioinformatics Research and Community Education) web service collection is the culmination of a 5-year project that set out to investigate issues involved in developing and deploying web services for use in the life sciences. The project concluded that in order for web services to achieve widespread adoption, standards must be defined for the choice of web service technology, for semantically annotating both service function and the data exchanged, and a mechanism for discovering services must be provided. Building on this, the project developed: EDAM, an ontology for describing life science web services; BioXSD, a schema for exchanging data between services; and a centralized registry (http://www.embraceregistry.net) that collects together around 1000 services developed by the consortium partners. This article presents the current status of the collection and its associated recommendations and standards definitions
The Kuiper Belt and Other Debris Disks
We discuss the current knowledge of the Solar system, focusing on bodies in
the outer regions, on the information they provide concerning Solar system
formation, and on the possible relationships that may exist between our system
and the debris disks of other stars. Beyond the domains of the Terrestrial and
giant planets, the comets in the Kuiper belt and the Oort cloud preserve some
of our most pristine materials. The Kuiper belt, in particular, is a
collisional dust source and a scientific bridge to the dusty "debris disks"
observed around many nearby main-sequence stars. Study of the Solar system
provides a level of detail that we cannot discern in the distant disks while
observations of the disks may help to set the Solar system in proper context.Comment: 50 pages, 25 Figures. To appear in conference proceedings book
"Astrophysics in the Next Decade
A near-infrared interferometric survey of debris disc stars. II. CHARA/FLUOR observations of six early-type dwarfs
High-precision interferometric observations of six early-type main sequence
stars known to harbour cold debris discs have been obtained in the
near-infrared K band with the FLUOR instrument at the CHARA Array. The measured
squared visibilities are compared to the expected visibility of the stellar
photospheres based on theoretical photospheric models taking into account
rotational distortion, searching for potential visibility reduction at short
baselines due to circumstellar emission. Our observations bring to light the
presence of resolved circumstellar emission around one of the six target stars
(zeta Aql) at the 5 sigma level. The morphology of the emission source cannot
be directly constrained because of the sparse spatial frequency sampling of our
interferometric data. Using complementary adaptive optics observations and
radial velocity measurements, we find that the presence of a low-mass companion
is a likely origin for the excess emission. The potential companion has a
K-band contrast of four magnitudes, a most probable mass of about 0.6 Msun, and
is expected to orbit between about 5.5 AU and 8 AU from its host star assuming
a purely circular orbit. Nevertheless, by adjusting a physical debris disc
model to the observed Spectral Energy Distribution of the zeta Aql system, we
also show that the presence of hot dust within 10 AU from zeta Aql, producing a
total thermal emission equal to 1.69 +- 0.31% of the photospheric flux in the K
band, is another viable explanation for the observed near-infrared excess. Our
re-interpretation of archival near- to far-infrared photometric measurements
shows however that cold dust is not present around zeta Aql at the sensitivity
limit of the IRS and MIPS instruments onboard Spitzer, and urges us to remove
zeta Aql from the category of bona fide debris disc stars.Comment: 14 pages, accepted for publication in A&
Circumstellar disks and planets. Science cases for next-generation optical/infrared long-baseline interferometers
We present a review of the interplay between the evolution of circumstellar
disks and the formation of planets, both from the perspective of theoretical
models and dedicated observations. Based on this, we identify and discuss
fundamental questions concerning the formation and evolution of circumstellar
disks and planets which can be addressed in the near future with optical and
infrared long-baseline interferometers. Furthermore, the importance of
complementary observations with long-baseline (sub)millimeter interferometers
and high-sensitivity infrared observatories is outlined.Comment: 83 pages; Accepted for publication in "Astronomy and Astrophysics
Review"; The final publication is available at http://www.springerlink.co
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