Seminars Temps-Espace

Since the detection of absorption features in spectra of beta Pictoris in 1990 (Beust et al., 1990) observations of absorption lines varying on short time scales in spectra of stars accumulate. Scientists refer to these findings as features caused by objects evaporating material on their orbit when they come close to the star and thus call them comets in exoplanetary systems -- exocomets. This theory is based on the knowledge about the Solar System. The aim of our dynamical investigation is to find a statistical model for the scattering of small bodies which shows the most probable whereabouts of these objects after the gravitational interaction with the planets. We will show results from our n-body simulations including a star, a Jupiter-like planet and a disk of planetesimals (testparticles). As a consequence of the migration of the gas giant planetesimals are scattered either inward or outward. The outward scattered objects will form analogues to the Kuiper belt respectively the Oort Cloud in our Solar System. The created reservoirs are different depending on the initial conditions of the planetesimal disk, migration of the Jupiter-like planet as well as mass and orbit of the giant planet. We measure semi-major axis, eccentricity, perihel, aphel, inclination and orbital period after 4byr of integration of each testparticle and compare the outcomes of the computations with different acting forces applied -- as there are gravitational influence of the galactic tide and passing stars. Keeping in mind the differences of the confirmed exoplanetary systems and the architecture of our own Solar System we change the number of planets interacting with the small bodies. We show that the scattering process of the testparticles, involving more than one gas giants, is more efficient in putting the planetesimals to further out distances. In order to complete our studies we, too, start with different masses of the central star and different initial conditions for the planets (mass, orbit...) as given from observations. Statistics of the orbits of small bodies after being scattered by the planets are shown for some sample confirmed planetary systems. This might give a clue to observers on where to look for features being produced by cometary bodies in extrasolar systems. The gained knowledge can be used to generate a general model for the formation of cometary reservoirs in extrasolar systems with respect to the system architecture which can be used to predict the location of cometary reservoirs in extrasolar systems.

The SPICA Infrared Observatory has been selected by ESA on May 7, 2018 for further study as part of the M5 competition. It carries 3 instruments, SMI, B-BoP, and SAFARI, covering the 17-230 µm range, with a wavelength resolution R between a few hundred and a thousand, combined with various efficient large area imaging and polarimetry modes. The SPICA telescope will be cooled down to about 8K, effectively suppressing most of the satellite's infrared thermal background, which will allow us to reach down to very low fluxes. SPICA will provide spectroscopic capabilities at a high sensitivity of 2-15 x1e-20 W/m2 (5?/1hr), much deeper than Herschel. The scientific key objectives of SPICA are i) to reveal the physical processes that govern the formation and evolution of galaxies and black holes, ii) to resolve for the first time the far-infrared polarization, and therefore the magnetic field, of galactic filaments, and iii) to understand the formation and evolution of planetary systems. I will present the SPICA mission, its capabilities and the key scientific objectives.

The aim of this work is to define the dynamical parameters of asteroids and their satellites based on their astrometric observations. We used the model of motion that took into account the gravitational influence of a primary's axisymmetric non-sphericity. This factor leads to precession of the line of apsides as well as to precession of a satellite's orbit around primary's axis of symmetry. The most appropriate object for our model is the asteroid (22) Kalliope with the satellite Linus. In addition to previously accumulated observations we used a new series of speckle interferometric observations of this system performed in 2017-2018. These observations extended the time interval of observations, thus enabling to detect the precession of the satellite's orbit at 216 degrees. This allowed to find all parameters of the satellite's orbit, the total mass of the system, non-sphericity of Kalliope and the direction of the orbit precession axis. The detected orbit precession is due to the attraction of an extended axisymmetric body formed by rapidly rotating Kalliope. These are the first results obtained on the basis of dynamical study of the primary's extension, unlike earlier studies where results were obtained by using photometric observations which give only apparent external shape of Kalliope that does not necessarily reflect its gravitational field. The paper gives values of all dynamical parameters of the system as well as the results of new positional observations of the Kalliope-Linus system.

Suite au succès de la visite et de la collecte d'échantillons de l’astéroïde de type-S Itokawa par la sonde spatiale Hayabusa-1, la JAXA a décidé d'initier l'exploration et le retour d’échantillons d'un autre astéroïde par une seconde mission Hayabusa-2. La cible retenue est un astéroïde de type-C nommé Ryugu. Si le satellite est très similaire à celui d'Hayabusa-1, cette mission est encore plus ambitieuse et propose une diversité unique de moyens d'exploration avec notamment plusieurs atterrisseurs dont un de conception franco-allemande (Mascot) qui a pu se poser avec succès sur la surface. La collecte de données et leurs analyses sont en cours mais elles s'avèrent déjà remarquables. Je présenterai donc cette mission, les opérations qui se sont parfois révélées aventureuses en raison de la surface surprenante de Ryugu et les résultats majeurs obtenus par certains des instruments à bord de Mascot et de Hayabusa-2.

Since the 1970s Very Long Baseline Interferometry (VLBI) has proven to be a main space geodetic technique by determining Terrestrial Reference Frame (TRF), monitoring the variable Earth rotation and orientation with highest precision, and by deriving many other parameters of the Earth system. Further, geodetic VLBI is the only space-geodetic technique able to realize the International Celestial Reference System (ICRS). Accurate Reference Frames (TRF) are indispensable for many applications, e.g. navigation and mapping on Earth, precise orbit determination for satellites, and geophysical applications, such as monitoring tectonic motions, and observing the variations of the sea level. Especially for the latter the requirements for the accuracy and long term stability are very high, i.e. better than 1 mm and 0.1 mm per year. This goal has not yet been achieved. Main obstacles are the inconsistencies between the different techniques which contribute to their determination and their dependencies on each other. The current realization of the ICRS, the third International Celestial Reference Frame (ICRF3, Charlot et al. 2018), is the main product of the astrometric and geodetic VLBI and its major contribution to fundamental astronomy. It was realized as three independent CRFs at three frequencies from one analysis center, in contrast to the ITRF which combine all space geodetic techniques. Further, the current coordinate model of the ICRF3 sources consists of time-invariant coordinates in right ascension and declination. Hence, any deviation from a constant position is categorized as noise. In reality, sources can have structures differing from the assumed point like ideal and their position can be subjected to significant changes. If unaccounted for, these changes will be absorbed by other parameters, leading to systematic effects in the Earth orientation parameter (EOP) estimates. This talk will give a short overview of geodetic VLBI and an insight to my recent work on the determination source positions and CRFs.

Asteroids in our solar system are metallic, rocky and/or icy objects, ranging in size from a few meters to a few hundreds of kilometers. Whereas we now possess constraints for the surface composition of most D>100 km primordial main-belt asteroids, little is known regarding their internal structure. Yet, this is a fundamental property whose characteristics result directly from (a) their formation location, (b) their time of formation, and (c) their collisional history. Characterizing the internal structure of the main compositional classes of asteroids would therefore allow us to address entirely new questions regarding the earliest stages of planetesimal formation and their subsequent collisional and dynamical evolution. To achieve this goal, we carry out - via an ESO Large Program (LP) that was awarded 152h on VLT/SPHERE (the observations are spread over 4 semesters from April 1st, 2017 till March 30, 2019 in service mode) - disk-resolved observations of a substantial fraction of all D>100 km main-belt asteroids (sampling the four main compositional classes) at high angular resolution with VLT/SPHERE throughout their rotation. These observations enable us to derive their volume (via their 3-D shape) which combined with already existing mass estimates allow us to determine their bulk density and hence to characterize their internal structure. The high-resolution images also allow us to detect craters larger than 30 km and use their morphology (crater diameter and depth) to characterize the density of the outer shell. The knowledge of both the bulk density and the density of the outer shell of our targets allows a characterization of their internal structure. This information, in turn, allows us to determine: (a) the nature of their initial building blocks (rock only, or a mixture of ice and rock) and (b) which compositional classes experienced differentiation. These constraints then serve as direct inputs to thermal evolution models for determining the time of formation and the formation location (inward or outward of the snowline) of the main compositional classes of objects in the asteroid belt.

Ce séminaire spécial à deux voix aura un format spécial, comme environ une fois l'an quand le sujet s'y prête. Deux interventions viendront donc ponctuer cet après-midi, avec une pause café méridienne qui facilitera les questions et échanges dans l'assistance. 14h-15h : Estefanía de Mirandés (BIMP). La révision du Système International d’Unités. Résumé : Le 16 novembre 2018 la Conférence Générale des Poids et Mesures a approuvé une révision du système international d’unités (SI) qui entrera en vigueur le 20 mai 2019. Quatre des sept unités de base du SI - le kilogramme, l’ampère, le kelvin et la mole - seront redéfinies par rapport à des valeurs fixées de constantes de la nature – la constante de Planck, la charge élémentaire, la constante de Boltzmann et la constante d’Avogadro -. Cette révision représente l’aboutissement du rêve de Stoney, Planck et d’autres de mettre en place un système naturel d’unités fondé sur des invariants de la nature, car après la révision du SI aucune unité ne sera plus définie à partir d’un étalon matériel. L’exposé présentera le détail de cette refonte, les raisons qui l’ont poussée, ainsi que la méthodologie suivie pour choisir et fixer la valeur de ces constantes. Une perspective sur les conséquences envisageables de cette révision sera également proposée. 15h30-16h30 : Jean-Philippe Uzan (IAP) Les constantes fondamentales - le nouveau SI et la Relativité générale. Résumé : Le nouveau système international d’unités qui a été adopté le 16 novembre 2018 fonde la définitions des unités en fixant la valeur numérique d’un jeu de constantes de la nature. Cet exposé reviendra sur ce choix qui est l’aboutissement d’une longue histoire. Il rappellera le rôle des constantes dans les lois de la nature et soulignera les échanges avec la théorie. Pour finir, nous discuterons de l’hypothèse selon laquelle ces paramètres sont constants, aussi bien d’un point de vue théorique qu’expérimental, ce qui soulignera un lien avec le principe d’équivalence au coeur de la Relativité générale.

In summer and autumn 1676 both Cassini and Rømer announced the discovery of the velocity of light to the Académie royale des Sciences and they mentioned a value of some 10-11 minutes/AU. Both Cassini and Rømer ascribed the discovery to Rømer, but it is nevertheless sometimes claimed that Rømer took over the idea from Cassini, who had abandoned it. These claims indirectly accuse Cassini and Rømer of scientific malpractice and leave many open questions. We discuss the background for the discovery, the difficulties involved and why the value was so far from the expected 8.3 minutes/AU. We show that by looking at the events in 1676 in connexion with the scientific priorities of Cassini the mystery of the double announcement can be resolved.

Comets in the Oort cloud evolve under the influence of internal and external perturbations, such as giant planets, stellar passages, and the galactic tide. We aim to study the dynamical evolution of the comets in the Oort cloud, accounting for the perturbation of the galactic tidal field and passing stars. We base our study on three main approaches; analytic, observational and numerical. We first construct an analytical model of stellar encounters. We find that the cumulative effect of passing stars can strip the Oort cloud on a very short time scale(<500 Myr). Using proper motions, parallaxes, and radial velocities from Gaia DR2 and combining them with the radial velocities from external surveys, we construct an astrometric catalogue of the 14,659 stars that are closer than 50pc to the Sun. We calculate the encounters that are closer than 2.5pc and that the Sun has had in the last 10Myr and will have in the near future 10Myr. Finally, we study the dynamical evolution of the comets in the Oort cloud under the effect of multiple stellar encounters from stars that pass within 2.5pc from the Sun and the galactic tide over ±10Myr. For this, we use the Astrophysical Multipurpose Software Environment (AMUSE), and the GPU-accelerated direct N-body code ABIE. We find that the cumulative effect of relative distant stellar encounters together with the galactic tidal field, proves to be an efficient mechanism in the creation of interstellar comets. This raises the question about the formation, evolution and current status of the Oort cloud, as well as, the existence of an Interstellar Oort Cloud. A larger sample of stars constructed through less filtering or an incompleteness correction can only increase the comet loss.

Since the detection of absorption features in spectra of beta Pictoris in 1990 (Beust et al., 1990) observations of absorption lines varying on short time scales in spectra of stars accumulate. Scientists refer to these findings as features caused by objects evaporating material on their orbit when they come close to the star and thus call them comets in exoplanetary systems -- exocomets. This theory is based on the knowledge about the Solar System. The aim of our dynamical investigation is to find a statistical model for the scattering of small bodies which shows the most probable whereabouts of these objects after the gravitational interaction with the planets. We will show results from our n-body simulations including a star, a Jupiter-like planet and a disk of planetesimals (testparticles). As a consequence of the migration of the gas giant planetesimals are scattered either inward or outward. The outward scattered objects will form analogues to the Kuiper belt respectively the Oort Cloud in our Solar System. The created reservoirs are different depending on the initial conditions of the planetesimal disk, migration of the Jupiter-like planet as well as mass and orbit of the giant planet. We measure semi-major axis, eccentricity, perihel, aphel, inclination and orbital period after 4byr of integration of each testparticle and compare the outcomes of the computations with different acting forces applied -- as there are gravitational influence of the galactic tide and passing stars. Keeping in mind the differences of the confirmed exoplanetary systems and the architecture of our own Solar System we change the number of planets interacting with the small bodies. We show that the scattering process of the testparticles, involving more than one gas giants, is more efficient in putting the planetesimals to further out distances. In order to complete our studies we, too, start with different masses of the central star and different initial conditions for the planets (mass, orbit...) as given from observations. Statistics of the orbits of small bodies after being scattered by the planets are shown for some sample confirmed planetary systems. This might give a clue to observers on where to look for features being produced by cometary bodies in extrasolar systems. The gained knowledge can be used to generate a general model for the formation of cometary reservoirs in extrasolar systems with respect to the system architecture which can be used to predict the location of cometary reservoirs in extrasolar systems.

For a dynamically closed universe governed by either Newtonian gravity or general relativity, I will discuss the consequences of two assumptions: 1) physical quantities are dimensionless ratios; 2) the scale variable of the universe increases monotonically in both temporal directions away from a unique minimum. In a talk given at the Observatory in 2014, I discussed the case of a non-vanishing minimum and its potential to explain the arrows of time, including the second law of thermodynamics. In this talk I will discuss the intriguing and possibly far-reaching consequences of assumption 1) if the scale variable vanishes at its minimum (total collision in the N-body problem and big bang in general relativity).

L'hypothèse d'une matière noire adéquate fut inventée par Fritz Zwicky en 1933 pour stabiliser les mouvements internes, trop rapides pour un équilibre gravitationnel ordinaire, dans les galaxies et les amas de galaxies. Une autre hypothèse explicative fut avancée par Mordehai Milgrom en 1987 : une petite modification des lois de la gravitation pour les accélération très faibles. La question se pose cependant de savoir si un équilibre strict est vraiment nécessaire pour faire admettre ces grandes formations. Déjà, en ce qui concerne les galaxies, il apparaît finalement que l'attraction interne des étoiles est suffisante pour un quasi-équilibre de leur presque totalité et ce sont essentiellement les nuages de gaz alentour qui ont une vitesse trop rapide. Sans doute ces nuages sont-ils en voie d'évasion tout comme le vent solaire (plusieurs millions de tonnes par seconde) s'échappe continuellement du Système solaire sans modifier notablement celui-ci. En dix milliards d'années de la vie du Soleil, la masse du vent solaire émis ne représente que 0,03% de la masse totale du Soleil. Pour les amas de galaxies la question principale n'est pas de savoir s'ils sont gravitationnellement stables : ils ne le sont pas. Ce qui importe est de savoir si leur dispersion est moins rapide que l'expansion de l'Univers. Les amas ayant une énergie cinétique bien supérieure à leur potentiel gravitationnel les galaxies qui les composent se comportent presque comme si elles étaient isolées dans l'espace, mais dans un espace en expansion un corps isolé n'avance pas à vitesse uniforme... Cette question requiert l'utilisation de la Relativité générale et le résultat est probant : dans le système de coordonnées co-mobile les vitesses relatives des galaxies sont en voie de décélération rapide et leurs déplacements sont limités. Bien entendu les (petites) attractions gravitationnelles intergalactiques renforcent cette stabilité. Les amas de galaxies conservent donc leur individualité même en l'absence de matière noire... Ce séminaire discutera l'ensemble de ces arguments, basés sur les lois de la gravitation de la mécanique classique et de la Relativité.

The Time Transfer by Laser Link (T2L2) experiment on-board the Jason-2 satellite (launched the 20 June 2008, at 1335 km of altitude) aims to synchronize remote clocks in the ground with a sub-nanosecond accuracy. Except short interruptions, the experiment worked perfectly from June 2008 to April 2018, for almost 10 years. T2L2 consists in an electronic device for timing, linked to the Doppler Orbitography Radiopositioning Integrated by Satellite (DORIS) Ultra Stable Oscillator (USO), which delivers the frequency reference to the whole satellite, and an optical device that detected the laser pulses coming from the laser stations of the International Laser Ranging Service (ILRS). T2L2 offered a time colocation with three geodetic techniques on-board the Jason-2 satellite (SLR, DORIS and Global Positioning System (GPS)), and with the ground. It is a unique opportunity to reduce the systematics of these techniques, linked to the “time observable” (e.g. clock stability, time biases…) and meet the next requirement for geodesy; “the millimeter level”. After a quick review of the main results obtained during these last 10 years, I will present the impacts and applications of the T2L2 experiment for space geodesy. I will focus on the DORIS and SLR techniques, by two aspects: - The development of an USO model, with the use of T2L2 and its impact on Precise Orbit Determination (POD) and beacons positioning. - The measurement of Time biases in the SLR stations, and their impacts on geodetic products.