Max-Planck-Institut für Sonnensystemforschung

Raum: Auditorium
Discussions on Comets - Heat transport phenomena in the outer layers of cometary nuclei [mehr]

MPS Seminar: Reflecting MHD waves in hot coronal loops observed by SDO/AIA (P. Kumar)

  • Datum: 25.07.2014
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Pankaj Kumar
  • Korea Astrononomy and Space Science Institute (KASI), Deajeon, Korea
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Hardi Peter
Reflecting MHD waves in hot coronal loops observed by SDO/AIA [mehr]

MPS Seminar: Asteroseismology, Exoplanets, and Galactic Archaeology: intriguing matches along the (Milky) way (V. Silva)

Asteroseismology, Exoplanets, and Galactic Archaeology: intriguing matches along the (Milky) way [mehr]

MPS Seminar: The Constant Sun: Measuring the Solar Radius and Oblateness with the Helioseismic and Magnetic Imager (R. Bush)

MPS Seminar: High resolution spectropolarimetric study of sunspot light bridges (L. Bharti)

High resolution spectropolarimetric study of sunspot light bridges [mehr]

MPS Seminar: Fast magnetic reconnection in the solar chromosphere mediated by the plasmoid instability (L. Ni)

  • Datum: 23.10.2014
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Lei Ni
  • Yunnan Observatories, Kunming, China and University Potsdam, Germany
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Hardi Peter
Fast magnetic reconnection in the solar chromosphere mediated by the plasmoid instability [mehr]

Planetary Group Seminar: Titan’s chaotic upper atmosphere (I. Mueller-Wodarg)

Titan’s chaotic upper atmosphere Abstract: Saturn’s largest moon Titan has been observed systematically since the arrival of Cassini/Huygens in 2004. While the landing of the Huygens probe in January 2005 provided amongst other a continuous, yet single vertical profile of atmospheric properties from the thermosphere down to the surface, regular in-situ observations by the Cassini orbiter’s Ion Neutral Mass Spectrometer (INMS) above 950 km provided information on global and time variations in Titan’s thermosphere. Infrared remote sensing onboard Cassini provided further details on Titan’s stratosphere and troposphere, while UV occultations measured the mesosphere and lower thermosphere.   After 10 years of regular observations, Titan has proven to possess one of the most enigmatic atmospheres explored to-date. Density variations observed in the thermosphere show dramatic variations by orders of magnitude between observations and temperatures can vary by 100 K from one flyby to another - rates which are difficult to interpret physically. Equally, horizontal structures are counter-intuitive, suggesting a slightly hotter dayside than nightside on Titan. Work over the past years has attempted and largely failed to systematically correlate these atmosphere structures with changing conditions in Saturn’s magnetosphere, another potential energy source.  Most recently, our work has explored the potential influence of vertical coupling in the atmosphere, of Titan’s lower atmosphere driving changes above. By coupling the Titan WRF stratosphere model with our Titan Thermosphere General Circulation Model, we have found small and short term variations in the stratosphere to drive considerable variability in the thermosphere as well, remarkably consistent with observations. Our findings highlight the broader principle of processes which play a secondary role in atmospheres of bodies closer to the Sun becoming primary in nature in atmospheres further out in the solar system where solar heating is no longer a dominant thermal energy source. [mehr]

MPS Seminar: Fragmented currents induced by shear flows as heating and dissipation mechanisms in flares and the quiet solar atmosphere (D. Nickeler)

Fragmented currents induced by shear flows as heating and dissipation mechanisms in flares and the quiet solar atmosphere [mehr]

Video-Seminar: Magnetic Islands and Singular Currents at Rational Surfaces in Three-dimensional MHD Equilibria (J. Loizum)

Magnetic Islands and Singular Currents at Rational Surfaces in Three-dimensional MHD Equilibria [mehr]

MPS Seminar: SOFIA - past, present, and future (H. Zinnecker)

SOFIA - past, present, and future Abstract:SOFIA, the Stratospheric Observatory for Infrared Astronomy, has reached full operational capability in April 2014 and has since undergone a major overhaul at Lufthansa Technik in Hamburg. Cycle 3 observing time has been awarded and some 80 flights will be carried out in 2015, including a southern deployment to New Zealand. In this talk we will summarize the current status of SOFIA, its instrument suite, and some of the recent science highlights of Cycle 1 and 2 (e.g. star formation and astrochemistry). After a difficult year in terms of NASA support, SOFIA is getting back into gear poised to continue delivering unique mid- and far-infrared science, in the post-Spitzer and post-Herschel era. [mehr]

MPS Seminar: Primary cause of the extended cycle 23 minimum (J. Jiang)

Primary cause of the extended cycle 23 minimum [mehr]

MPS Seminar: Spectropolarimetry for solar magnetometry (R. Manso Sainz)

Spectropolarimetry for solar magnetometry [mehr]

Planetary Group Seminar: Rocks from Vestas: Implications for understanding Earth’s evolution (K. Mengel)

  • Cancelled!
  • Datum: 06.05.2015
  • Uhrzeit: 10:00 - 11:00
  • Vortragende(r): Kurt Mengel
  • University of Technology, Clausthal, Germany www.ielf.tu-clausthal.de
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall

S3 Seminar: Correlation of Magnetic Field wiht Chromospheric Features (K. Barczynski)

MPS Seminar: A Closer Look at Sunspot Oscillations with IRIS (C. Madsen)

  • Datum: 07.05.2015
  • Uhrzeit: 14:30 - 15:30
  • Vortragende(r): Chad Madsen
  • Harvard-Smithsonian Center for Astrophysics, Cambridge and Boston University
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Hardi Peter

Solar Group Seminar: How deep are sunspots? (B. Beeck)

MPS Seminar: Spring in Martian polar areas (G. Portyankina)

Spring on Mars is a time of active changes in polar areas, at latitudes covered by seasonal CO2 ice. The High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO) has imaged five southern and four northern spring seasons. This temporal coverage allows studying seasonal changes in details, comparing phenomena in the south to the north, and one spring to the next. The volatile nature of the CO2 sublimation in spring leads to erosion and local redistribution of loose material on the surface. The best known and one of the most enigmatic examples of resulting terrain are so called araneiforms (shown in Fig. 1). Araneiforms are observed in southern polar areas only. They are believed to be troughs carved in the substrate by gaseous CO2, with the CO2 ice layer subliming from its bottom. In the northern hemisphere seasonal activity is mostly concentrated on the circumpolar dunes. When gaseous CO2 travels between seasonal ice layer and the dune surface, it creates furrows – channels so small, they get erased in summer by sand movement and created again in spring. The dark and bright fans, observed in both north and south polar areas (an example from the north is in Fig. 2) are a representation of the same phenomena. The fans are results of outbursts of CO2 gas coming from below CO2 ice layer dragging dust and sand with it. A hypothesis for creating the observed phenomena was proposed by H. Kieffer. It is based on the solid-state green house effect acting in the seasonal CO2 ice layer. The diversity of observed features in seasonal polar caps of Mars are produced when this process interacts with water ice, dust, and/or sand grains of the surface and the atmosphere. Most recent observations as well as modeling of spring activity on Mars and related experimental investigations will be discussed in the talk. [mehr]

S3 Seminar: Fast Solar Polarimeter: First Results and Future Work (F. Iglesias)

Planetary Group Seminar: At the heart of Jupiter's aurora (D. Grodent)

  • Datum: 21.05.2015
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Denis Grodent
  • Laboratory for Planetary and Atmospheric Physics Université de Liège, Belgium
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall

Planetary Group Seminar: Waves in terrestrial and planetary atmospheres (E. Yigit)

Atmospheric gravity waves are basic features of all planetary atmospheres. But what is their importance? In Earth's atmosphere they are primarily generated by various meteorological processes, propagate upward, produce substantial dynamical and thermal effects and variability in the mesosphere and thermosphere, and thus vertically couple the lower and upper atmosphere. Similar gravity wave processes are increasingly encountered in other planetary atmospheres. In this seminar, I will introduce how small-scale gravity waves are represented in global models and present a snapshot of recent progress in modeling their effects, specifically, in Earth and Martian atmospheres. Gravity wave processes in the context of NASA’s MAVEN mission are discussed. [mehr]

S3 Seminar: The Activity of Comet 67P / CG (S. Höfner)

S3 Seminar: Formation of Comets by Gravitational Collapse of Pebble Clouds (S. Lorek)

Planetary Group Seminar: AIDA: Asteroid Impact & Deflection Assessment (J.-B. Vincent)

The AIDA mission will be the first space experiment to demonstrate asteroid impact hazard mitigation by using a kinetic impactor to deflect an asteroid. It consists of ESA's orbiter AIM which will orbit the binary asteroid Didymos in 2022, and NASA's DART projectile scheduled for impact on the secondary in October 2022, while Didymos is at its closest approach to Earth. Both AIM and ground based telescopes will measure the change of orbit of the secondary. AIDA will return vital data to determine the momentum transfer efficiency of the kinetic impact and measure key physical properties of the target asteroid. Additionally, a lander and a full suite of instruments will give us the first tomographic map of an asteroid interior. [mehr]

Planetary Group Seminar: A tale about dwarfs (M. Hoffmann)

The Dawn spacecraft has visited asteroid Vesta and is now in orbit around dwarf planet Ceres. Its data revealed quite individual bodies despite similar size and similar location in the solar system. These “minor planets” are new milestones on the way to a revised view onto the planets: Classification as “planets”, “comets”, “satellites” becomes more misleading than describing. A comparative view on the former “asteroids” Vesta and Ceres will demonstrate this. [mehr]

S3 Seminar: Coronal Active Region Modelling based on SDO Data (S. Barra)

S3 Seminar: Observing and Modelling the Dust Mantle Activity on Comet 67P / C.-G. (X. Hu)

S3 Seminar: Photometric Calibration of Historical SHGs (T. Chatzistergos)

S3 Seminar: Anomalous Reversed Evershed Flow in a Sunspot Penumbra (A. Siu)

MPS Seminar: THOR: Turbulent Heating ObserveR (E. Kronberg)

Planetary Group Seminar: The Heavy Bombardment Eon of the Earth-Moon-System (V. Assis Fernandes)

  • Datum: 03.09.2015
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Vera Assis Fernandes
  • Museum für Naturkunde, BerlinLeibniz-Institut für Evolutions- und Biodiversitätsforschung, Berlin The Centre for Earth Evolution and Dynamics, University of Oslo, Oslo
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Introduction: The impact cratering shaped Moon’s landscapes offer a fossil record of the Near Earth Object populations. This record goes back to the formation and cooling of the lunar crust [1-3] when the crust was sufficiently viscous to retain the cratering “scars”. The crater densities of highland and mare surfaces testify a substantially higher impact flux rate during the first ~1.5 Ga compared to that for the last 3 Ga of our Solar System. The temporal evolution of the impact flux (i.e., the bombardment timeline) is the topic of intense scientific debate for at least the past 40 years. The end-member interpretations are 1) the “Early Heavy Bombardment” (EHB) that assumes an exponentially declining impact flux rate until it oscillated around a much lower value during the last 3 Ga, and 2) the “Late Heavy Bombardment” (LHB) referring to a brief “terminal lunar cataclysm” with a sharply rising and falling peak centered around 3.9 Ga ago [1,2]. On current state of concepts: While the EHB may still be considered the least assumptions model consistent with our fuzzy sample-based knowledge of the bombardment timeline, it lacks a proper physical (orbital) explanation. In light of the recent knowledge from lunar, terrestrial and asteroid belt samples, the classical LHB scenario is no longer attractive [1,2]. In addition, it appears highly inconsistent with orbital models [4-5]. This particularly stems from the difficulty or even impossibility to properly correlate the Apollo and Luna samples to their bedrock or crater ejecta source. However, present re-interpretation of old data together with acquisition of new data from Apollo and Luna samples suggest that intermediate views that consider a complex bombardment timeline with moments of heavy bombardment are a better venue to consensus. Two events able to initiate moments of heavy bombardment are: 1) The giant Moon forming impact event created an extremely massive heliocentric debris disk; meaning a new projectile population with high impact probability onto the Earth and the Moon for the following few hundred million years [6-7]. 2) The reorganization of the planetary system architecture as proposed by the updated “Nice”-model basically explains the extended tail-end of the heavy bombardment as testified by the crater density on mare basalts and possibly the Archean spherule layers on Earth [4]. However the level of resolution in dynamical models is not yet equal to data from samples. 3) Other impactor populations (planetary left overs, comets, debris discs, asteroid belts) that resulted from single events or dynamical processes leading to additional spikes in the impact flux cannot be excluded. One should be aware that “you don’t know what you don’t know”. Therefore, additional work on current samples and/or new samples is required. Acknowledgments: All this work has been carried out in collaboration with Jörg Fritz and Stephanie Werner. References: [1] Fernandes V. A. et al. 2013. MaPS 48:241–269. [2] Fritz J. et al. 2014. PSS 98:254–267. [3] Werner S.C. et al. 2002. Icarus 156:287-290. [4] Werner, S.C. 2014. EPSL 400:54–65. [5] Morbidelli A. et al. 2012. EPSL 355:144–151. [6] Schlichting H. et al. 2012. Astroph. J. 8:8. [7] Jackson A.P. and Wyatt M. 2012. Month. N. R. Astron. Soc. 425:657–679. [mehr]

MPS Seminar: Probing Solar Magnetic Fields at the Base of Convection Zone (D. Chou)

Rosetta Seminar: First touch down of Philae - an update (R. Roll)

MPS Seminar: Numerical simulation modelling of convection and pulsation (F. Kupka)

Solar Group Seminar: Eruptions at Sun and in the Laboratory (J. Büchner)

MPS Seminar: Asteroseismology: Observations of solar-like pulsators (G.Davies)

Assumptions on the early evolution of the Asteroid Vesta include a combined (i) ordinary plus carbonaceous chondritic bulk composition, (ii) complete melting of the silicate fraction within tens of Ma after CAI, (iii) equilibration of silicate material and FeNiS-core, as well as (iv) formation of an ultramafic (peridotitic/pyroxenetic) lower crust and upper mantle plus a basaltic crust. There is, however, little consensus about the volume proportions within the silicate components. Estimates of the thickness of the basaltic crust depend on crystallization models of the bulk silicate composition. The diogenitic component of DAG 779 (believed to originate from Vesta) reveals temperatures of orthopyroxene (opx) formation from 1450 and 1200 °C measured for bulk exsolved opx and for host regions between exolution lamellae , respectively. This range coincides with calculated temperatures of opx formation by equilibrium and fractional crystallization sequences for Vestas silicate shell. Calculations of the thickness of the remaining basaltic (eucritic) crust and the onset of the ultramafic interior suggest depths of 20 to 40 km. The early large impacts that produced the Veneneia and Reasilvia basins most probably excavated rocks from this depth but did not produce large amounts of olivine-rich rocks on Vestas surface. In the light of the above mentioned crystallization models, an orthopyroxenite-rich layer can be assumed to depth of up to 80 km; olivine-dominated rocks are probably restricted to Vestas deeper mantle. [mehr]

Kometenfieber: Kometenforschung von Giotto bis Rosetta (E. Grün)

Öffentliche Vortragsreihe

Planetary Group Seminar: Deep subsurface radio probing of the icy moons: what can we expect from it? (Y. Ilyushin)

Icy moons of giant planets are now known to have liquid water oceans beneath their icy mantles. Deep radio probing is the only chance to get immediate proof of that now. In the presented talk, issues of deep radio probing of icy moons are addressed. Previously developed theoretical background of Martian GPR exploration is reviewed. A new type instrument concept -- a passive radio wave sounder -- is introduced. Utilization of Jovian natural radio emissions as a sounding wave allows to create a low mass and weight radio instrument exceeding active radars in sounding capabilities. Comparative analysis of both active and passive instrument types and simulation results supporting feasibility of the new instrument are presented. [mehr]
Recent surface processes on Mars are dominated by aeolian and ice-related activity controlled by seasonal atmospheric cycles. For the Martian past, it has become widely accepted that cyclic changes in the planet's orbital configuration has been causing changes on much larger temporal and regional scales leading to re-distribution of polar ices and deposition of ice-rich so-called mantling deposits. While some observational evidence indeed points towards links between extensive mid-latitude glaciation and climate cycles on Mars, questions related to the origin of ice remain unanswered. In this talk, some of these links based on geomorphic observations are discussed. [mehr]

MPS Seminar: Observing Cycles, Seasons, and Storms (S.W. McIntosh)

Recent observational findings suggest that the 11(-ish) solar sunspot cycle is a pattern resulting from the interaction, or interference, of large scale magnetic field bands that evolve within the Sun’s convective interior over it’s 22-year magnetic polarity reversal cycle. These toroidal magnetic bands are anchored deep in the solar convection zone and migrate from high latitudes to the equator over 22 years, and new analysis techniques have allowed us to trace their migration from birth to death. We will see that the spatio-temporal interaction of these magnetic bands helps us frame the landmarks of the sunspot cycle with a surprising realization that, once considered, permits a deeper look into the gross energetics of the star, its radiative, particulate and eruptive output and how they vary with time. It is possible that, with refinement and an ongoing commitment to synoptic observational programs, these results offer greatly improved forecast skill on monthly, annual and decadal timescales while a comprehensive physical model can be developed. Finally, we'll think about what observations are required to "close the loop" and drive that modeling effort. [mehr]

Planetary Group Seminar: Are HED meteorites from asteroid (4) Vesta? (G. Thangjam)

Meteorites are often used as ground truth for celestial bodies for which we have no samples. For the Moon the link between lunar samples and their origin has been proven. Among the achondrites, HED meteorites are one of the most abundant population. The hypothesis that HED meteorites have originated from Vesta has generally been accepted. However, recently this assumption has been questioned in the literature. Because of the relevance of this hypothesis for the analysis of remote sensed data from Vesta, we review the pros and cons of the ongoing debate in the scientific community. [mehr]

Planetary Group Seminar: The study of the global Heliosheath using Energetic Neutral Atom measurements obtained by the Cassini/INCA imager (K. Dialynas)

  • Datum: 25.11.2015
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Kostas Dialynas
  • University of Athens Department of Physics Section of Astrophysics, Astronomy and Mechanics GREECE
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Energetic Neutral Atoms (ENAs) result from Charge Exchange (CE) interactions between energetic, singly charged particles and cold neutral gases that co-exist in a plasma environment. Although the Ion and Neutral Camera (INCA), as part of the Magnetospheric Imaging Instrument (MIMI) suite on board Cassini, is designed to perform ENA measurements originating from the vicinity of Saturn (the Cassini s/c is in orbit around Saturn since 2004), imaging of the Heliosphere (in Hydrogen ENAs) lies well within the instrument capabilities. After 11 years of imaging the heliosphere with INCA, the ENA observations together with the Voyager-LECP in-situ measurements (in overlapping energy bands), have already revolutionized our notions about the formation and interactions of the global heliosphere, providing insights on the plasma processes at ~100 AU that were substantially at variance with previous theories and models. Although the question of how the HS responds to the variability of solar wind conditions and in what manner this response is connected to solar activity through the solar cycle has been addressed partly through modeling, the true manifestation of the HS (moreover in a global scale) to the solar activity have not been directly measured to date. Assessing any proposed interpretation of the HS requires the evaluation of the physical properties of the underlying source proton population in the broad context of the solar wind. Our current analysis on yearly averaged all sky ENA maps over the time period 2003-2014, show that ENA intensities decrease during the declining phase of SC23 by ~x3 from 2003 to 2011 but recover through 2014 (SC24). Similarly, V1,2 ion intensities also decrease and then recover through 2014. The similarity of time profiles of remotely sensed ENA and locally measured ions show that (a) ENA originate in the HS, and (b) the global HS responds promptly (within ~1-1.5 years) to outward-propagating solar wind changes throughout the SC. Further, recovery of the HS during SC24 proceeds asymmetrically from south to north in the general direction of the nose, which may be related to the non-symmetric evolution of solar coronal holes during SC recovery. [mehr]

MPS Seminar: Sunspot number series: how can we get out of the current mess? (I. Usoskin)

S3 Seminar: Spherical Couette Dynamos (A. Barik)

S3 Seminar: Non Local Heat Flux in Solar Flares (S. de Souza)

S3 Seminar: In-Orbit Calibration of the SO/PHI Instrument (K. Albert)

S3 Seminar: Constraining Differential Rotation in Sun-Like Stars (M.B. Nielsen)

Kometenfieber: Von Steilhängen und Staubfontänen. Die veränderlichen Landschaften des Rosetta-Kometen (C. Güttler)

Öffentliche Vortragsreihe

S3 Seminar: Sub-Grid Approach of Magnetic Reconnection (F. Widmer)

MPS Seminar: Eruptions driven by magnetic Flux Emergence in a Coronal Hole Environment (K. Galsgaard)

Magnetic flux emergence in to an existing coronal magnetic configuration represents one of the simplest ways to generate fast magnetic energy release processes. When the coronal magnetic field contains the favourable configurations different eruptions may take place forming simple jet like features or ejections of flux robes in the from a CMEs. This talk discusses the evolution of a magnetic flux emergence into a simple unipolar magnetic field using 3D non-ideal MHD modelling. The simple model gives rise to a much more complicated temporal evolution than expected. After a longer steady state jet phase the system reaches a phase where five eruptions take place. These are discussed in terms of the stressing of the system as it approaches the instability and the eruptions impact on the ambient magnetic field. [mehr]

Kometenfieber: Die Rosetta-Landemission aus Sicht der Wissenschaft (F. Goesmann)

Öffentliche Vortragsreihe
Here, we present a study of ionospheric convection at high latitudes that is based on satellite measurements of the Electron Drift Instrument (EDI) on-board the Cluster satellites, which were obtained over a full solar cycle (2001-2014). The mapped drift measurements are covering both hemispheres and a variety of different solar wind and interplanetary magnetic field (IMF) conditions. The large amount of data allows us to perform more detailed statistical studies. We show that flow patterns and polar cap potentials can differ between the two hemispheres on statistical average for a given IMF orientation. In particular, during southward directed IMF conditions, and thus enhanced energy input from the solar wind, we find that the southern polar cap has a higher cross polar cap potential. We also find persistent north-south asymmetries which cannot be explained by external drivers alone. Much of these asymmetries can probably be explained by significant differences in the strength and configuration of the geomagnetic field between the Northern and Southern Hemisphere. Since the ionosphere is magnetically connected to the magnetosphere, this difference will also be reflected in the magnetosphere in the form of different feedback from the two hemispheres. Consequently, local ionospheric conditions and the geomagnetic field configuration are important for north-south asymmetries in large regions of the geospace. The average convection is higher during periods with high solar activity. Although local ionospheric conditions may play a role, we mainly attribute this to higher geomagnetic activity due to enhanced solar wind - magnetosphere interactions. [mehr]

S3 Seminar: Forward and Inverse Problems in Asteroseismology (E. Bellinger)

S3 Seminar: Error Budget for Exoplanet Parameers from Asteroseismology (K. Rodenbeck)

S3 Seminar: Galactic Cosmic Rays Tracing in the Magnetosphere of Saturn (A. Kotova)

MPS Seminar: On-Board Computer System Architecture based on Commercial Off the Shelf components (F. Schön)

  • Datum: 28.01.2016
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Friedrich Schön
  • Frauenhofer-Institut für offene Kommunikationssysteme / System Quality Center, Berlin, Germany
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Patrick Bambach

S3 Seminar: Studying the Small Scale Magnetic Features in the Quiet Sun (F. Kahil)

S3 Seminar: Small Scale Chromospheric Fibrils Observed by Sunrise II (R. Gafeira)

MPS Seminar: Solar flares, current sheets, and finite-time singularities in Hall MHD (Y. Litvinenko)

  • Datum: 04.02.2016
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Yuri Litvinenko
  • Department of Mathematics, University of Waikato, New Zealand
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: -

MPS Seminar: Global Programmes in Astronomy Education and Public Outreach (P. Russo)

MPS Seminar: "Wave phenomena in sunspots" (J. Löhner-Böttcher)

Planetary Group Seminar: Water and ices in protoplanetary disks - links to the Solar System (I. Kamp)

S3 Seminar: The Fast Solar Polarimeter Prototype (F. Iglesias)

MPS Seminar: Modelling solar spectral irradiance with a Monte Carlo simulation of active region decay (C. Bolduc)

Kometenfieber: Rosettas Navigation am Kometen 67P/Churyumov-Gerasimenko: vom Anflug bis zur Landung (F. Budnik)

Öffentliche Vortragsreihe

MPS Seminar: Imaging the Earth from sedimentary basins to the deep mantle (A. Fichtner)

Planetary Group Seminar: Constraints on the solar system origin from Galileo, Cassini and Rosetta missions (O. Mousis)

  • Datum: 22.02.2016
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Prof. Olivier Mousis
  • Laboratoire d'Astrophysique de Marseille, Aix-Marseille Université, Institut Universitaire de France
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall

Planetary Group Seminar: Chemistry at the dawn of star formation and links to our Solar System (P. Caselli)

  • Datum: 24.02.2016
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Paola Caselli
  • Max Planck Institute for Extraterrestrial Physics, Garching
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall

Kometenfieber: Kometen und das frühe Sonnensystem (H. Böhnhardt)

Öffentliche Vortragsreihe

MPS Seminar: Looking Back by Looking Up: (Exo)planets and the Earliest History of Earth and Life (E. Gaidos)

Rosetta Seminar: Comparative study of icy patches on comet nuclei (N. Oklay)

MPS Seminar: Stellarators, fusion energy, and the Wendelstein 7-X experiment (P. Helander)

The Princeton astrophysicist Lyman Spitzer famously figured out how a magnetic field can be used to confine a fully ionised plasma in steady state. His solution, the so-called stellarator, involves a counter-intuitive twisting of the field without employing an electric current. Six decades later, Spitzer’s idea is put to a billion-euro test in the Wendelstein 7-X experiment of the Max Planck Society. This talk will describe some basic physics and mathematics underpinning stellarators, including the use of “hidden symmetries” to improve plasma confinement. An overview will also be given of Wendelstein 7-X, which after a decade of construction started operation in December 2015 and has already produced plasmas with electron temperatures exceeding 100 MK. If successful, it should produce steady-state plasmas under conditions suitable for extrapolation to a fusion reactor. [mehr]

Public Talk: ESA, die europäische NASA? (J.-D. Wörner)

Planetary Group Seminar: On the characterization of exoplanets with optical phase curves (A. García Muñoz)

MPS Seminar: Einstein for everyone: a common sense approach (N. Dadhich)

Planetary Group Seminar: Debris disks: Comets, asteroids, and dust around stars (A. Krivov)

  • Datum: 10.05.2016
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Alexander Krivov
  • Astrophysical Institute and University Observatory Friedrich Schiller University Jena
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall

Planetary Group Seminar: The chemical heritage of protoplanetary disks (C. Walsh)

Solar Group Seminar: Active region emergence: passive or active? (H. Schunker)

Solar Group Seminar: Coronal abundances by remote sensing: numerical experiments (H. Peter)

MPS Seminar: Stellar Evidence of a Transitional Sun (T. Metcalfe)

Rosetta Seminar: 67P Microscopic particle morphology (S. Merouane)

Rosetta Seminar: 67P Sublimation of dust grains (A. Giquel)

Rosetta Seminar: Alkali metals in 67P dust particles (O. Stenzel)

MPS Seminar: The hydrogen ionization front/stellar photosphereinteraction in Cepheids and RR Lyraes (S. Kanbur)

Solar Group Seminar: Response functions and node-based inversion for NLTE lines (I. Milic)

Rosetta Seminar: Philae Dust Measurements at 67P (H. Krüger)

Rosetta Seminar: 67P Volatiles as seen by ROSINA (U. Mall)

Rosetta Seminar: The Electric Charging of Nanoparticles AroundSolar-Type Stars (H. Kimura)

Solar Group Seminar: The Sun’s Radiant Energy - Measurements, Models,Mismatches, and Merging (G. Kopp)

Solar Group Seminar: In search of coronal loop footpoints (P. Chitta)

MPS Seminar: Solar Cycle Prediction Using a Surface FluxTransport Model (P. Bhowmik)

MPS Seminar: Flux Transport Dynamo Models: Understanding theSolar Magnetic Field generation process (G. Hazra)

The solar cycle is the magnetic cycle of the Sun. Inorder to understand the solar cycle and its properties, we need to understandhow the Sun is generating its own magnetic fields and organizing them. The FluxTransport Dynamo model is the most successful model to understand the solarmagnetic field generation process. But it has some inherent limitations. Inmost of the dynamo models, a single cell meridional circulation is used butthere is some recent observational evidence that the meridional circulation ofthe Sun may not have a single cell structure rather it might have a double cellor multi-cell structure. I shall discuss that the new observations are notimposing any serious threat and our model works perfectly fine. Many processesin this models are inherently 3D. In 2D we can model them very crudely by usingsome simple parametric form. So I shall explain the next generation 3D Flux TransportDynamo model which will be more realistic. The build up of solar polar fieldsusing this model will also be discussed. Apart from that I shall discuss thathow inclusion of observed high resolution non-axisymmetric convective flows inour model from SDO Dopplergram data affects the behaviour of theBabcock-Leighton process and helps us to put a better constraint on the surfacediffusivity. [mehr]

MPS Seminar: Information Transfer - from the Solar System to Exoplanets (L. Kaltenegger)

MPS Seminar: Effects of Coronal Eruptions Observed in the Chromosphere (M. Kirk)

S3 Seminar: Reconstructions of Solar Irradiance on the Millennial Timescale (C. J.Wu)

MPS Seminar: Introduction of NICT space weather researchactivities (M. Ishii)

  • Datum: 14.11.2016
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Mamoru Ishii
  • National Institute of Information and Communications Technology (NICT), Japan
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Hardi Peter

MPS Seminar: The VO And Why It Matters To You (M. Demleitner)

MPS Seminar: Why does the solar wind turn the wrong way, sometimes? (A. Otto)

MPS Seminar: High-precision spectroscopy and fundamental parameters of stars (M. Bergemann)

MPS Seminar: Observing stellar dynamos in action (T. Hackman)

MPS Seminar: Vortex flows and magnetic fields in the quiet Sun (I. Requerey)

Solar Group Seminar: tba (A. Künstler)

Solar Group Seminar: How investigating shear-driven turbulence helps to understand stellar interiors (V. Witzke)

MPS Seminar: Solar Limb Oscillations as Rotation Tracers and the Near Surface Shear (J. Kuhn)

  • Datum: 05.01.2017
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Jeff Kuhn
  • Institute for Astronomy, University of Hawaii, Maui, Hawaii, USA
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Aaron Birch
The HMI limb data pipeline is creating new information about the outer few hundred km of the solar atmosphere. The high signal to noise limb displacement and brightness oscillation data have yielded some surprising results. One of these is evidence of the largest rotation shear in the sun in the photosphere. This radial gradient is evidence of a stress that seems only possible from the radiated photon angular momentum. This seminar describes the limb oscillation data and the physical arguments that support a "photon brake" acting in the solar photosphere. [mehr]

MPS Seminar: Exploring the Diversity of Planetary Magnetospheres (E. Bunce)

MPS Seminar: Space Missions and Future Challenges (H. Dittus)

Numerous planetary bodies contain internal liquid layers in the form of either partially molten iron cores, buried water oceans or primitive magma oceans. Convection in these layers is usually driven by the combination of two buoyancy sources: a thermal source directly related to the planet’s secular cooling, the release of latent heat and possibly radioactive decay, and a compositional source due to some process of cristallisation or fusion, for example the growth of a solid inner core which releases light elements into the liquid outer core, or the melting/freezing of an ice layer which locally enriches or depletes the adjacent water ocean in salts. The dynamics of fusion/crystallization being dependent on the heat flux distribution, the thermochemical boundary conditions are locally coupled at a melting/crystallizing boundary which may affect the convection in various ways, particularly if heterogeneous conditions are imposed at one boundary. In addition, the thermal and compositional molecular diffusivities usually differ by at least 2 orders of magnitude. This can produce significant differences in the convective dynamics compared to pure thermal or compositional convection due to the potential occurence of double-diffusive phenomena. Traditionally, temperature and composition have been combined into one single variable called codensity under the assumption that turbulence mixes all physical properties at an "eddy-diffusion" rate. This description does not allow for a proper treatment of the coupling of the thermochemical boundary conditions and is probably incorrect inside stably stratified layers in which turbulence is diminished and double-diffusive phenomena can be expected. Temperature and composition should therefore be treated separately in simulations, but the weak diffusivity of the compositional field is technically difficult to handle in current geodynamo codes and requires the use of a semi-Lagrangian description to minimize numerical diffusion. During my PhD, I implemented and tested a semi-Lagrangian ”particle-in-cell” method into a geodynamo code (PARODY, E. Dormy, J. Aubert) to properly describe the compositional field. In this seminar, I will describe the general principles of this method and will discuss its advantages compared to classical field descriptions. I will then show first applications of this new tool to the formation of a chemically stratified layer below the CMB, and to geodynamo simulations including the coupling of the thermochemical boundary conditions. [mehr]

Planetary Group Seminar: Strata and envelopes of comet 67P (M. Massironi)

  • Datum: 25.01.2017
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Matteo Massironi
  • Dipartimento di Geoscienze, Universita' degli Studi di Padova, Italy
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Since August 2014, the OSIRIS cameras provided the first detailed images of the bilobate nucleus of 67P/Churyumov-Gerasimenko comet, and the extremely variegated geomorphology of its surface became immediately clear. Most of the morphological features have been subsequently attributed to evolving processes dominated by sublimation and thermal fatigue. Erosional processes have indeed shaped the nucleus exposing terraces, persistent steep cliffs and continuous and parallel linear features. Hence, the resulting morphology appears to be structurally controlled by a primary stratification. A 3D geological model, constrained by strata attitudes and equipotential surfaces of the gravity fields of the two lobes considered separately, can easily explain complex surface morphologies such as cuestas, mesas, series of stair-case terraces and persistent cliffs and provides important clues on the nucleus interior structure confirming that its bilobate shape is most probably the result of a gentle merging of two independent objects characterized by a primordial onion-like inner structure. This geological interpretation would have far-reaching consequences on how comets may have formed and evolved. [mehr]

MPS Seminar: How to form a millisecond magnetar ? Magnetic field amplification in a proto-neutron star (J. Guilet)

Planetary Group Seminar: Raumfahrttechnik an der Technischen Universität Berlin (K. Brieß)

Mit 11 erfolgreich gestarteten Satelliten ist die TU Berlin unter den Universitäten mit eigenen Satelliten weltweit führend. 7 Satelliten der TUBSAT-Familie und 4 Cubesats wurden bereits gebaut. Weitere 6 Nanosatelliten sind gegenwärtig in der Entwicklung. 2017 startet der Nanosatellit Technosat als Technologie-Demonstrator. Satelliten sind Bestandteil des Forschungsprogramms des Fachgebiets Raumfahrttechnik, das sich in 4 Schwerpunkte gliedern lässt: 1. Miniaturisierung von Raumfahrtkomponenten, wie Reaktionsräder, Sender und Empfänger, Navigationstechnik, sowie Erforschung neuer Technologien wie fluiddynamische Aktuatoren und multifunktionale Komponentenintegration, 2. Miniaturisierung von ganzen Raumfahrtsystemen wie Satelliten, Rover, Höhenforschungsraketen und Bodenstationen, 3. Verteilte Raumfahrtsysteme wie Satelliten-Konstellationen, -Formationen und -Schwärme sowie modulare fraktionierte Satelliten, 4. Anwendung von Raumfahrtsystemen, wie Fernerkundungs-Datenfusion, Data Mining, weltraumgestützte Frühwarnsysteme und "Capacity building" für die Erdfernerkundung. Der Vortag stellt die Aktivitäten und Ergebnisse des Fachgebietes auf den genannten Forschungsfeldern vor sowie die enge Verbindung zwischen Forschung, Lehre und Praxis in der studentischen Ausbildung. [mehr]

Solar Group Seminar: Connecting Solar and Stellar Variabilities (A. Shapiro)

We give an overview of the Rosetta Plasma Consortium (RPC) instruments onboard Rosetta and outline a few results on cometary plasma characteristics. We discuss in more detail observations during the cometary outburst on 19 February 2016. [mehr]
The oxygen isotopic ratio 18O/16O has been measured in cometary gas for a wide variety of comets, but it has only been measured in cometary dust by Stardust. Most such measurements find a value of the ratio that is consistent with Vienna Standard Mean Ocean Water within errors. In this talk I will present the result of a measurement of the oxygen isotopic ratio in dust from Comet 67P/Churyumov-Gerasimenko with the COSIMA instrument aboard the Rosetta spacecraft. Measuring the 18O/16O ratio with COSIMA is challenging for a number of reasons, but it is possible with a reasonable degree of precision. [mehr]

MPS Seminar: Did Neanderthal meet Modern Human? The Sun and Radiocarbon will tell (S. Talamo)

Planetary Group Seminar: Laboratory experiments on comet formation and activity (B. Gundlach)

  • CANCELED!
  • Datum: 02.03.2017
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Bastian Gundlach
  • TU Braunschweig, Institut für Geophysik und extraterrestrische Physik
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
This presentation will be providing an overview on laboratory experiments conducted at the TU Braunschweig with the aim to study comet activity and planet formation. First, an overview on recent competing comet formation scenarios is given, followed by with a discussion on how laboratory experiments can help to understand the different formation processes better. The second half of this talk will be focusing on the question of how laboratory works can be utilized to help interpreting observational data, for example gathered by the Rosetta spacecraft, to learn about comet activity. This presentation will be ending with an outlook on planned experiments and with an invitation to discuss the importance of future laboratory experiments with the audience. [mehr]

MPS Seminar: Large eddy simulations of compressible MHD turbulence in space plasma (A. Petrosyan)

MPS Seminar: High-Resolution Observations of Emerging Flux Regions (S. J. Gonzales Manrique)

MPS Seminar: From the Sun's atmosphere to the Earth's magnetosphere: Simulations of magnetic reconnection and dissipation of currents (P.-A. Bourdin)

Cometary dust activity is usually explained by a gas drag force which lifts micrometer-sized dust particles from the nucleus' surface against the weak nucleus gravity. However, taking into account the additional cohesion forces among the dust grains then this idea becomes questionable. We present the status of a thermophysical model of dust activity and compare it with observations of the Rosetta mission to comet 67P/Churyumov-Gerasimenko. [mehr]

Solar Group Seminar: New insights on penumbra magneto-convection (N. Bello Gonzalez)

MPS Seminar: Weather on remote worlds: the atmospheric circulation of hot Jupiters (A. Showman)

MPS Seminar: Empirical modelling of planetary magnetospheres in response to solar wind dynamics using EOF analysis and multivariate linear regression (M. He)

  • Datum: 05.04.2017
  • Uhrzeit: 10:00 - 11:00
  • Vortragende(r): Maosheng He
  • Leibniz Institute of Atmospheric Physics, Kühlungsborn, Germany
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Markus Fränz
This talk introduces an empirical modelling approach. The approach synthesizes the EOF analysis and multivariable regression analysis flexibly. Different from predefined basis functions and parametric equations, EOFs are data-customized and do not require prior information. Tailored is the approach to different datasets, COSMIC RO observation and CHAMP, VEX and MESSENGER magnetic field datasets. The applications provide quantitative descriptions for the ionospheric F2-layer peak, the field-aligned currents at Earth, the induced magnetic field near Venus, and the response of Mercury’s cusp to solar wind variability, respectively. The model constructions and methodology, and the main scientific results are illustrated comparatively. [mehr]
From the angular positions of the glory features observed on the upper cloud deck of Venus in three VMC channels (at 0.365, 0.513, and 0.965 mkm), the dominating sizes of cloud particles and their refractive index have been retrieved, and their spatial (in latitude) and temporal (in local time) variations have been analyzed. For this, the phase profiles of brightness were compared to the singe-scattering phase functions of particles of different sizes. [mehr]

Solar Group Seminar: High resolution calculations of solar convection zone and dynamo using the reduced speed of sound technique (H. Hotta)

MPS Seminar: Radiative feedback and the formation of massive stars and star clusters (R.E. Pudritz)

  • Datum: 08.05.2017
  • Uhrzeit: 10:00 - 11:00
  • Vortragende(r): Ralph E. Pudritz
  • Dept. of Physics and Astronomy, and Origins Institute, McMaster University, Canada
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Rene Heller

Solar Group Seminar: Stellar convection models with Kramers-type opacity law (P. Käpylä)

Planetary Group Seminar: The MASCOT lander onboard the Hayabusa2 mission (T.M. Ho)

MASCOT is a small asteroid lander launched on December 3rd, 2014, aboard the Japanese Hayabusa2 asteroid sample-return mission towards the 980 m diameter C-type near-Earth asteroid (NEA) 162173 Ryugu. The lander was jointly developed by the German Aerospace Centre (DLR) and the Centre National d'Etudes Spatiales (CNES). It is equipped with a sensor suite consisting of four fully-fledged instruments: a spectrometer (MicrOmega, IAS Paris), a camera (CAM, DLR Berlin), a radiometer (MARA, DLR Berlin) and a magnetometer (MAG, TU Braunschweig) to investigate Ryugu's surface structure, mineralogical composition, physical properties, thermal behavior and magnetic effects. The MASCOT lander has a total weight of only ~10kg and a size of 30 cm x 30 cm x 20 cm, comparable to a shoebox. Next to the 4 science payloads it accommodates all subsystems to guarantee the survival during the four years cold cruise phase and an on-surface operation and data uplink of up to 2 asteroid days. Upon arrival in Summer 2018 at the target, Hayabusa2 will map NEA Ryugu for several months before it will release MASCOT at an altitude of approx. 100m to free fall on the asteroid's surface. Since MASCOT has no attitude control, it will reach the surface and undergo a certain bouncing phase before it will finally come to rest. A mobility system allows the lander to upright into the correct measurement attitude and to relocate across the asteroids surface after the completion of its first science cycle. The system design, science instruments, and operational concept of MASCOT will be presented, with sidenotes on the development of the mission and its integration with Hayabusa2. [mehr]

Planetary Group Seminar: A Multi-instrument Study of a Cometary Outburst (J. Agarwal)

Abstract: On 2016 July 3, when comet 67P was already at 3.32 AU from the sun outbound from perihelion, several instruments on board Rosetta witnessed a small outburst of activity from a point on the surface emerging from the night's shadow. The dust plume above the surface was observed by OSIRIS and Alice, and the ejected material was detected in situ by COSIMA, GIADA, ROSINA, and the Startracker camera. This talk presents a summary and synthesis of the measurements, and discusses their implications for the properties of the ejected material and the process leading to this event. [mehr]

MPS Seminar: What Magnetic Structures Harbor Coronal Loop Plasmas? (G.-S. Choe)

Vortrag für Erwachsene und Kinder ab 10 Jahren [mehr]

Planetary Group Seminar: Radiation Belt Modeling and Forecasts: Limitations, Challenges and Future Needs (R. Friedel)

  • Datum: 30.05.2017
  • Uhrzeit: 15:00 - 16:00
  • Vortragende(r): Reiner Friedel
  • Center for Space and Earth Science (CSES) Los Alamos National Laboratory
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
In the scientific community, the focus of space research and model development is on understanding the underlying physics and system science of the environment in question. This often leads to a good understanding of the system, while at the same time the models in question are incapable of predicting or modeling any actual state of the system with any accuracy. Using current, state-of the art diffusion codes for the Earth’s radiation belt I will argue that our main limitation no longer lies in the models themselves but rather in the specification of their boundary conditions and other required inputs. I will further argue that in Space Weather modeling and prediction we are neither committing sufficient resources to providing these inputs, nor are we performing the required research that can effectively provide these inputs for either now-casting or forecasting needs into the future. [mehr]
Seit ihrer Entdeckung durch Galileo Galilei im Jahr 1610 sind wir von Saturn und seinen majestätischen Ringen fasziniert. Jedoch sind Ringe nicht das Alleinstellungsmerkmal dieses Planeten. Nein, alle vier Riesenplaneten unseres Sonnensystems zieren filigrane Ringe aus Eis und Staub. Aber nicht nur die Schönheit dieser „kleinsten“ kosmischen Scheiben erweckte das Interesse der Wissenschaftler, sondern sie sind exemplarisch für ihre „großen kosmischen Geschwister“: z.B. Akkretionsscheiben um kompakte Sterne, präplanetare Gas-Staubscheiben um junge Sterne (die „Kinderstuben“ von Planeten) oder gar die gigantischen Galaxienscheiben. Viele Prozesse, die die Physik planetarer Ringe bestimmen, laufen - wenngleich auf viel größeren Zeit- u. Längenskalen - auch in diesen zeitlich und räumlich weit entfernten kosmischen Scheiben ab. Von unschätzbaren Vorteil für uns ist aber, dass wir planetare Ringe mit Raumsonden in situ über dynamisch relevante Zeitskalen (Orbitperioden ~10 h) studieren und so mehr über die Physik aller kosmischen Scheiben lernen können. Dichte planetare Ringe sind granulare Gase im All - hauptsächlich bestehend aus Eisklumpen von Faust- bis hin zu Villagröße, die häufig (ca. 10-20 mal) pro Orbit inelastisch miteinander kollidieren. Sie sind die flachsten Strukturen im Universum mit einem Aspektverhältnis von 1 zu mehreren Millionen; d.h. bei einer vertikalen Ausdehnung (Dicke) von < 10 m erstrecken sie sich Hunderttausende km in lateraler Richtung. Des Weiteren zeichnen sie sich durch eine komplexe Dynamik aus, die u. a. zur Ausbildung von (sog. dissipativen) Strukturen führt: „Rillen", Wellen verschiedenen Typs und z.B. auch so-genannte „Propeller" bilden sich in diesen, von gravitativen Störungen getriebenen Nichtgleichgewichtssystemen. Moderne Raummissionen, wie gegenwärtig die Cassini-Raumsonde am Saturn, entlocken den Ringsystemen ihre Geheimnisse und stellen somit theoretische Vorhersagen auf den Prüfstand. Am Beispiel der von wolkenkratzer-großen Moonlets verursachten Propeller-Strukturen und deren Bedeutung für die Entstehung planetarer Ringe als auch der von Planeten allgemein, möchte ich das aktuelle Spannungsfeld zwischen theoretischen Vorhersagen und Beobachtungen der Cassini-Raumsonde etwas näher vorstellen. [mehr]

S3 Seminar: Image pre-processing pipeline for the space-borne spectropolarimeter PHI (K. Albert)

Planetary Group Seminar: Laboratory experiments on comet formation and activity (B. Gundlach)

  • Datum: 14.06.2017
  • Uhrzeit: 15:00 - 16:00
  • Vortragende(r): Bastian Gundlach
  • TU Braunschweig, Institut für Geophysik und extraterrestrische Physik
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
This presentation will be providing an overview on laboratory experiments conducted at the TU Braunschweig with the aim to study comet activity and planet formation. First, an overview on recent competing comet formation scenarios is given, followed by with a discussion on how laboratory experiments can help to understand the different formation processes better. The second half of this talk will be focusing on the question of how laboratory works can be utilized to help interpreting observational data, for example gathered by the Rosetta spacecraft, to learn about comet activity. This presentation will be ending with an outlook on planned experiments and with an invitation to discuss the importance of future laboratory experiments with the audience. [mehr]

MPS Seminar: Investigating the motion patterns of magnetic structures in active regions (J.C. Santos)

Planetary Group Seminar: Chlorine isotope constraints on volatility of the Moon (Z. Sharp)

  • Datum: 21.06.2017
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Zachary Sharp
  • UNM Earth and Planetary Sciences Department, Center for stable Isotope, Albuquerque, NM
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Chlorine and hydrogen isotope ratios of lunar materials are different from all other solar system materials measured to date. The isotopic constraints place conditions on the formation and volatility of the Moon. [mehr]

MPS Seminar: Realistic numerical simulations of convective overshooting in a DA white dwarf (F. Kupka)

MPS Seminar: Remote In-Situ Solar Sensing - A Year at the MPS (G. Kopp)

MPS Seminar: Exploring a new effect in large-scale galactic dynamos (L. Chamandy)

MPS Seminar: Applications of the Fluctuation-Dissipation Theorem to Space Plasmas (J. Araneda)

Seit sich die Raumsonde Cassini in einem Orbit um Saturn befindet, ist dessen bemerkenswerter Eismond Enceladus in den Fokus der Wissenschaft gerückt. 2005 entdeckten die Instrumente der Sonde gewaltige Fontänen aus Eispartikeln und Gas. Diese schießen aus stark erwärmten Öffnungen am Südpol des Mondes hunderte Kilometer in die Höhe. Ein Ozean, der sich unter dem -200°C kalten Eispanzer verbirgt, erwies sich als Quelle dieser „Cryo-Vulkane“. Inzwischen geht man davon aus, dass es sogar heiße Gebiete am Grund des Ozeans gibt, ähnlich den Hydrothermalschloten am Grunde der irdischen Ozeane. In der kurzen Liste der Himmelskörper in unserem Sonnensystem, auf denen man Leben finden könnte, belegt Enceladus seit diesen Entdeckungen einen Spitzenplatz. [mehr]

MPS Seminar: Interferometry of Solar Features with MAST: Preliminary Experiments (P. Venkatakrishnan)

MPS Seminar: Laminar and Turbulent Dynamos in chiral MHD (I. Rogachevskii)

MPS Seminar: Electric Currents in Emerging Flux Regions: Confrontation of Observations with Simulations (P. Venkatakrishnan)

Planetary Group Seminar: Experimental and numerical analysis of MHD effects in weakely ionized space relevant plasmas (G. Herdrich)

  • Datum: 16.08.2017
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Georg Herdrich
  • Universität Stuttgart , Institut für Raumfahrtsysteme
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Georg Herdrich is head of the Plasma Wind Tunnels and Electric Propulsion department of the Institute of Space Systems (IRS) at the university of Stuttgart. The department is specialized on electric propulsion systems, plasma measurement systems and test benches for reentry simulations as well as test branches for Interial electrostatic confinement devices for small electron and ion jets. In his talk he will give an overview of the IRS activities, with a focus on the experimental and numerical work on MHD effects in weakly ionized plasmas, which i.a. present on the lunar surface. [mehr]

MPS Seminar: Turbulent helicity and the effective momentum transport (N. Yokoi)

Helicity density (hereafter helicity), representing local structural properties of turbulence, is known to play important roles in the global magnetic-field induction (dynamos). In this talk, special emphasis is put on the role of helicity in the momentum transport. In addition to the usual eddy viscosity (represented by the turbulent energy), in the presence of breaking symmetry, a finite turbulent helicity effect enters the Reynolds stress. Recent developments on this line of studies are reported, which include the analysis of the stress equation, subgrid-scale (SGS) modelling. A possible application of this effect to the angular-momentum transport in the solar convection zone, as well as the extension to the magnetohydrodynamic (MHD) case, will be discussed. [mehr]

Planetary Group Seminar: Polarization Spetra of Planet Earth (M. Sterzik)

Polarimetry is routinely used as a diagnostic tool to characterize surfaces of solar system bodies, and polarization measurements of starlight reflected by exoplanets are becoming a powerful tool to study atmospheres and surfaces of other worlds. If extra-terrestial life has similar signatures as life as we know, then astronomical observations of planet Earth represent a prime benchmark case to probe biomarkers on other planets. In fact, linear polarization spectra of Earthshine (the sunlight that has been first reflected by Earth and then reflected back to Earth by the Moon) allows us to detect the presence of oxygen, ozone, and clouds in the atmosphere of our planet. Surface properties such as fractional contributions of continents and ocean, as well as vegetated areas can be inferred. Earthshine observations provide strong observational constraints on model predictions for Earth-type exoplanets. In this talk, we will compare observed polarization spectra with detailed simulations of Earthshine based on atmosphere models, and will discuss their applications to the search for life indicators in exoplanets. [mehr]

MPS Seminar: Fine-structures dynamics in sunspots: jets, dots, and the like (T. Samanta)

Planetary Group Seminar: Light scattering by large particles: Size does matter (Y. Grynko)

  • Datum: 11.09.2017
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Yevgen Grynko
  • Department of Theoretical Electrical Engineering, University of Paderborn
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
A numerical solution of the problem of light scattering by particles and particulate media becomes difficult if the particle size is much larger than the wavelength of the incident light. Accurate methods require huge hardware resources in this case. However, one can apply the geometric optics (GO) approximation. I will discuss such a GO model, its application and the prospectives of the rigorous wave-optics modelling. [mehr]

MPS Seminar: An observational study on the generation and propagation of intensity disturbances in solar polar coronal holes (L. Xia)

In this talk we will focus on diagnostic potential of the spectral region around D lines of Sodium. We will first outline our approach to non-lte inversions, and present a method for computation of response functions in non-local thermodynamic equilibrium. We will then discuss the sensitivity of Sodium D lines to the atmospheric parameters and present some example inversions of that spectral region. [mehr]

MPS Seminar: On the Origin of Life, Darwin`s Warm Little Pond revisited and implications for the search for life in the solar system (M. J. van Kranendonk)

  • Datum: 28.09.2017
  • Uhrzeit: 14:00 - 15:00
  • Vortragende(r): Martin van Kranendonk
  • Australian Centre for Astrobiology, University of New South Wales, Sydney, Australia
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
Darwin first postulated - 145 years ago - that life might have originated in “…some warm little pond with all sorts of ammonia and phosphoric salts, light, heat, electricity, etc. present, that a protein compound was chemically formed, ready to undergo still more complex changes…”. However, the 1970’s discovery of deep sea black smokers and their rich vent fauna, together with evidence from the mitochondrial tree of life, led to the currently prevailing view that life got started at deep sea vents. But it turns out that the energy required for polymerisation of organic molecules from simple amino acids comes from expelling a water molecule. In addition, the cytoplasm of cells from all three branches of life have K+/Na+ ratios more aligned with fresh water than seawater, and that certain key elements (B, Zn, Mn) required as catalysts for polymerisation are hard to concentrate in the uniform marine reservoir. Thus, it turns out that the oceans, or any permanently wet environment, are not suitable for prebiotic chemistry and thus a land-based environment undergoing wet-dry cycles is required for an Origin of Life setting. But what kind of environment? Previous authors have suggested a desert with seasonal rain, or a river flowing over komatiitic crust as possible sites for the Origin of Life. But these cold-water environments lack the capacity for compositional complexity and highly reactive interfaces. Recent discoveries from an ancient analogue site in Western Australia’s Pilbara region provide support for an Origin of Life in terrestrial hot springs. The 3.48 Ga Dresser Formation is well known as hosting some of Earth’s oldest convincing evidence of life (stromatolites, fractionated stable isotopes, and putative microbial remains), all within an active volcanic caldera characterised by voluminous hydrothermal fluid circulation. Previously, the depositional environment was considered as shallow marine, but the recent discovery of geyserite and other siliceous sinter deposits containing biosignatures and spatially closely associated with stromatolites, point to a thriving terrestrial hot spring setting with wet-dry cycles. A parallel, key, discovery is of concentrations of the critical elements required for prebiotic chemistry (B, Zn, and Mn), which arise from hot water-rock interactions. These discoveries are leading to a developing model for the Origin of Life in terrestrial hot spring fields, and have implications for Astrobiology and the search for life elsewhere in the Solar System. On Mars, we advocate for the Columbia Hills site that has known hotspring deposits identified from a previous rover mission. Further afield, advocates for exploration of the icy water moons of Saturn and Jupiter face the problem of a permanently wet environment that appears not to be favourable for life to develop. [mehr]

Planetary Group Seminar: Soft Protons in the Magnetosphere focused by X-ray Telescopes (F. Gastadello)

One of the major and unfortunately unforeseen sources of background for the current generation of X-ray telescopes, in particular the ESA X-ray satellite XMM-Newton, is due to soft (few tens-hundreds of keV) protons concentrated by the X-ray mirrors. The observing time lost is 40% in the case of XMM, affecting all the major broad science goals of this observatory, ranging from cosmology to astrophysics of neutron stars and black holes. The soft proton background can impact dramatically future large X-ray missions such as the ESA planned Athena mission. We will review the still poor understanding of the physical process at work and the connection with the magnetospheric population and acceleration sites originating the phenomenon. [mehr]

Planetary Group Seminar: Biomineralisation in complex animals as a time-travelling tool (D. J. Jackson)

  • Datum: 25.10.2017
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): David Burgess
  • Courant Research Centre Geobiology, Georg-August University of Goettingen
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
The evolutionary diversification of complex animal life on the planet earth was greatly supported by the wide-spread adoption of various biomineralising strategies. The so called ‘Cambrian Explosion’ (543 million years ago) records this rapid diversification of biomineralised forms in the fossil record. Study of the genetic and molecular biomineralising tools employed by various extant animal lineages can therefore provide a better understanding of how complex animal life first diversified. [mehr]

MPS Seminar: Reconnection and shock wave acceleration in astrophysical plasmas (T. Hoshino)

Planetary Group Seminar: Radiation Belts of the Giant Planets (P. Kollmann)

A fundamental property that a planet can have is if it is encompassed by radiation belts of highly energetic electrons and ions approaching light speed. The radiation belts of Jupiter and Saturn differ from Earth’s Van Allen belts not only in their extent and intensity but also in the physical processes governing them. We will explain the physics of giant planet radiation belts based on data from space missions as Juno and Cassini, and show examples of recent and ongoing studies. [mehr]
At the interface between the Sun's surface and million-degree outer atmosphere or corona lies the chromosphere. At 10,000K it is much cooler than the corona, but also many orders of magnitude denser. The chromosphere processes all magneto-convective energy that drives the heating of the million-degree outer atmosphere or corona, and requires a heating rate that is at least as large as that required for the corona. Yet many questions remain about what drives the chromospheric dynamics and energetics and how these are connected to the transition region and corona. The Interface Region Imaging Spectrograph (IRIS) is a NASA small explorer satellite that was launched in 2013 to study how the Sun's magneto-convection powers the low solar atmosphere. I will review recent results from IRIS in which observations and models are compared to study the role of small-scale magnetic fields in the generation of violent jets and how these jets feed plasma into the transition region and hot corona. [mehr]

Planetary Group Seminar: Halogen-bearing in the coma of comet 67P/Churyumov-Gerasimenko (F. Dhooghe)

  • Datum: 06.12.2017
  • Uhrzeit: 11:00 - 12:00
  • Vortragende(r): Frederic Dhooghe
  • BIRA-IASB, Belgian Institute for Space Aeronomy, Brussels, Belgium
  • Ort: MPS
  • Raum: Auditorium
  • Gastgeber: Urs Mall
The double focusing mass spectrometer (DFMS) of theROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis)instrument on board Rosetta has enabled the discovery of a zoo ofneutral constituents in the coma of comet 67P/Churyumov-Gerasimenko.This talk will focus on halogen-bearing species in the coma andaddress their abundances, variability and isotopic composition. [mehr]
Surges are ubiquitous cool ejections in the solar atmosphere that often appear associated with other interesting phenomena such as UV bursts or coronal jets. Recent observations from the Interface Region Imaging Spectrograph show that surges, although traditionally related to chromospheric lines such as H I 6563 Å or Ca II 8542 Å, can exhibit enhanced emission in Si IV and, as a consequence, lead to spectral profiles that are brighter than for the average transition region. However, a theoretical explanation to understand that behaviour was missing. In this talk, we analyse the response of the transition region to surge phenomena. To that end, we carried out two 2.5D radiative-MHD numerical experiments using the Bifrost code and including the non-equilibrium ionisation of silicon and oxygen. In the experiments, a cool and dense surge is obtained as a consequence of magnetic flux emergence. We find that non-equilibrium is key to understand why surges show enhanced emissivity in transition region lines. Studying the properties of emitting surge plasma, we point out the important role of the optically thin radiative cooling and heat conduction for the non-equilibrium ionisation. Furthermore, through the calculation of synthetic spectra of O IV, we provide predictions for future observations. [mehr]

MPS Seminar: Exoplanets and Habitability (K. Heng)

Solar and Stellar Group Seminar: Latest news from the solar g modes (E. Fossat)

MPS Seminar: Sunspots and active regions: fine structure, coronal heating and explosions (S.K. Tiwari)

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