Mardi 15 janvier 2019 à 11h00 (ATTENTION : changement de salle : bâtiment 14)
Victor Marchiori (LESIA)
ESA’s PLATO space mission is devoted to unveiling and characterizing new extrasolar planets and their host stars. It will encompass a very large (>2200 deg2) field-of-view, granting it the potential to survey up to one million stars depending on the final observation strategy. Spacecraft telemetry budget cannot handle transmitting individual images for such a huge stellar sample, so the development of an appropriate strategy to perform on-board data reduction is mandatory. We employ mask-based (aperture) photometry to produce stellar lightcurves in-flight. Our aim is thus to find the mask model that optimizes the scientific performance of the reduced data. Three distinct aperture structures are considered. First, we set up a weighted mask delivering global minimum noise-to-signal ratio, computed through a novel fast convergence algorithm. A second weighted mask is built following a Gaussian function. Lastly, we define a mask containing exclusively binary weights. Each strategy is tested on synthetic imagettes generated for 50,000 potential PLATO targets. Stellar population is extracted from Gaia DR2 catalogue. A pioneer criteria is adopted for choosing the optimal solution (structure) : the one providing the best compromise between sensibility to detect true and capability to reject false planet transits, determined based on noise-to-signal ratio and frequency of threshold crossing events. Our results show that, although binary mask statistically presents a few percent higher noise-to-signal ratio compared to weighted masks, all three strategies have nearly the same efficiency in detecting legit planet transits. When it comes to avoid spurious signals from contaminant stars though, binary mask statistically collects significantly less contaminant flux than weighted masks, making the former to be 30% less likely to deliver false transit signatures at 7.1sigma detection threshold. In planet transit finding context thus, choosing apertures based exclusively on how well a transit-like signal can be detected may not be the optimal approach.
Mardi 15 janvier 2019 à 11h00 (Salle de rĂ©union du bâtiment Jean-Louis Steinberg (bât. 16))
K. Sasikumar Raja (LESIA)
Various types of remote sensing observations have been used so far to probe the weakly compressible density turbulence in the extended solar corona and solar wind. Using the angular broadening observations of radio celestial point like sources, we have studied various turbulent parameters in the solar wind : anisotropic broadening, amplitude of density turbulence, density fluctuations, proton heating rate and the dissipation scales. For this study, we used the observations of Gauribidanur radioheliograph, Very Large Array and other historical observations carried out during 1952-2017. In this talk, I will discuss, the way these parameters vary with heliocentric distance and the solar cycle. The newly launched Parker Solar Probe and upcoming Solar Orbiter missions are going to play a crucial role in addressing these issues and other long standing mysteries of the solar wind.
Mercredi 9 janvier 2019 à 11h00 (Salle de confĂ©rence du bâtiment 17)
Sophie MUSSET (University of Minnesota, USA)
Solar X-rays provide the most direct diagnostics of energetic electron populations during solar flares. I will present recent results concerning particle acceleration and propagation in the solar corona from X-ray observations with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and extend the discussion to the need for new X-ray instrumentation using X-ray focusing optics. This instrumental concept was demonstrated with the FOXSI sounding rocket program and I will present results on X-ray diagnostics of microflares obtained with FOXSI observations.
Jeudi 20 dĂ©cembre 2018 à 16h00 (Salle de confĂ©rence du bâtiment 17)
Jean-Philippe Beaulieu (IAP)
The microlensing technique is a unique method to hunt for cold planets over a range of mass and separation, orbiting all varieties of host stars in the disk of our galaxy. It provides precise mass-ratio and projected separations in units of the Einstein ring radius. In order to obtain the physical parameters (mass, distance, orbital separation) of the system, it is necessary to combine the result of light curve modeling with lens mass-distance relations and/or perform a Bayesian analysis with a galactic model. A first mass-distance relation could be obtained from a constraint on the Einstein ring radius if the crossing time of the source over the caustic is measured. It could then be supplemented by secondary constraints such as parallax measurements, ideally by using coinciding ground and space-born observations. These are still subject to degeneracies, like the orbital motion of the lens. A third mass-distance relation can be obtained thanks to constraints on the lens luminosity using high angular resolution observations with 8 m class telescopes or the Hubble Space Telescope. The latter route, although quite inexpensive in telescope time is very effective. If we have to rely heavily on Bayesian analysis and limited constraints on mass-distance relations, the physical parameters are determined to 30–40% typically. In a handful of cases, ground-space parallax is a powerful route to get stronger constraint on masses. High angular resolution observations will be able to constrain the luminosity of the lenses in the majority of the cases, and in favorable circumstances it is possible to derive physical parameters to 10% or better. Moreover, these constraints will be obtained in most of the planets to be discovered by the Euclid and WFIRST satellites. We describe here the state-of-the-art approaches to measure lens masses and distances with an emphasis on high angular resolution observations. We will discuss the challenges, recent results and perspectives.
Mardi 11 dĂ©cembre 2018 à 11h00 (Salle de confĂ©rence du bâtiment 17)
Morgan Deal (LESIA)
Atomic diffusion, including the effect of radiative accelerations on individual elements, leads to variations of the chemical composition inside the stars as well as the surface abundances evolution. Indeed the accumulation in specific layers of the elements, which are the main contributors of the local opacity, modifies the internal stellar structure and surface abundances. Here we show that the variations of the chemical composition induced by atomic diffusion in G and F type stars can have significant impact on their structure, stellar parameters and seismic properties. We will also discuss the effect of the coupling between rotation and atomic diffusion for such stars. These processes need to be taken into account in stellar evolution models as the observations are more and more precise, especially in the context of the space missions TESS and PLATO.
Vendredi 30 novembre 2018 à 11h00 (Salle de confĂ©rence du bâtiment 17)
Benjamin Charnay (LESIA) et Boris Sauterey (IBENS, Institut de Biologie de l’Ecole Normale SupĂ©rieure)
La vie et l’atmosphère de la Terre primitive semblent avoir évolués de façon couplée. L’exemple le plus frappant est la Grande Oxygénation de l’atmosphère, provoquée par l’apparition de la photosynthèse oxygénique, qui a bouleversée la chimie atmosphérique et océanique, la minéralogie, l’évolution de la vie et potentiellement le climat avec le déclenchement des glaciations Huroniennes. Il a également été proposé qu’avant la Grande Oxygénation, l’atmosphère archéenne était riche en méthane issu d’organismes méthanogènes. Ce méthane aurait provoqué un effet de serre permettant de compenser la plus faible insolation à cette époque, et donc de maintenir un climat tempéré. Cependant, aucune modélisation globale et réaliste du système Terre incluant la biosphère primitive n’a été réalisée pour tester ces hypothèses.
Notre objectif est d’étudier les interactions entre les écosystèmes et l’environnement (atmosphère, océan et activité géologique) de la Terre primitive, ainsi que leur évolution. Pour cela, nous avons couplé un modèle climatique incluant la photochimie, à un modèle du cycle du carbone et un nouveau modèle réaliste et dynamique d’écosystème primitifs, qui inclut les différents métabolismes non photosynthétiques.
Durant cette présentation, nous décrirons le modèle climat-photochimique (le GCM Générique du LMD), le modèle du cycle du carbone et le modèle d’écosystème. Nous présenterons ensuite les résultats obtenus en couplant ces différents modèles, qui nous permettent de quantifier les teneurs en méthane durant l’Hadéen/Archéen et d’étudier les rétroactions climatiques causées par les écosystèmes de méthanogènes. Nous terminerons en discutant brièvement des différentes perspectives que nous offre ce modèle unique.
Lundi 26 novembre 2018 à 14h00 (Salle de confĂ©rence du bâtiment 17)
Arlette Noels (Université de Liège, STAR institute)
La Professeure Arlette Noels fera un cours d’Ă©volution stellaire avancĂ©e pour les Ă©toiles de faible masse sur la phase des gĂ©antes rouges. Cours en langue française.
Mardi 13 novembre 2018 à 11h00 (Salle de confĂ©rence du bâtiment 17)
Emilia Kilpua (University of Helsinki, Finlande)
Coronal mass ejections (CMEs) are key drivers of magnetospheric storms at Earth. Two key structures in CMEs are the turbulent sheath and the magnetic flux rope with smoother variations of solar wind plasma and magnetic field parameters. In this presentation I will discuss the status and challenges in predicting in advance (at least half-a-day) geoefficiency of flux ropes and sheath regions. The key focus will also be on observational and data-driven modelling efforts at the University of Helsinki space physics team to predict the magnetic field characteristics of flux ropes.
Mardi 6 novembre 2018 à 14h00 (Salle de confĂ©rence du bâtiment 17)
Anna Ciurlo (UCLA)
Au centre de la Voie lactée, l’environnement du trou noir supermassif (SMBH) présente un mélange complexe de jeunes étoiles, de gaz et de poussière. Le parsec central du Centre galactique a été observé à haut résolution avec le Keck pendant plus de 20 ans, le but principal étant de surveiller les étoiles en orbite autour du SMBH. Cependant, les caractéristiques du gaz situé au centre peuvent être examinées de près en utilisant cette base de données unique.
En particulier, les observations effectuĂ©es avec le spectromètre Ă intĂ©grale de champ OSIRIS au Keck nous permettent d’examiner les propriĂ©tĂ©s dynamiques du gaz et d’identifier un certain nombre d’objets aux propriĂ©tĂ©s inhabituelles. Certains d’entre eux ont de treĚ€s hautes vitesses radiales (200-800 km/s) et changent de vitesse, positon ou de forme au cours du temps. Parmi ces objets on observe plusieurs nouveaux objets de « type G » (Gillessen et al. 2012) ou objets stellaires poussiĂ©reux (dusty stellar objects DSO, Eckart et al. 2013).
Nous prĂ©sentons une Ă©tude de la morphologie et de la dynamique orbitale de ces objets compacts. Nous discutons des hypothèses pour leur formation et leur Ă©volution. Ces objets pourraient jouer un rĂ´le dans l’accrĂ©tion sur le SMBH. Initialement supposĂ©s ĂŞtre des nuages ​​de gaz compacts et poussiĂ©reux, les DSO sont probablement des objets stellaires entourĂ©s d’enveloppes gonflĂ©es de poussière et de gaz. Diverses hypothèses ont Ă©tĂ© proposĂ©es mais aucun consensus gĂ©nĂ©ral n’a encore Ă©tĂ© atteint sur leur nature. Jusqu’Ă prĂ©sent, deux de ces objets ont Ă©tĂ© identifiĂ©s et Ă©tudiĂ©s en dĂ©tail : G2 et G1. Nous dĂ©crivons ici les observations de trois autres DSO, y compris deux signalĂ©s pour la première fois, et utilisons cette population DSO pour contraindre leur nature intrinsèque.
Mardi 6 novembre 2018 à 14h00 (Salle de rĂ©union du bâtiment 14)
Vincent Prat (AIM, CEA)
Internal gravity waves provide us with a unique way to probe the stellar interior of intermediate-mass and massive stars. Those waves are also able to transport angular momentum. However, the propagation, the frequencies of waves and the transport they induce may be strongly affected by rotation and the presence of a magnetic field. For slow rotators, rotation can be taken into account using perturbative methods. For rapid rotators, which is the case of many early-type pulsators such as gamma Doradus, delta Scuti, SPB and Be stars, such methods fail, and the eigenvalue problem is fully 2D and computationally expensive. The traditional approximation of rotation, which neglects the horizontal component of the rotation vector, allows for efficient computation of modes. Another approach is to consider only small-wavelength waves and model them as propagating rays. Using these two complementary methods, I will discuss the impact of an axisymmetric magnetic field on gravito-inertial waves and the implications for the detection of deep magnetic fields.
