1,305 research outputs found
Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to beta Pictoris b and SPHERE observations
We aim to interpret future photometric and spectral measurements from these
instruments, in terms of physical parameters of the planets, with an
atmospheric model using a minimal number of assumptions and parameters.
We developed Exoplanet Radiative-convective Equilibrium Model (Exo-REM) to
analyze the photometric and spectro- scopic data of directly imaged planets.
The input parameters are a planet's surface gravity (g), effective temperature
(Teff ), and elemental composition. The model predicts the equilibrium
temperature profile and mixing ratio profiles of the most important gases.
Opacity sources include the H2-He collision-induced absorption and molecular
lines from eight compounds (including CH4 updated with the Exomol line list).
Absorption by iron and silicate cloud particles is added above the expected
condensation levels with a fixed scale height and a given optical depth at some
reference wavelength. Scattering was not included at this stage.
We applied Exo-REM to photometric and spectral observations of the planet
beta Pictoris b obtained in a series of near-IR filters. We derived Teff = 1550
+- 150 K, log(g) = 3.5 +- 1, and radius R = 1.76 +- 0.24 RJup (2-{\sigma} error
bars from photometric measurements). These values are comparable to those found
in the literature, although with more conservative error bars, consistent with
the model accuracy. We were able to reproduce, within error bars, the J- and
H-band spectra of beta Pictoris b. We finally investigated the precision to
which the above parameterComment: 15 pages, 14 figures, accepted by A&
Evaluation de la méthode SAS sur un rotor de compresseur haute-pression
International audienceThe main design objectives of a high pressure compressor are the aerodynamic efficiency and the operating range (e.g. the surge margin). Those quantities are impacted by secondary and leakage flows occurring in the blade passage such as corner separation or stall and tip leakage flows. The turbulence modeling influences strongly the prediction of the overall performances. The aims of the present study were (i) the validation of the combination of the SAS approach with the DRSM turbulence model by comparison to experimental data, especially to laser measurements in the tip of a rotor of a high pressure compressor and (ii) the discussion of the flow prediction improvements with respect to turbulence approaches classically used in CFD and industry: URANS simulations and standard SAS simulation i.e. combined with SST turbulence model. The SAS results are compared to experimental data and to URANS results (SST and DRSM). Only the simulations with IGV wakes predict the velocity fluctuations near tip gap, from the leading edge. Concerning the time-averaged performances, the stagnation pressure losses are slightly overestimated by SAS, especially with DRSM model. This is due to an amplification of the hub corner separation. Moreover, the isentropic efficiency is very sensitive to the SAS approach and to the turbulence model. The spectral analysis shows that the prediction of the amplitude and frequencies of the power spectral density of static pressure is improved using the SAS approach instead of URANS one. The SAS approach leads to PSD similar to ZDES, especially with the DRSM model. Thus, the SAS-DRSM is able to well predict the tip leakage flow with the fine mesh. Nevertheless, this approach amplifies the hub corner separation leading to a strong underestimation of overall performances
Titan's atmosphere as observed by Cassini/VIMS solar occultations: CH, CO and evidence for CH absorption
We present an analysis of the VIMS solar occultations dataset, which allows
us to extract vertically resolved information on the characteristics of Titan's
atmosphere between 100-700 km with a characteristic vertical resolution of 10
km. After a series of data treatment procedures, 4 occultations out of 10 are
retained. This sample covers different seasons and latitudes of Titan. The
transmittances show clearly the evolution of the haze and detect the detached
layer at 310 km in Sept. 2011 at mid-northern latitudes. Through the inversion
of the transmission spectra with a line-by-line radiative transfer code we
retrieve the vertical distribution of CH and CO mixing ratio. The two
methane bands at 1.4 and 1.7 {\mu}m are always in good agreement and yield an
average stratospheric abundance of %. This is significantly less
than the value of 1.48% obtained by the GCMS/Huygens instrument. The analysis
of the residual spectra after the inversion shows that there are additional
absorptions which affect a great part of the VIMS wavelength range. We
attribute many of these additional bands to gaseous ethane, whose near-infrared
spectrum is not well modeled yet. Ethane contributes significantly to the
strong absorption between 3.2-3.5 {\mu}m that was previously attributed only to
C-H stretching bands from aerosols. Ethane bands may affect the surface windows
too, especially at 2.7 {\mu}m. Other residual bands are generated by stretching
modes of C-H, C-C and C-N bonds. In addition to the C-H stretch from aliphatic
hydrocarbons at 3.4 {\mu}m, we detect a strong and narrow absorption at 3.28
{\mu}m which we tentatively attribute to the presence of PAHs in the
stratosphere. C-C and C-N stretching bands are possibly present between 4.3-4.5
{\mu}m. Finally, we obtain the CO mixing ratio between 70-170 km. The average
result of ppm is in good agreement with previous studies.Comment: 51 pages, 28 figure
Aerodynamic design of a Martian micro air vehicle
International audienceThis paper presents a numerical and experimental study of the aerodynamic characteristics of a vertical takeoff and landing (VTOL) micro air vehicle (MAV) designed to fly in Mars' atmosphere. Numerical tools are validated through experimental data from the literature where Martian conditions are replicated. Innovative airfoils are designed for the specific flying conditions of the Martian MAV, i.e. compressible and ultra-low Reynolds number flows. An optimized airfoil is evaluated in different Reynolds and Mach number conditions using unsteady laminar Navier-Stokes simulations. Rotors are designed by optimizing the chord and twist distributions using a free wake lifting line method with different geometrical and lift constraints. Rotors are numerically evaluated using two different Navier-Stokes solvers. A coaxial configuration is also defined to achieve zero total torque and double lift. To validate the simulations, experiments are performed in the ONERA's low pressure tank, recreating Martian atmosphere in terms of density and gas. Thrust and torque are measured by a two-component setup developed by ISAE-SUPAERO, with independent measures on each rotor in coaxial configuration. Tests are performed up to transonic flow conditions at blade tip
Simulated performance of the molecular mapping for young giant exoplanets with the Medium Resolution Spectrometer of JWST/MIRI
Young giant planets are the best targets for characterization with direct
imaging. The Medium Resolution Spectrometer (MRS) of the Mid-Infrared
Instrument (MIRI) of the recently launched James Webb Space Telescope (JWST)
will give access to the first spectroscopic data for direct imaging above 5
m with unprecedented sensitivity at a spectral resolution up to 3700. This
will provide a valuable complement to near-infrared data from ground-based
instruments for characterizing these objects. We aim to evaluate the
performance of MIRI/MRS to detect molecules in the atmosphere of exoplanets and
to constrain atmospheric parameters using Exo-REM atmospheric models. The
molecular mapping technique, based on cross-correlation with synthetic models,
has been introduced recently. This promising detection and characterization
method is tested on simulated MIRI/MRS data. Directly imaged planets can be
detected with MIRI/MRS, and we are able to detect molecules (HO, CO,
NH, CH, HCN, PH, CO) at various angular separation depending on
the strength of the molecular features and brightness of the target. We find
that the stellar spectral type has a weak impact on the detection level. This
method is globally most efficient for planets with temperatures below 1500 K,
for bright targets and angular separation greater than 1. Our parametric
study allows us to anticipate the ability to characterize planets that would be
detected in the future. The MIRI/MRS will give access to molecular species not
yet detected in exoplanetary atmospheres. The detection of molecules as
indicators of the temperature of the planets will make it possible to
discriminate between the various hypotheses of the preceding studies, and the
derived molecular abundance ratios should bring new constraints on planetary
formation scenarios.Comment: 25 pages, 13 figure
Upper limits for undetected trace species in the stratosphere of Titan
In this paper we describe a first quantitative search for several molecules
in Titan's stratosphere in Cassini CIRS infrared spectra. These are: ammonia
(NH3), methanol (CH3OH), formaldehyde (H2CO), and acetonitrile (CH3CN), all of
which are predicted by photochemical models but only the last of which
observed, and not in the infrared. We find non-detections in all cases, but
derive upper limits on the abundances from low-noise observations at 25{\deg}S
and 75{\deg}N. Comparing these constraints to model predictions, we conclude
that CIRS is highly unlikely to see NH3 or CH3OH emissions. However, CH3CN and
H2CO are closer to CIRS detectability, and we suggest ways in which the
sensitivity threshold may be lowered towards this goal.Comment: 11 pages plus 6 figure file
New laboratory measurements of CH4 in Titan's conditions and a reanalysis of the DISR near-surface spectra at the Huygens landing site
International audienceLaboratory spectra of methane-nitrogen mixtures have been recorded in the near-infrared range (1.0 - 1.65 µm) in conditions similar to Titan's near surface, to facilitate the interpretation of the DISR/DLIS spectra taken during the last phase of the descent of the Huygens Probe, when the surface was illuminated by a surface science lamp. We used a 0.03 cm-1 spectral resolution, adequate to resolve the lines at high pressure (pN2 ~ 1.5 bar). By comparing the laboratory spectra with synthetic calculations in the well-studied ν2 + 2ν3 band (7515-7620 cm-1), we determine a methane absorption column density of 178±20 cm-am and a temperature of 118±10 K in our experiment. From this, we derive the methane absorption coefficients over 1.0-1.65 µm with a 0.03 cm-1 sampling, allowing for the extrapolation of the results to any other methane column density under the relevant pressure and temperature conditions. We then revisit the calibration and analysis of the Titan "lamp-on" DLIS spectra. We infer a 5.1±0.8 % methane mixing ratio in the first 25 m of Titan's atmosphere. The CH4 mixing ratio measured 90 sec after landing from a distance of 45 cm is found to be 0.92±0.25 times this value, thus showing no post-landing outgassing of methane in excess of ̴ 20 %. Finally, we determine the surface reflectivity as seen from 25 m and 45 cm and find that the 1500 nm absorption band is deeper in the post-landing spectrum as compared to pre-landing
A Time-Dependent Radiative Model of HD209458b
We present a time-dependent radiative model of the atmosphere of HD209458b
and investigate its thermal structure and chemical composition. In a first
step, the stellar heating profile and radiative timescales were calculated
under planet-averaged insolation conditions. We find that 99.99% of the
incoming stellar flux has been absorbed before reaching the 7 bar level.
Stellar photons cannot therefore penetrate deeply enough to explain the large
radius of the planet. We derive a radiative time constant which increases with
depth and reaches about 8 hr at 0.1 bar and 2.3 days at 1 bar. Time-dependent
temperature profiles were also calculated, in the limit of a zonal wind that is
independent on height (i.e. solid-body rotation) and constant absorption
coefficients. We predict day-night variations of the effective temperature of
\~600 K, for an equatorial rotation rate of 1 km/s, in good agreement with the
predictions by Showman &Guillot (2002). This rotation rate yields day-to-night
temperature variations in excess of 600 K above the 0.1-bar level. These
variations rapidly decrease with depth below the 1-bar level and become
negligible below the ~5--bar level for rotation rates of at least 0.5 km/s. At
high altitudes (mbar pressures or less), the night temperatures are low enough
to allow sodium to condense into Na2S. Synthetic transit spectra of the visible
Na doublet show a much weaker sodium absorption on the morning limb than on the
evening limb. The calculated dimming of the sodium feature during planetary
transites agrees with the value reported by Charbonneau et al. (2002).Comment: 9 pages, 8 figures, replaced with the revised versio
Preparation for the Solar system observations with Herschel: Simulation of Jupiter observations with PACS
Observations of the water inventory as well as other chemically important
species on Jupiter will be performed in the frame of the guaranteed time key
project of the Herschel Space Observatory entitled "Water and related chemistry
in the Solar system". Among other onboard instruments, PACS (Photodetector
Array Camera and Spectrometer) will provide new data of the spectral atlas in a
wide region covering the far-infrared and submillimetre domains, with an
improved spectral resolution and a higher sensitivity compared to previous
observations carried out by Cassini/CIRS (Composite InfraRed Spectrometer) and
by ISO (Infrared Space Observatory). In order to optimise the observational
plan and to prepare for the data analysis, we have simulated the expected
spectra of PACS Jupiter observations. Our simulation shows that PACS will
promisingly detect several H2O emission lines. As PACS is capable of spatially
resolving the Jovian disk, we will be able to discern the external oxygen
sources in the giant planets by exploring the horizontal distribution of water.
In addition to H2O lines, some absorption lines due to tropospheric CH4, HD,
PH3 and NH3 lines will be observed with PACS. Furthermore, owing to the high
sensitivity of the instrument, the current upper limit on the abundance of
hydrogen halides such as HCl will be also improved.Comment: to be published in Planetary and Space Scienc
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