LESIA - Observatoire de Paris

Sauf exception, les séminaires ont lieu sur le site de Meudon, dans la salle de conférence du bâtiment 17.

Prochains séminaires

  • Jeudi 21 juin 2018 à 16h00 (Salle de conférence du bâtiment 17)

    Birth of high angular resolution : VLT and VLTI

    Pierre Léna (LESIA)

    The High Angular Resolution (HRA) at optical wavelengths was re-born during the 1970-1980s, and led to impressive developments : worldwide with adaptive optics and at Paranal with the VLTI. The seminar will recall the European emergence of these during these years, along with the conception of the VLT/VLTI. ESO became then the focus of an intense exploration of an almost entirely new domain of observational astronomy, leading to a considerable scientific and technical activity, which prepared for the impressive achievements of the next 25 years.


  • Lundi 25 juin 2018 à 11h00 (Salle de réunion du bâtiment 16)

    Magnetic Energy Buildup and Explosive Release

    Spiro K. Antiochos (NASA/GSFC, USA)

    It is now widely believed that solar eruptions such as CMEs, eruptive flares, and coronal hole jets are all due to the explosive release of magnetic free energy stored in the corona ; specifically, in the highly stressed magnetic field that supports filaments and prominences. An important observational finding in recent years is that the mechanisms underlying these eruptions may be invariant over many decades in energy release. We have proposed that the formation of the filament field and, consequently, the free energy buildup, is due to an inverse cascade of magnetic helicity injected into the corona by motions and flux emergence at the photosphere. We present our latest 3D MHD numerical simulations of the self-consistent energy buildup by helicity condensation and eventual explosive energy release. The calculations are in a realistic spherical domain that extends outward to 30 solar radii. We conclude from these simulations that the onset for the eruption, the trigger mechanism, is magnetic reconnection in the coronal field overlying the filament. Our results demonstrate that solar eruptions are an amazing example on cosmic scales of self-organization leading to catastrophic dynamics.


  • Lundi 9 juillet 2018 à 11h00 (Salle de conférence du bâtiment 17)

    First Science Results from the 2017 Eclipse Observation of the Airborne Infrared Spectrometer

    Jenna Samra (Harvard-Smithsonian Center for Astrophysics, USA)

    On August 21, 2017, the Airborne Infrared Spectrometer (AIR-Spec) observed the total solar eclipse at an altitude of 14.3 km from aboard the NSF/NCAR Gulfstream V research aircraft. The instrument successfully observed the five coronal emission lines that it was designed to measure : Si X (1.43µm), S XI (1.92µm), Fe IX (2.84µm), Mg VIII (3.03µm), and Si IX (3.94µm). Characterizing these magnetically sensitive emission lines is an important first step in designing future instruments to monitor the coronal magnetic field.

    During the eclipse observation, AIR-Spec measured the average linewidths, peak intensities, and center wavelengths of all five lines radially outward from the limb at four positions in the corona. One of the positions sampled a prominence, where a number of H I lines were also observed. The observation of Fe IX at 2.84µm was the first of that line. The radial intensity gradient of Si X was measured with high sensitivity, providing information on the dominant excitation processes for that line. The relative Doppler velocity of Si X was measured with a resolution of 5 km/sec, revealing variations across different coronal structures and an interesting case of bimodal velocities near the solar prominence.

    AIR-Spec is a slit spectrometer that measures light over a 1.55 Rsun field of view in four spectral passbands between 1.4 and 4 µm. The package includes an image stabilization system, feed telescope, grating spectrometer, and slit-jaw imager. Several follow-on experiments are being proposed to expand on the results from the 2017 eclipse, including a re-flight of AIR-Spec during the 2019 total eclipse, development of a new spectrometer or spectropolarimeter to observe the 2020 eclipse, and a laboratory study of infrared coronal emission lines.


  • Mercredi 18 juillet 2018 à 14h00 (Salle de conférence du bâtiment 17)

    Young LMC clusters : the role of red supergiants and multiple stellar populations in their integrated light and CMDs

    Randa Asa’d (New York University of Abu Dhabi, United Arab Emirates)

    The optical integrated spectra of three LMC young stellar clusters (NGC 1984, NGC 1994 and NGC 2011) exhibit concave continua and prominent molecular bands which deviate significantly from the predictions of single stellar population (SSP) models. In order to understand the appearance of these spectra, we create a set of young stellar population (MILES) models, which we make available to the community. We use archival International Ultraviolet Explorer integrated UV spectra to independently constrain the cluster masses and extinction, and rule out strong stochastic effects in the optical spectra. In addition, we also analyze deep colour-magnitude diagrams of the clusters to provide independent age determinations based on isochrone fitting. We explore hypotheses including age-spreads in the clusters, a top-heavy initial mass function, different SSP models and the role of red supergiant stars (RSG). We find that the strong molecular features in the optical spectra can only be reproduced by modeling an increased fraction of about ∼ 20 per cent by luminosity of RSG above what is predicted by canonical stellar evolution models. Given the uncertainties in stellar evolution at Myr ages, we cannot presently rule-out the presence of Myr age-spreads in these clusters. Our work combines different wavelengths as well as different approaches (resolved data as well as integrated spectra for the same sample) in order to reveal the complete picture. We show that each approach provides important information but in combination can we better understand the cluster stellar populations.


Séminaires passés

  • Jeudi 24 mai 2018 à 11h00 (Salle de réunion du bâtiment 17)

    Pièges à ions multichargés dans la couronne solaire

    Véronique Bommier (LESIA)

    Je voudrais vous présenter ce que l’on a pu obtenir au LESIA par la superposition de cartes de champ magnétique ou courant électrique photosphérique (données SDO/HMI, inversion UNNOFIT faite au LESIA), d’émissions UV coronales (données SDO/AIA), d’émissions X coronale aussi (données RHESSI). En particulier, il a été remarqué dans les colloques où ces superpositions étaient présentées, que les émissions UV se situent préférentiellement au-dessus des zones à courant électrique montant (Jz > 0), là où ces courants sont suffisamment forts, c’est-à-dire dans les rubans d’éruptions. Cette corrélation dissymétrique a donné à penser à plusieurs théoriciens et je présenterai, aussi bien que je peux, leurs propositions d’explications.

    En pratique, le séminaire sera fait de :

    • brève présentation des travaux de Miho Janvier
    • brève présentation de l’article de Sophie Musset
    • présentation de l’article de Haerendel, avec l’explication qu’il propose
    • présentation de l’article de Fleishman, avec explication, autant que possible, de ce qu’il propose

  • Jeudi 17 mai 2018 à 16h00 (Salle de conférence du bâtiment 17)

    Alpha and Omega of the PicSat mission

    Mathias Nowak (LESIA)

    As most of you probably already know, PicSat stopped emitting on March, 20, 2018. The satellite was successfully launched from India in January, carrying an ambitious "fibered photometer" to Low-Earth-Orbit. This 1.5 kg / 2 W instrument was supposed to help us explore the Beta Pictoris system, detect the potential transit of Beta Pic b, study the dust tail of transitting exocomets. A proposal had even been accepted to trigger the HARPS spectrograph on alerts coming from the small satellite ! Unfortunately, none of this will happen, as the mission abruptly came to an end two months ago.

    I will present a retrospective of the project, from the early development of the payload, to the final integration of the satellite here in Meudon, and its deliverie(s) in Delft (Netherlands). I will also talk about the 10 weeks of operations : what we did, what we did not do, which data ’we’ (understand : ’radio-amateurs around the world’) received from the satellite, etc. All of this will lead me to summarize what we have learned from this short-lived mission, and what we plan to do next.

    Be aware : there will be technical CubeSat jargon, sordid details about a failed delivery in Delft, ’amazing’ pictures of "Incredible India", and the very sad story of a post-mortem analysis of PicSat...


  • Mercredi 11 avril 2018 à 14h00 (Salle de conférence du bâtiment 17)

    Application of new inversion technique to the solar modelling problem and the determination of masses of red giants

    Gael Buldgen, University of Birmingham, HiROS group

    In the last decades, inversion techniques have been the most fruitful tools for the seismic analysis of the solar structure. They have allowed for the determination of the radial profile of thermodynamic quantities such as the density and the sound speed, thereby validating the so-called "standard" solar models, until the downward revision of the photospheric abundances of carbon, nitrogen and oxygen casted doubts on these models. This talk will show how inversion techniques of new quantities such as the entropy or the Ledoux discriminant can help provide new insights on the solar modelling problem and guide theoretical developments to its resolution.in addition to the solar problem, this seminar will discuss the application of mean density inversions to the radial oscillations of red giants. This part of the talk will show howmean density inversions can be used to determine more accurate values of this quantity than using the usual scaling laws, taking into account all the information of the radial oscillation spectrum.

    Les inversions sismiques ont été durant ces dernières décennies les approches les plus fructueuses pour l’analyse de la structure interne du soleil. Elles ont permis de déterminer les profils radiaux de grandeurs thermodynamiques telles que la vitesse du son et la densité, validant ainsi les modèles dits "standards" du soleil, jusqu’à ce que la révision de l’abondance photosphérique de carbone, azote et oxygène ne sème le doute sur les modèles théoriques. Ce talk présentera comment la combinaison de multiples inversions de nouveaux profils de grandeurs thermodynamiques telles que l’entropie et le discriminant de Ledoux permettent de jeter un regard neuf sur le problème de la métallicité solaire et peut guider les développements théoriques vers sa résolution. En plus de traiter du problème solaire, ce talk abordera également l’application des méthodes d’inversion sismiques aux modes radiaux des géantes rouges. Ce volet portera sur l’extension des inversions de densité moyenne à la branche des géantes, permettant une détermination plus exacte de cette grandeur qu’au moyen des lois d’échelles car tenant compte de toute l’information du spectre des oscillations radiales.


  • Jeudi 5 avril 2018 à 15h00 (Salle de réunion du bâtiment 16)

    A new look at the Sun with LOFAR : observations and implications

    Eduard Kontar (University of Glasgow, UK)


  • Jeudi 29 mars 2018 à 11h00 (Salle de conférence du bâtiment 17)

    PLATO (PLAnetary Tranists and Oscillations of stars) : statuts, concept instrumental et objectifs

    Martin Pertenaïs (Optical System Engineer of PLATO, DLR, Institute of Optical Sensor Systems)

    La mission spatiale de l’ESA PLATO – sélectionnée en 2014 par l’ESA dans le programme Cosmic Vision - progresse dans son développement qui l’amènera à un lancement vers L2 en 2026. Les deux objectifs scientifiques principaux de la mission sont la détection d’exoplanètes de type terrestres dans la zone habitable d’étoiles de type solaire, ainsi que le caractérisation de centaines de planètes de tous types.

    Durant ce séminaire, en plus du statut général de la mission, je rappellerai ces objectifs scientifiques et détaillerai les solutions instrumentales explorées pour résoudre ce challenge.


  • Mercredi 28 mars 2018 à 11h00 (Salle de conférence du bâtiment 17)

    Evolution of magnetic structures in the pre-phase of X class flares

    Guiping Ruan (Shandong University, Weihai, Chine & LESIA)

    We analysed the long term pre-flare conditions of X2.1 and X1.8 flares. The events respectively includes a sigmoidal filament eruption, a coronal mass ejection, and a GOES X flare from NOAA active region 11283. Based on the HMI observation, for an area along the polarity inversion line underneath the filament, we found gradual pre-eruption decreases of both the mean strength of the photospheric horizontal field (Bh) and the mean inclination angle. We propose that the pre-event evolution of Bh may be used to discern the driving mechanism of eruptions. We also showed the expansion of the arcades overlying the filament until the reconnection. The reconnection occurred between the arcades and the pre-existing magnetic field. A NLFFF modelling confirmed the present scenario. I will present the two projects that I started at the LESIA :
    1. Study of eruptions and jets observed during a IRIS campaign with the MSDP of the solar tower.
    2. Study of the prominence plasma characteristics based on IRIS Mg II line profiles and MSDP Halpha line and radiative codes developed in Czech Republic.


  • Vendredi 23 mars 2018 à 14h00 (Salle de conférence du bâtiment 17)

    An ADCS 3-axis testbed system for nano/micro satellites

    Hoang The Huynh (USTH & LESIA)

    The development of nano/micro satellites is a new trend in space. The amount of those satellites is increasing rapidly by the time. Testing attitude determination and control system (ADCS) is playing an important role to the success of a satellite project. A testbed system is an essential tool to support the satellite developers. The talk will present the project of a hardware-in-the-loop system to test control laws and algorithms for ADCS of nano/micro satellites managed by the Vietnam National Space Center (VNSC). The system consists of three space environment condition simulators : zero gravity, Earth’s magnetic field and Sun light. This testbed system is expected to test various ADCS configurations of nano/micro satellites. Firstly, it will be a test platform for ADCS of NanoDragon satellite at VNSC. In addition, the talk will also present the PhD topic “Advanced Attitude Determination for Satellite ADCS Test-bed Using Multi-Sensor Fusion” that is one of the improvement research topics for above testbed system.

    Proposé par Boris Segret et Benoit Mosser.


  • Jeudi 22 mars 2018 à 11h00 (Salle de conférence du bâtiment 17)

    About Type II Radio Bursts (to be defined)

    Iver Cairns (University of Sydney, Australie)


  • Mardi 20 mars 2018 à 14h00 (Salle 204 du bâtiment Evry Schatzman (18))

    Ringdowns and echoes from the optical geometry perspective

    Marek Abramowicz (Varsovie et Göteborg)

    An observational proof for the existence of the event horizon is fundamentally impossible. However, there are many strong "near proofs". One of them, recently pointed out by Thibault Damour, and further discussed by Vitor Cardoso and others, is an absence of echoes in the gravitational wave ringdowns. I will give a pedagogical explanation of the issue in terms of the optical geometry. The optical geometry was introduced (in a different context) by Garry Gibbons and later explained dynamically by Brandon Carter, Jean-Pierre Lasota and me, and explored by many other authors.


  • Jeudi 15 mars 2018 à 16h00 (Salle de conférence du bâtiment 17)

    Observations of fast-moving structures in the debris disk of AU Microscopii : 3 years of follow-up with SPHERE

    Anthony Boccaletti (LESIA)

    The instrument SPHERE was installed at the VLT in 2014 and provides a significant gain in terms of contrast with respect to the previous generation of instruments. As a result, we now have access to very high contrast in the close environment of bright stars in particular the young systems in order to search for giant planets and circumstellar disks. During the commissioning in Aug 2014, SPHERE has revealed several structures (several AU in size) in the form of arches or undulations in the midplane of the debris disk around the star AU Microscopii. This disk is seen edge on and the system is conveniently close ( 10 pc) and young as well ( 20 Myr). The comparison of these SPHERE observations with the ones from STIS/HST 4 years before, not only allowed us to re-identify the structures in older data but most importantly led us to conclude that these structures were moving outwards in the disk, some with very large projected speed (4-10 km/s) hence possibly escaping the system. Several assumptions were considered to explain this behaviour, one of the them involves a body in Keplerian motion releasing some dust under the influence of the star’s activity. Since then, the object is regularly observed with SPHERE as part of the GTO and during a monitoring program. After a short introduction on the instrument and its modes as well as the achieved performance, I’ll remind the initial results from 2014 which led to the discovery of these fast-moving structures. Then, I’ll present the recent observations obtained from the last 3 years which unambiguously confirm the motion of the structures. The hypothesis of a parent body emitting an outflow of dust will be discussed in the light of these observations.


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