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PhD projects at the IMPRS
MPE Infrared-Astronomy
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The research of the MPE infrared group centers on near-infrared, far-infrared and millimeter, high resolution imaging and spectroscopy of the Galactic center, starburst galaxies and AGN, the dense interstellar medium in star-forming regions of our own Galaxy, and on extragalactic infrared surveys. We study the physical properties, dynamics, and evolution of high-z galaxies, and of galaxy mergers. Key results have been the unambiguous detection of the supermassive black hole in the center of our galaxy through stellar proper motions, the identification of star formation as the main power source of dusty ultraluminous galaxies by mid-infrared spectroscopy, and the first substantial survey of high redshift galaxy dynamics using integral field spectroscopy. These results are part of our pursuit of issues like existence and formation of black holes in galactic nuclei, nature and evolution of (ultra)luminous infrared galaxies at low and high redshift, gas dynamics and fuelling of AGN, and the properties of starburst galaxies.Within our own Galaxy, research focusses on the physical and chemical evolution of dense gas associated with protostars and protoplanetary disks, with special emphasis on the role of water.
These research activities are supported largely by a parallel program of innovative
infrared instrumentation development. Our near-infrared high resolution cameras at the NTT and VLT were crucial for the key results on the Galactic center, our Infrared Space Observatory short wavelength spectrometer SWS for the study of ultraluminous infrared galaxies. Diffraction limited observations with our new near infrared field imaging spectrometer (SINFONI, at the ESO VLT since 2003) as well as with NACO are now empowered by the laser guide star facility, for which we have just provided our powerful laser. A major next event will be the launch of the Herschel Space Obervatory hosting our far-infrared camera/spectrometer PACS. Projects under development include instrumentation for SOFIA, the Large Binocular Telescope (LBT), and for the VLT interferometry. In addition, we have regular access to the facilities at IRAM and ESO. Our approach is to tackle a few key science issues on a broad front with observations and novel instruments across the entire infrared to millimeter wavelength band. In many cases, we have aimed for a detailed physical understanding of a few representative sources, rather than a statistical approach. Often, our research is in an experimental physics group mode with a team and key project approach.
Research fields for which PhD projects are offered:
- Novel instrumentation concepts in high resolution astronomy by adaptive optics and interferometry
- Exploring galaxy evolution by high resolution observations of high redshift galaxies
- Herschel Space Observatory surveys and the nature of the cosmic infrared background
- The Black Hole in the center of our Galaxy and its surrounding stellar cluster - a laboratory for understanding black holes and strong gravity
- Black holes and star formation in nearby galaxies
- Herschel Space Observatory observations of water in star- and planet-forming regions within our Galaxy
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High resolution studies of galaxy evolution like the surprising detection of a massive rotating disk in the z=2.38 galaxy BzK-15504 are made possible by our active instrumentation program, for example the PARSEC laser at the ESO VLT.
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MPE X-ray Astronomy
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X-rays originate in the universe from regions under extreme conditions, from plasma with temperatures up to billions of degrees, and from the interactions of highly energetic electrons with magnetic and photon fields. Studying cosmic objects in X-rays gives insights in the physical processes, that often cannot be achieved observing in other wave bands.
The X-ray astronomy group at MPE, comprising about 80 members, has its major scientific emphasis in the study of the origin of hot gas in our galaxy, around nearby galaxies, the development of supernova remnants, the production mechanisms and the radiation transfer of X-rays observed from compact objects and from galaxies and galaxy clusters. Aditionally we deal with cosmological questions arising from the observation of galaxy clusters and active galactic nuclei. In recent years, we have been involved in the resolution of the X-ray background radiation into discrete sources, mainly active galactic nucleii at cosmological distances.
Access to observational data is gained largely through the development of X-ray instrumentation. In our Semiconductor Lab we develop highly specialized X-ray detectors, most recently the EPIC pn-CCD camera on XMM - Newton. We have long experience in the realization of X-ray telescopes, while whole satellite payloads are calibrated in our 130 m test facility PANTER. This engagement has enabled us to build and operate for over 8 years the ROSAT observatory, and collaborate actively in all major X-ray observatory missions, especially XMM-Newton and Chandra. Currently, the institute is preparing the eROSITA telescope for the Russian Spectrum-RG mission. After its launch in 2011 eROSITA will perform a new X-ray all-sky survey a factor of 10-30 deeper than ROSAT and HEAO1. Using optical, Infrared and radio data to better interpret the X-ray results has also stimulated working in a worldwide net of astronomy collaborations.
Research fields for which PhD projects are offered:
- Study of compact X-ray sources in galaxies
- Multiwavelength studies of supernova remnants, Pulsars and Neutron Stars
- High-Energy processes in active galactic nuclei
- Hot intergalactic gas in clusters of galaxies and galactic filaments
- Development of the eROSITA Survey
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The X-ray satellite ROSAT, which was developed and operated by MPE performed the first all-sky survey in the X-ray band with an imaging X-ray telescope. The image shows thediffuse X-ray sky as seen by ROSAT. More recent X-ray missions like XMM-Newton and Chandra largely gain from the results obtain with ROSAT. eROSITA will significantly expand the survey.
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MPE Gamma-ray Astronomy
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Gamma-rays are produced by the most energetic processes in the universe:
We study the acceleration of charged particles to relativistic energies, and the formation of new atomic nuclei in (mostly explosive) nucleosynthesis events.
Cosmic particle acceleration is observed in a wide range of objects, yet still mysterious: Plasma jets from active galaxies (with gamma-ray blazars as a subclass where the jet points towards us); gamma-ray bursts caused by transient accretion disks around a new-born black hole; pulsars as particle accelerators through the neutron star’s magnetosphere. Gamma-ray emission most directly reflects the conditions inside these sources. Also, propagation of these energetic charged particles in interstellar space causes diffuse Galactic gamma-ray emission; its synoptic view across many wavelength regimes including cosmic-ray data provides an integrated view of how high-energy processes shape the Galaxy.
Formation of new elements inside massive stars, in supernovae, and in novae is revealed through gamma-rays from radioactive trace elements created as by-products. With a range of half-lives from days to million years, their gamma-rays are unique messengers from the core of supernova explosions, but also reflect the evolution of supernova remnants from explosion to final dilution, and ejecta mixing with the interstellar-medium.
Unidentified sources of gamma-rays are puzzling, our study of their nature and physics across the entire electromagnetic spectrum may reveal new astrophysical processes.
With about 30 members, the gamma-ray group of MPE supports the INTEGRAL, FERMI/FERMI-GBM, OPTIMA, SWIFT and GROND projects with first-hand access to data and analysis software tools, and the development of a next-generation gamma-ray telescope. (For more details see webpage)
Research fields for which PhD projects are offered:
- the nature of supernova explosions, and nucleosynthesis in the Galaxy
- the nature of gamma-ray sources in the Galaxy
- prompt and afterglow emission of gamma-ray bursts
- high-time resolution photo-polarimetry of pulsars, CVs, and transients
- cosmological applications of gamma-ray burst afterglows
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The sky in gamma-rays emitted from radioactive decay of 26Al (decay half life ~700000 years)
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MPE Theory Group
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The theoretical group of the institute conducts analytical, numerical and observation - related interpretational research. It addresses topics that cover all experimental research areas of the MPE. The direct interaction of theoreticians, observers and experimenters provides an important synergetic boost for research.
The mutual interactions also stimulates new directions of research. Recently, the young field of research in "Complex Plasmas" was developed at MPE as a new laboratory activity, following the discovery of "plasma crystals".
For some of the activities microgravity is important, and these research conditions have been achieved by means of rocket and aircraft flights and by experiments on the International Space Station.
Research fields for which PhD projects are offered:
- Experimental and theoretical investigations of complex plasmas
- Interstellar and magnetospheric plasmas
- High-energy processes in Active Galactic Nuclei
- Clusters of galaxies and the large scale structure of the Universe
- Young stars and planet formation , extrasolar planets
- Advanced methods in data analysis and applications in astrophysics, plasma physics, medical research and engineering
For more details visit our homepage www.mpe.mpg.de/www_th/theory.html
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MPE Optical and Interpretative Astronomy &
USM Extragalactic Astronomy |
The USM-MPE extragalactic research group is a joint effort of the University Observatory of Munich (USM) and the Max-Planck Institute for Extraterrestical Physics. The group is located both at the USM (see `Extragalactic Astronomy') and at MPE ). Senior group members are Prof. Ralf Bender, Prof. O. Gerhard, Dr. U. Hopp, P.D. Dr. R.P. Saglia, Dr. S. Seitz.
The research of the group focusses on dark energy and dark matter in the Universe, on local and distant galaxies, and planets. The aims of our current science projects are:
- to constrain the nature of dark matter, by searching for MACHOS with pixellensing towards M31, and by analysing cluster and galaxy dark matter halo profiles with strong and weak lensing in combination with dynamical and photometric information for nearby galaxies;
- to derive constraints on the nature of dark energy, by measuring the power spectra of galaxies and clusters of galaxies at various redshifts, the number density of clusters as a function of mass and redshift, and the redshift dependence of the gravitational lens effect;
- to understand the structure and dynamics of local and distant galaxies, their stellar populations, their formation and evolution;
- to build a model of the Milky Way which can be used as a template for galaxy formation;
- to quantify the role of black holes and dark matter in galaxies;
- to search for extrasolar planets using the transit method in wide field surveys and understand their properties (mass, density, atmosphere).
We pursue these science questions with a combination of optical and near-infrared observations, theory, numerical modelling, and data interpretation. The group is one of the principal partners in the Pan-STARRS survey which images 3/4 of the sky with unprecedented depth. It is also an important partner in several large international collaborations (e.g., the NUKER team, the PN.S project).
The observational data necessary for our scientific programs come from running own telescope (Wendelstein), partnership in the Hobby-Eberly-Telescope and Pan-STARRS projects, from guaranteed time received for providing instruments to ESO ( FORS , SPIFFI , OmegaCAM , KMOS), and from participation in public surveys ( ). Last, not least we obtain time from applications to the ESO telescopes and the german-spanish Calar-Alto Observatory. In addition we use our Wendelstein observatory in the Alps for pixellensing and other monitoring projects. (The currently used 0.8m telescope will soon be replaced by a 2m-telescope with adequadate imaging and spectroscopic instrumentation).
The numerical modelling uses state-of-the-art numerical methods run on PC clusters. Some of these methods are developed or implemented within our group for specific projects. Recent examples are Schwarzschild's orbit superposition method used for measuring black hole masses, and the NMAGIC adaptive N-body code for modelling galaxy dynamics.
In addition, the USM-MPE extragalactic research group is designing and building imaging and spectroscopy instruments for 1-10m class telescopes, together with national and international partners. We built, e.g., the FORS instruments for the VLT, and LRS (Low Resolution Spectrograph) for the 10m Hobby-Eberly-Telescope in Texas (which we share with the Universities of Texas, Penn State University, Standford and Göttingen). We currently wait for our newly built 1-square degree imager OmegaCam to start operations on the 2.6m VLT-survey telescope (VST) in Chile. Right now we started the design of a multi-IFU-infrared spectrograph (KMOS@VLT) and a giant optical IFU spectrograph ((VIRUS@HET).
Finally, we also develop data reduction and analysis software. We are member of ASTROWISE, a european team (USM, Paris, Groeningen, Leiden and Naples) providing data analysis software for the OmegaCAM and any wide field data. This software is essential for all wide field imaging surveys carried out within the ESO community in the future. For the VIRUS project we are developing the pipeline for the automatic reduction of the integral field spectra.
We offer PhD projects within our group in any of the above science areas and in instrumentation as well.
Some examples:
- Imprints of Dark Energy in Galaxy Powerspectra using Pan-STARRS
- Weak lensing and photometric cluster search
- 3D-lensing
- Variability studies in the OmegaTrans Project
- Dynamical modelling of galaxies
- Stellar content and structure of the Milky Way
- New instruments
Our homepages provide detailed information on currently available PhD projects. See, e.g. the weblinks OPINAS and PhD projects.
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Difference image movie of a 30 x 30 arcsec2 area in the bulge of M31 from our WECAPP pixellensing project. Long period variables and other variable stars show up as varying black and white spots. Towards the end of the movie a microlens event is visible in the center of the field.
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| USM Computational Astrophysics |
| The research of the computational astrophysics group at the USM is focussed on dynamical processes in galaxies, related to galaxy formation and evolution, the evolution of the interstellar medium and star and planet formation. Using different numerical methods and codes, coupled with special hardware connected to local PC clusters for fast computations we explore the complex non-linear evolution of gas in galaxies and its condensation into dense molecular clouds and stars. We explore the collapse of protostellar clumps and cores, the formation of protostellar disks and their condensation into planets. On larger scales we investigate galaxy-galaxy interactions including dark matter, stars and gas and study the morphological transitions of galaxies and the origin of their spheroidal components.
Research fields for which PhD projects are offered:
- Origin of very old, massive elliptical galaxies.
- The cosmological angular momentum problem.
- The origin of turbulence in the interstellar medium.
- Formation of clumpy, turbulent molecular clouds.
- Formation of stellar clusters and disruption of molecular clouds.
- Origin and evolution of stellar disks around massive black holes
in the centers of galaxies.
- Evolution of protoplanetary disks and their condensation into
brown dwarfs and massive planets.
More infos are available at www.usm.uni-muenchen.de/CAST/
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| USM Stellar Astrophysics - Expanding Atmospheres of Hot Stars |
| Hot Stars cover sub-groups of objects in different parts of the HR diagram and at different evolutionary stages. The most important sub-groups are massive O/B Stars, Central Stars of Planetary Nebulae, and Supernovae. All these objects have in common that they are characterized by high radiation energy densities and expanding atmospheres. Due to these properties, the state of the outermost parts of these objects is characterized by non-equilibrium thermodynamics and radiation hydrodynamics.
The USM Hot Star group is experienced in the corresponding theory of stellar atmospheres, and in model simulations and the computation of realistic synthetic spectra for these astrophysically important objects.
Specific topics address the relevance of Hot Stars for current astronomical research:
- The present cosmological question of the reionization of the universe requires quantitative predictions about the influence of very massive, extremely metal-poor Population III stars on their galactic and intergalactic environment. The objective is to deduce the ionization efficiency of a Top-heavy IMF via realistic spectral energy distributions of these very massive stars.
- Due to the impact of massive stars on their environment the underlying physics for the spectral appearance of starburst galaxies are rooted in the atmospheric expansion of massive O stars which dominate the UV wavelength range in star-forming galaxies. Therefore, the UV-spectral features of massive O stars can be used as tracers of age and chemical composition of starburst galaxies even at high redshift
- Distant SNe Ia appear fainter than standard candles in an empty Friedmann model of the universe. This surprising result requires investigating the role of Supernovae of Type Ia as distance indicators with respect to diagnostic issues of their spectra
Research fields for which PhD projects are offered:
- Diagnostics of UV and optical spectra of O type stars
- Synthetic spectra of the x-ray range of O type stars
- Synthetic spectra for SN Ia at late phases
- IR-spectroscopy of massive stars
- Clumping in hot star winds - constraints from a multi-wavelength analysis
The main focus of the working group thus is to develop diagnostic techniques in order to extract the complete physical stellar information from the spectra at all wavelength ranges.
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Observations
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Theory
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Applications
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Diagnostics
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IR - Optical - UV - EUV - X-ray
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| More details about the USM Hot Star group and further information on the projects can be found here. |
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USM Plasma-Astrophysics
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The Plasma-Physic group at the USM is involved in the research of the macroscopic dynamics of astrophysical plasmas. 99% of the visible Universe is in the plasma state. Thus, the understanding of the dynamics of cosmic multi-particle systems under the influence of electromagnetic forces, is of outstanding importance.
Phenomena of special interest to our group are:
- a) high-energy particle acceleration processes in the context of (proto)-stellar flares, pulsars, extragalactic jets and cosmic rays,
- b) plasma heating in, e.g., (proto)stellar coronae, galactic high-velocity clouds and the interstellar medium,
- c) the generation, reconfiguration, filamentation and energy conversion of magnetic fields in (proto)galaxies, accretion disks, active galactic nuclei.
Our analytical and numerical investigations are carried out on the grounds of the (multi)fluid- as well as the kinetic plasma theory.
Research fields for which PhD projects are offered:
- TeV Emission from Active Galactic Nuclei
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In the Centaurus A x-ray jet high-energy particles are continuously accelerated on kpc length scales up to Lorentz factors of some 107.
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MPA Extragalactic Astrophysics and Cosmology
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The MPA Cosmology group is interested in the structure, evolution and material content of our Universe. Scientific topics under active study include:
The structure, formation and evolution of galaxies and of their central supermassive black holes; the phenomenology of star formation in galaxies, of active galactic nuclei and of galaxy interactions, and its relation to the astrophysics driving the evolution of the galaxy population.
Galaxy clusters, galaxy clustering and the large-scale structure of the universe. The morphology, quantitative characterisation and observational measurement of structure in the galaxy, dark matter and intergalactic gas distributions.
- The structure and formation history of the Milky Way
- The use of gravitational lensing to characterise the dark matter environments of galaxies and galaxy clusters and statistical properties of the cosmic mass distribution.
- The intergalactic medium, its evolution and structure, its chemical enrichment, its interaction with galaxies and AGN detecting and characterizing the reionization epoch.
- The microwave background radiation as a probe of the origin of structure, of the physics of the early universe, of the nature of Dark Matter and Dark Energy, of matter between us and the last scattering surface at z=1000, of cosmological parameter values.
- Using all of the above to test the current standard LCDM paradigm for the growth of cosmic structure, and to find tests for the nature of Dark matter and Dark Energy
Group members use a mixture of pure theory, numerical simulation, data interpretation, and direct observation to address these questions. The group is one of the principal nodes of the international Virgo Supercomputing Consortium which has carried out many of the largest cosmological simulations ever completed. It is a Partner in the Sloan Digital Sky Survey which has imaged a quarter of the sky in 5 photometric bands and obtained 1 million galaxy and quasar spectra. With the MPA High Energy group it is the German centre for the Planck mission which is currently mapping the microwave background radiation. It is building a remote station for the Low Frequency Array (LOFAR) telescope. Finally, we led the international consortium carrying out the ESO Distant Cluster Survey a Large Programme on the ESO VLT and NTT telescopes. The group can host PhD students in any (or a combination of) these areas.
Research fields for which PhD projects are offered:
- Phenomenology and evolution of the galaxy/AGN population
- Simulation of the formation and evolution of galaxies, galaxy clusters, large-scale structure and the intergalactic medium
- Gravitational lensing
- Structure, dynamics and evolution of the Milky Way
- Microwave background studies
- Constraining the nature of Dark Matter and Dark Energy
A thin slice through the dark matter distribution in part of the Millennium Simulation, one of the largest simulations of cosmic structure formation ever carried out. This simulation is used as a testbed to comparing models for galaxy/AGN evolution with data from few large-scale surveys, both nearby and at high redshift. For more information see http://www.mpa-garching.mpg.de/galform.
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A thin slice through the dark matter distribution in part of the Millennium Simulation, the largest simulation of cosmic structure formation ever carried out. This simulation is used as a testbed to comparing models for galaxy/AGN evolution with data from new large-scale surveys, both nearby and at high redshift. For more information see http://www.mpa-garching.mpg.de/galform.
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MPA High Energy Astrophysics
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The area of interests of the MPA High Energy Astrophysics group can be broadly outlined as physical processes and interaction of matter and radiation under extreme astrophysical conditions. The objects where these processes are investigated include the Universe as a whole, clusters of galaxies, supermassive black holes and jets in AGN, accreting black holes and neutron stars in X-ray binaries, Gamma-ray bursts and the Cosmic Microwave Background. Similarities in the underlying physical processes bind these diverse subjects together. A special focus of the work is accretion onto compact objects (black holes, neutron stars and white dwarfs). This includes theories for the hydrodynamics of the accretion process and the origin of the energetic radiation. Examples are detailed theories for the boundary layer around accreting neutron stars, and the theory of Comptonization and it's applications. In addition members of the group are closely involved with interpretation of the observational signatures of accreting black holes and neutron stars, the study of X-ray emission from the clusters of galaxies, relic radio sources, theories for the central engines of Gamma-ray Bursts, the evolution of binary stars, and the behavior of magnetic fields in a wide range of astrophysical environments. Likewise, this research group has interests in the study of the interaction of CMB photons with matter at different evolutionary epochs of our universe. These include the cosmological recombination, the end of the Dark Ages/beginning of reionization, and the late accelerated expansion phase seeded by a cosmological constant or any sort of Dark Energy. Particular emphasis is paid on the characterization of the CMB spectrum generated during recombination, the interaction of the CMB with the heavy elements synthesized by the first stars, and the secondary anisotropies introduced by newly ionized bubbles, galaxy groups and clusters during the ntermediate and late ages of our universe. The group can host PhD students in any (or a combination of) these areas.
One of the key elements of the group's approach is to complement the theoretical advancement of the field with state-of-the-art data analysis of the experimental data. The group is actively using the data from the RXTE, CHANDRA, XMM-Newton, INTEGRAL, Swift and WMAP/LAMBDA observatories. The group also provides scientific support for future missions that will lead to substantial progress in high resolution X-ray spectroscopy and microsecond timing. Further information can be found at http://www.mpa-garching.mpg.de/high_energy/
Research fields for which PhD projects are offered:
- Physical cosmology: CMB, interaction of matter and radiation during
recombination, reionization and the late stages of our universe
- Accretion onto black holes and neutron stars: theory and observations
- Jets in quasars and micro-quasars
- Elementary physical processes, including theory of Comptonisation
- Origin and growth of supermassive black holes
- Populations of accreting black holes and neutron stars in young and old galaxies
- X-ray emission from clusters of galaxies and cooling flows
- Models for central engines of Gamma-ray bursts
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| MPA Supernovae |
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The MPA Supernovae group is a world-leader in modelling the violent deaths of stars in the form of supernovae and studying how such explosions produce the chemical elements, generate gravitational waves or can be used as reliable cosmic distance indicators. Massive stars end their lives in core collapse supernovae when the star has run out of nuclear fuel in the interior. In some cases the explosion following the initial collapse can lead to particularly energetic hypernovae or gamma-ray bursts. Another type of supernovae occurs in binary systems involving white dwarfs, the compact remnants of less massive stars. These thermonuclear supernovae explosion can either be triggered by accretion of material from a companion star or during the merger of two white dwarfs. The MPA group specializes in performing realistic multi-dimensional hydrodynamical supercomputer simulations of the different types of supernovae and gamma-ray bursts, which takes into account detailed microphysics such as turbulent flame propagation, neutrino transfer, magnetic fields and special and general relativistic effects. The supernova models are also used to predict he emergent spectrum to compare with observations.
Most of the work within the group is theoretical/computational in nature but more recently the group has lead several observational programs aimed at understanding the physics of supernovae. The group has a long track-record of developing novel and sophisticated numerical methods to enable the extremely computing-intensive hydrodynamical simulations. The group has excellent access to powerful parallel supercomputers and is engaged in two long term Collaborative Research Centers of the German Science Foundation (DFG) on Gravitational Wave Astronomy and on Neutrinos and Other Weakly Interacting Particles in Physics, Astrophysics and Cosmology. It also actively participates in the Excellence cluster on Origin and Structure of the Universe involving MPA, MPE, MPP, ESO, LMU and TU.
Research fields for which PhD projects are offered::
- Explosion physics of thermonuclear supernovae
- Simulating gamma-ray bursts
- Neutrino transfer and core-collapse supernova
- Supernova nucleosynthesis
- Modelling and observations of supernova spectra
- Gravitational wave signature from supernova explosions
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Left: A snapshot from a 3D simulation of a core collaps supernova,which demonstrates the complex hydrodynamical velocity field and neutrino heating during the earliest phases of the collapse prior to the final explosion. Right: A simulation of a thermonuclear supernova (SNe type Ia), which shows the 3D structure of the thermonuclear burning front in blue incinerating the white dwarf.
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| MPA Stellar Astrophysics and Galactic Archeology |
| The MPA Stellar Astrophysics and Galactic Archeology (SAGA) group has a two-fold aim: understand the physics of stars and use stars as probes of the cosmos, be it to study the Big Bang, the history of the Milky Way or the origin of the elements. The research encompasses both sophisticated modelling with supercomputers and large-scale observations with the most powerful telescopes.
A common thread for much of the work is the study of the origin of the elements -- when, where and how the different chemical elements were produced in the Universe. Essentially all elements have been forged by nuclear reactions in the fiery interiors of stars and MPA has for decades been a world-leader in simulating stellar evolution and nucleosynthesis. More recently this work has focussed on understanding low- and intermediate mass stars and testing the models by means of helio- and asteroseismology. Another critical ingredient for this endeavour is how to decipher the light emitted by stars in terms of stellar properties such as masses, temperatures, ages and chemical compositions. The group has pioneered developing realistic 3D hydrodynamical simulations of stellar atmospheres and convection. Among other things this modelling has completely changed our understanding of how convection operates in stars as well as caused a dramatic revision of a fundamental astronomical yardstick, namely the solar chemical composition. We are currently extending this modelling to other types of stars, including brown dwarfs and extrasolar giant planets.
The stellar modelling within the group provides the basis for the work on the formation and evolution of galaxies, which is one of the main outstanding problems in astronomy today. By studying stars born at different locations and with varying ages in a galaxy it is possible to piece together its history, an approach dubbed Galactic Archeology. In particular the group is trying to disentangle the evolution of our own Milky Way Galaxy. Currently the main emphasis is to discover the oldest stars in the Galactic halo, to study the old but metal-rich Galactic bulge and to investigate the origin of the thick and thin disks. The group is an active partner in three massive Galactic surveys which will revolutionize the field in the coming
few years: Sloan Digital Sky Survey, LAMOST and Skymapper Southern Sky Survey. In addition, we are a frequent user of the VLT, Keck, Subaru and Gemini telescopes.
Research fields for which PhD projects are offered:
- First stars
- Atmospheres of brown dwarfs and extrasolar planets
- Tracing the evolutionary history of the Milky Way
- Physics of stellar convection
- Chemical compositions of stars
- Stellar evolution, mixing and nucleosynthesis
- Probing stellar interiors through asteroseismology
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A small but representative volume of the stellar atmosphere is simulated by computing the convective and radiative energy transport. The 3D geometry of the atmospheric structure and the velocity field and their time-evolution can thereby be calculated and used to predict the emergent stellar spectrum.
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ESO Astronomy
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The research activities at ESO focus on optical, infrared and millimeter wave astronomy using ground-based facilities at ESO observatories in Chile. One of the focal points of current research is the development and utilization of high-spatial resolution techniques such as adaptive optics or interferometry. The scientific expertise at ESO covers all major areas of observational astronomy. Research interests of ESO scientists range from the Solar system to studies of the solar neighborhood (extrasolar planets, evolved stars, star formation), interstellar medium, Galactic structure, local universe (Local Group and beyond) and cosmology (galaxy clusters, Gamma-ray bursts, dark matter, lensing).
Research fields for which PhD projects are offered:
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VLT/ISAAC near-infrared image of the Galactic giant HII region NGC 3603 with its central starburst cluster. Stars with masses between 0.1 and 120 solar masses formed simultaneously in the cluster.
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