Stellar Phoenix Windows Data Recovery Pro V9.0.5.1 Crack
Shanae Maerz
During the sessions, you can choose from a selection of 175 talks. The oral presentations are divided into 11 Plenary Talks sessions and 14 Parallel Talks sessions spread across three rooms:
Additionally, there are over 500 posters to view in the 4 poster rounds.
If multiple presentations are scheduled in 1 session round, there will be no room change; participants are expected to attend all presentations in that session.
One of the most fundamental results in the study of exoplanets has been the finding that small planets are extremely abundant in the Universe and that they are bifurcated into seemingly two separate population: rocky super-Earths and gas-rich sub-Neptunes. Strikingly, recent studies have suggested the existence of a long-hypothesized new category of planets, referred to as water worlds, representing larger and warmer planetary versions of the volatile-rich icy moons in the Outer Solar System. In this talk, we will present the highlights from our 82-hour JWST/NIRSPEC+NIRISS survey probing the transmission spectra of five water-world candidates in unprecedented detail. We discuss the main findings regarding the prevalence and diversity of volatile-rich water worlds, based on molecular detections on at least three planets in our survey. We put particular emphasis on the temperate planet TOI-270d for which we detect, for the first time, a high-metallicity atmosphere rich in carbon, oxygen, and sulfur.
The demographics of exoplanets are a key lever we have to understand how they form and evolve. However, because hot Jupiters are intrinsically rare, our knowledge of their statistics has been limited by small number found by any individual survey, and the heterogeneity of the overall sample. Over the past two years, we have been conducting an extensive observational campaign to assemble a magnitude-limited sample of transiting hot Jupiters unified by the all-sky transit search of TESS. We observed >200 candidates and confirmed >80 new planets, and combined this with previously known objects to create a homogeneous sample of 400 hot Jupiters. I will present the first demographic results to emerge from this survey, including the >4-sigma detection of the "three-day" pile-up in the period distribution, the dependence of their occurrence rate on host star metallicity and mass, and comparisons with smaller and longer-period planets.
Recent improvements in instrumentation and computational methods have unlocked a wealth of information in high spectral resolution (R > 15,000) data of transiting exoplanets. Current data of hot- and ultra-hot Jupiters is of high enough quality that three-dimensional effects, such as from thermochemical gradients and winds, can manifest in the data. However, 1D retrieval frameworks have struggled to keep pace. Here, we present ARDA - Atmospheric Retrieval via Disk Averaging - a 3D atmospheric modeling and retrieval code accelerated by GPUs to be fast enough for high spectral resolution retrievals. ARDA can map analytic global pressure-temperature and velocity fields, calculate vertical gas abundances, and perform radiative transfer extremely fast, allowing the estimation of longitudinal thermal structure and wind speeds from high resolution spectroscopic phase curves. We also present preliminary results applying ARDA to combined data sets from Gemini South/IGRINS and JWST/NIRISS of the ultra-hot Jupiter WASP-18b.
The near-infrared spectropolarimeter SPIRou located at the Canada-France-Hawaii Telescope is one of the best for atmospheric characterisation of exoplanets from the ground, due to its properties and location. It observed WASP-76b following a reported and confirmed asymmetry in the limbs of its atmosphere, detected through observations in the visible (Ehrenreich et al. 2020). This led to extensive theoretical and observational work around this planet to understand its peculiarity. In acquiring infrared data of this atmosphere, different species and pressure layers are expected to be probed, which could reveal different temperature and dynamical profiles of the atmosphere. I will detail my study of the characterisation of the atmosphere of WASP-76b using SPIRou data and how it led to the detection of H2O and CO. Such detections open a new window into the understanding of the dynamics, physics and chemistry of WASP-76b, and new insight on ultra-hot planetary atmospheres.
Combining high resolution spectroscopy to high contrast imaging is a very powerful approach to detect and characterize very faint exoplanets, expecially using large telescopes and long integration times for the most interesting cases. Some interesting data have been obtained in a diversity of observing cases and instruments such as ERIS or HiRISE (SPHERE-CRIRES) from the ground or from JWST. The obtained results can be quantitatively compared to the predictible level of signal in such observing modes, and the corresponding level of noise set by fundamental limitations. We draw some lessons learnt from this comparison, on the instrumental side, concerning the level of non-ideal effects inducing residual systematics effects. We also discuss on the astronomical point of view, the similarity or mismatch between the actually observed companion spectra with respect to the models. Such lessons learnt are important for the preparation of future instruments, in particular ELT, and observation programs.
JWST allows for the first time to observe atmospheres of rocky exoplanets including the well-studied Hot Super Earth 55 Cnc e. If cloud formation takes place, this could affect gas composition on the planet, dim spectral features or change the temperature structure in its atmospheres. Observation of silicate clouds could also point to the presence of a magma ocean. Hence, it is important to understand cloud formation on magma planets, to interpret spectroscopic information accurately.To investigate this, we have run a grid of models for atmospheres of magma planets by coupling the outgassing with equilibrium chemistry taking into account condensation. We then iterate the results with radiative transfer for self-consistent TP-structures. In this talk I will present the results of our grid calculation focusing on the type of condensable species in these worlds, the conditions for them to form and their effect on the atmosphere.
Atmospheric escape can have crucial consequences for the evolution of exoplanets, and is thought to sculpt the hot Neptune desert and radius valley. The Lyman-α, metastable helium and several UV metal lines have presented evidence of escape for individual planets. Growing this sample of spectral lines that are used, as well as combining observations of multiple lines, will help us understand atmospheric escape in much greater detail. To this end, we make synthetic transit spectra and discover new spectral lines that should serve as good tracers of atmospheric escape, but have never been observed yet. We predict various lines with transit depths of up to tens of percent, which is stronger than some of the currently used tracers. Our model is open-source and available to the community, and can also be used to infer important outflow characteristics such as the mass-loss rate from observations.
The Solar system stands out from most known planetary systems. Detecting Jupiter-like planets helps unravel the uniqueness of the Solar system and sheds light on the formation of other planetary systems.
We present the discovery of a cold Jupiter in a system alongside a hot Jupiter. We investigate how changes in observation strategy can influence the ease with which such planets can be detected. By varying cadence and measurement precision, we estimate the additional data required to detect hypothetical cold Jupiters.
These systems are intriguing. Hot Jupiters are thought to form far away and migrate inward. Cold Jupiters can end in a distant and eccentric orbit, which could be the result of the influence of a third body that was ejected. To test this hypothesis, it is critical to search for additional planets in those systems. Our work will inform the best observation strategy to perform that search.
Evolution models of planetary systems find that resonant chains of planets often arise from the formation within protoplanetary disks. However, the occurrence of observed resonant chains, such as the notable TRAPPIST-1 system, is relatively low. This suggests that the majority of these chains become destabilized after the dissipation of the protoplanetary disk. Stellar tides, especially the wavelike dynamical tide, could be proposed as potential contributors to the destabilization of resonant chains. The dissipation of the dynamical tide, because of the frequency-dependant tidal excitation of stellar oscillation eigenmodes, potentially leads to a boost in migration for the close-in planets and disrupts the fragile stability of resonant chains. Thus, we investigate the influence of the stellar dynamical tide on multi-planet systems with taking their dissipation into account in the N-body code Posidonius. Notably, this research represents the first exploration of the impact of frequency-dependent dynamical tides on multi-planet systems.
We explore interior models for Super-Earths and Sub Neptunes to better understand the diversity of their interiors and atmospheres. The majority of current interior models suffer from simplified assumptions of chemically inert interiors and the neglect of volatile-exchange at the rock-atmosphere interface. In our work, the presence of magma oceans and their chemical and compositional coupling with the atmosphere are of prime interest. We quantify their effects on mass-radius relationships and the consequences of using different interior models for the interpretation of bulk water and bulk H/He content. Our results show that estimates can vary by more than one order of magnitude. Our new interior models are essential tools for the interpretation of data, e.g., from Kepler, TESS, CHEOPS (and RV-follow-ups), but also JWST.
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