Institut für Theoretische Physik
Start / Aktuell
Oktober  2014
Mo
27.10.2014
MPS Cygnus + Draco
MPI für Sonnensystemforschung
11:00
Solar-Seminar

Thierry Dudok de Wit

The solar butterfly diagram: from a low-dimensional model to new proxies of solar activity (T. Dudok de Wit)



Mo
27.10.2014
MPS - Aquila + Bootes
MPI für Sonnensystemforschung
14:00
MPS-Seminar

Avijeet Prasad
IIA, Bangalore, India

Separable solutions of force-free spheres and applications to solar active regions



Kontakt: Hardi Peter
Mo
27.10.2014
Seminarraum A.04.101
Theoretische Physik
14:15
Quantenfeldtheorie (Forschungsseminar M.Phy.412)

Gruppe Covi-Rehren

Semester-Planung



Kontakt: K.-H. Rehren
Di
28.10.2014
MPS - Aquila + Bootes
MPI für Sonnensystemforschung
11:00
Solar-Seminar

Johann Hirzberger
MPS

The PHI instrument on Solar Orbiter



Di
28.10.2014
MPS Cygnus + Draco
MPI für Sonnensystemforschung
11:00
Planetary-Seminar

Wojciech J. Markiewicz
MPS

Morphology, dynamics and physical properties of the Venus upper clouds from imaging with Venus Monitoring Camera on Venus Express

The Venus Monitoring Camera (VMC) on Venus Express (VEX) spacecraft has been observing the upper cloud layer since April 2006. To date more than three hundred thousand images have been acquired. VEX has a highly elliptical orbit allowing for global as well as close up views with resolution down to 200 meter per pixel. The VMC is a CCD camera with four channels in the UV, visible and near IR, with centre wavelengths at 365, 513, 965 and 1010 nanometers respectively. The VMC UV wavelength corresponds to the spectral feature of a, so far unidentified, absorber. In particular this subset of the VMC data shows great variety of morphologies. On global scales these include equatorial belts, bright polar bands and polar caps. The observed small scale features change their appearance from mottled clouds and convective cells at low latitudes to streaky patterns at middle and high latitudes. Time sequences of global views have been used extensively to track clouds and hence to obtain wind speed vectors. 90 orbits were processed manually resulting in 50000 wind speed vectors. With a correlation algorithm we have to date obtained more than 400000 vectors. Many of the morphological features we see in UV channel are also visible in other wavelengths. As the VEX spacecraft comes closer to the planet we no longer monitor cloud motion and rather quickly fly over them. During this pericentre passage it is possible to make dayside mosaics of the clouds as well as night side mosaics of the surface. The pericentre passage allows for the highest resolution images. Some of the most interesting ones are found in the equatorial convective region. The scales of the cells go down to few tens of kilometers and are significantly smaller than observed previously. This may have implications for the thickness of the convective zone itself and hence provide clues for understanding the difficult problem of vertical transport of energy and momentum. In near polar regions, usually above 50º latitude, we see many waves. These are most likely gravity waves and are visible in all four VMC channels. By modeling phase dependence of brightness in the VMC data in all channels we can infer the physical properties of the upper clouds as well as the haze which in most cases lies above the clouds. In the seminar I will also discuss observations and analysis of the glory on the top of the clouds. These data are the first observations of a full glory outside of the Earth environment.

Kontakt: Urs Mall
Do
30.10.2014
Seminarraum Astrophysik (SR 17, F 05.104)
Astrophysik
14:15

I will present hydrodynamical simulations of the formation of galaxies starting from cosmological initial conditions at high redshift. In these simulations, a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae, and stellar winds has been used (Hopkins et al. 2011). Our final objects have structure and stellar populations consistent with observed galaxies. Results indicate that feedback from massive stars plays a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM), and the low efficiency of star formation. I will focus the last part of my talk on the properties of the dwarf galaxies halos in the FIRE sample and its comparison with observations.

Kontakt: Wolfram Schmidt
Do
30.10.2014
Sitzungssaal Mathematik
Theoretische Physik
15:15

Connes' Noncommutative Geometry has allowed to gain deeper insights into the geometrical foundations that underly General Relativity as well as the Standard Model of Particle Physics. A fascinating aspect of the theory is the close link between abstract mathematical concepts and experimentally measurable quantities.

The aim of my talk is to provide the basic mathematical notions of Noncommutative Geometry (spectral triples, generalised Dirac operators, spectral actions, etc.) and to give an overview of our current understanding of the Standard Model of Particle Physics. Furthermore I will show how the notions of Particle Physics (and General Relativity) can be formulated within the framework of Noncommutative Geometry, proedicting measurable physical quantities, for example the mass of the Higgs boson.

Kontakt: K.-H. Rehren
Do
30.10.2014
Astrophysik
19:00
Öffentliche Führung Astrophysik

Öffentliche Führung Astrophysik

Beobachtungsobjekte: Mond, Ringnebel, Kugelsternhaufen
Thema des Vortrags: Plasma Turbulenz - misst Du noch oder simulierst Du schon? (Grete)

Das Institut für Astrophysik bietet in unregelmäßigen Abständen öffentliche Führungen mit Beobachtungsmöglichkeit am 50-cm-Spiegelteleskop an. Während der Führungen werden die Forschungs- und Ausbildungseinrichtungen des Instituts vorgestellt und, bei klarem Himmel, eindrucksvolle Himmelsobjekte (z. B. Mond, Planeten, Gasnebel, Sternhaufen, Galaxien) im Fernrohr gezeigt. Die Führungen werden durch eine halbstündige Präsentation zu einem aktuellen Thema aus der astronomischen Forschung ergänzt.

Kontakt: Reinsch
Fr
31.10.2014
MPS Aquila + Bootes
MPI für Sonnensystemforschung
13:30
Rosetta-Seminar

Fred Goesmann
MPS

Last MS spectrum prior to crash?




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Last modified: Mon Mar 5 10:17:50 CET 2012