Winter Term 2025/2026

Content

In this astrophysics lecture we cover the theoretical concepts of how planets and planetary systems are thought to form. This includes the planets in our solar system as well as exoplanets. The journey starts with the formation of a star, surrounded by a disk of gas and cosmic dust: the protoplanetary disk. This disk is the environment in which (and contains the matter from which) planets form. We will therefore discuss in quite some depth the structure, dynamics, thermodynamics and chemistry of these disks, including radiative transfer, hydrodynamics, magnetohydrodynamics, etc. And we will discuss the wealth of observations of these disks that have been obtained, in particular in the last decade, with the VLT and Subaru telescopes, with ALMA, and with several space-borne telescopes such as JWST. We will then move on to discuss the richness of physical phenomena that underpin the long journey from micrometer-sized dust (=rock) particles all the way to many-thousand kilometer sized planets. These include, among other things: gas turbulence, dust particle drift, coagulation and fragmentation of dust aggregates, formation of planetesimals through streaming instability, restricted three-body problem, dynamical friction, pebble accretion, planetary migration, planetary collisions, N-body dynamics, gas accretion, (pebble-)isolation mass, planetary interiors, equations of state at high pressures and temperatures, phase diagrams of rocks, magma oceans, clues from the Solar system (meteoritic evidence, planetary orbits, etc), and many more.

Goal

After this course you will have an overview of the research field of planet formation, including the basics and the currently 'big open questions' in the field.

Content

Observational methods using photons (from gamma rays to radio), gravitational waves, other particles, and in-situ exploration.  
MVAstro1 ("Astronomical Techniques (compact)") consists of lectures, exercises, and a lab course.  See Master Module Manual for details.

Course Information

Content

The lecture is equivalent to the bachelor module parts WPAstro.1+2 during the winter and summer terms but requires a slightly higher level of basic physical knowledge. 


Nevertheless also motivated 3rd semester BSc students are welcome to participate. 
This lecture is organised as a block course with 2 parts from Sep. 22 - Oct. 19th, 2024. 

Certificates are only given for active participation in the exercises (meaning also being present at all exercises) and passing the written examination.

Homework should/can be done in groups of 2(3)

Bachelor students

You can choose:

WPAstro.1,2:
- 8CP with marks (lab course needed for complete module)
- The written examination will be graded
- Marks count for the full 10CP including the lab course

MVAstro0:
- 8CP, no marks as a master module in the ‘Wahlbereich’
-
Master students (MVAstro0)
- 8CP, no marks - only passed
- Can be used as part of MVMod (specialisation in Astrophysics)
- Can be used as an option: just 8CP

PhD (including IMPRS)
Active participation in exercises is strongly recommended, and a successful written exam for certificate

More info on the rules for studying astronomy in Heidelberg: https://www.zah.uni-heidelberg.de/fileadmin/user_upload/downloads/Miscellaneous/Studyplan_Astro_English.pdf


Lecturers: Prof. Dr. Stefan Jordan, Dr. Markus Pössel

Lecture Introduction to Astronomy (V, block)
Time: daily 9:30 - 13:00, 22.09. - 10.10.2024 (1 free day on October 3)
Location: gHS (großer Hörsaal at Phil.12, 2nd floor) 

Exercises to Introduction to Astronomy 
Time: daily 14:30 - 16:00 (group 1), 16:00-17:30 (group 2)
Location: Neuer Hörsaal (at Phil.12)


Content
22.9.  Introduction/Fundamentals of Astronomy: Jordan
23.9.  Fundamentals 2: Jordan
24.9.  Sun and Planetary System 1: Jordan
25.9.  Sun an Planetary System 2: Jordan
26.9.  Telescopes and Instruments: Jordan
29.9.  Radiation and stars: Jordan
30.9.  Stellar evolution: Jordan
1.10.  Introduction; Expanding Universes 1: Pössel
2.10.  Expanding Universes 2; Big Bang Phase: Pössel
6.10.  Structure Formation; Basic Galaxy Properties: Pössel
7.10.  Galaxy Spectra; Stellar Motion in Galaxies 1: Pössel
8.10.  Stellar Motions in Galaxies 2; Star Formation in Galaxies; The Milky Way: Pössel
9.10. Central Black Holes; Active Galaxies; Gravitational Lensing: Pössel
10.10. Galaxy Groups and Clusters; Milky Way Archaeology; Galaxy Evolution: Pössel
TBD:  Written exam

Content

See Master Module Manual.  The block course consists of lectures, exercises, a seminar, and a written exam at the end.

Content

From binaries to Dwarf galaxies and everything in between: Binaries; Star clusters: chemical elements & their formation; dynamics & structure; dwarf galaxies: chemical evolution & Dark Matter; different flavours of star clusters and dwarf galaxies.

Content

As most of the radiation we receive from galaxies is star light, we can use it to measure and study their properties. These lectures aim at showing how much we can learn about galaxy evolution from the study of stellar populations in galaxies (young to old stellar clusters, field stars, resolved and integrated stellar populations). We will review the methods commonly used in this respect, all resting on our understanding of stellar evolution, and discuss the results obtained when we apply them to observational data, such as multi-wavelength photometry and spectroscopy.

Content

C1: - Basic properties of fluids and plasmas in astrophysics
	Ideal versus dissipative fluids
	Euler and the Navier-Stokes equations
	Compressible, weakly compressible and incompressible fluid flows
	Magnetohydrodynamics
C2: Numerical methods in hydrodynamics
	The equations in the finite space
	Conditionally versus unconditionally stable numerical schemes
Explicit & implicit formulation
	Preconditioning techniques and defect-correction iteration procedure

C3: Introduction to programming and computer-solving of simple      
       equations
C4: Introduction to General Relativity & Relativistic Cosmology
	Derivation of the relativistic & general relativistic Euler and Navier-Stokes equations
	Dynamics of the expanding univbbbberse
	Basic concepts in modern cosmology: 
Black holes, dark matter, dark energy, inflation
C5: Numerical aspects of relativistic Cosmology: UNIMOUN

Course Information

Content

Stellar structure, evolution and explosions, including practical tutorials based on the MESA stellar evolution code. 

In the first half of the term, teaching will be via classical blackboard-style lectures that lay the foundation of stellar evolution. In contrast to classical lectures on stellar astrophysics, the second half is a practical course where students employ the stellar evolution code MESA to study the evolution and final fates of low-, intermediate- and high-mass stars. This allows us to follow the evolution of stars interactively, enabling us to investigate stellar structures in great detail. For the practical part, a laptop is required (all operating systems are supported). 

All course materials will be provided online.

Content

Introduction to the dynamics of systems dominated by gravity (from planetary systems to galaxies) and their numerical treatment.

Content

In this class, we will discuss the basics of asteroseismology. After some more theoretical introduction, each student will analyse a star for its asteroseismic signal and deduce stellar parameters. We end with a journal club.

Course Information

Content

This is a five day block course with lectures in the morning and practical hands-on exercises in the afternoon. We will learn the basic technique to use GPU (graphical processing units, graphics cards) for numerical accelerated computing at the example of CUDA - an extension of the C programming language, which is used for the NVIDIA GPU accelerated supercomputer to be used in our course. More general approaches for other systems will be discussed. Concepts of parallel programming are introduced. GPU accelerated parallel computing is a technique, which is now widely used in computational physics and astrophysics. Many supercomputers of EuroHPC Petascale systems use GPU.
Topics: Parallel Computing, GPU Hardware, Elements of CUDA Language, Data Transfer, Vector and Matrix Operations, Simple Application for N-Body Problem.

Content

- Lessons learned from gravitational wave sources.
- Compact object formation from stars and binary stars.
- Dynamics of compact objects in dense star clusters.
- Merger rate density evolution of binary compact objects across cosmic time.
- Observations and models of dormant compact objects.
- Numerical models of compact-object populations.

Goal

After completion of this course, the students will acquire state-of-the-art knowledge in the field of astrophysical compact objects. They will be aware of the main results of gravitational-wave observatories, and will have advanced knowledge of the formation channels of binary compact objects and dormant black holes. They will run some of the main scripts and codes to model compact object formation (population synthesis codes, direct N-body codes, semi-analytic codes, simplified LIGO-Virgo data analysis scripts).

Content

An introduction to fluid dynamics in an astrophysical context, with an emphasis on analytical results rather than numerical simulations.

Content

- Observable signatures of black holes and binaries thereof, calculations of predictions in GR
- Post-Newtonian approximation
- 3+1, Numerical Relativity
- Black Hole images with Very-Long baseline Interferometry (EHT): theory and data analysis
- Accreting black holes, GRMHD
- Bayesian Methods
- Simulated data generation and utilization: eht-imaging, PyCBC, Bilby, Themis

Course Information

Content

• Ray optics
• Wave optics
• Beam optics, Gaussian optics
• Fourier optics
• Interference and coherence
• Photons and atoms
• Laser theory and lasertypes
• Ultra-short laser pulses
• Non-linear optics
• Modern applications

Goal

After completing this course the students will be able to ¿ describe the basic principles and experimental methods of optics and photonics, ¿ analyse standard experimental approaches to optics and photonics, ¿ design experimental set-ups in optics and photonics, ¿ apply the methods to simple experimental examples.

Content

Basic physical principles in imaging techniques such as X-ray/CT and MRI.

Content

Biospectrscopy
Lasers in Medicine

Content

- Physics of the atmosphere (structure, composition, dynamics, global circulation, radiation) 
- Applications in atmospheric physics (e.g. micro-meteorology, trace gas cycles, atmospheric chemistry, measurement techniques)

Goal

Students achieve an advanced understanding of the physical and chemical processes in the atmosphere, the methods to study them, and their role in the climate system. They are able to solve advanced problems and interpret the results in the context of current questions in research and application. They can assess and use current scientific literature to further develop their knowledge base, enabling them to conduct independent master research projects in atmospheric physics.

Content

Various remote sensing methods in different spectral ranges for the measurement of atmospheric properties are presented. 
The individual chapters start with the underlying physical interactions. Then the technical realisations and instruments are discussed. Finally examples of atmospheric measurements presented and their relevance for scientific questions (e.g. air pollution, climate change) are discussed.
If non-German speaking participants attend the lecture, it will be given in English. Otherwise in German.

Goal

Comprehensive knwoledge about various atmospheric remote sensing rechniques

Content

Lecture on the physics of the climate system, its statistical nature, energy and mass transfer, its sensitivity to external forcing and internal feedback. Climate variability will be discussed on different time scales as well as the cycles of water and green house gases and some important aspects on the response of system compartments on forcing. Lastly, a glimpse is given on climate modelling of present and past climate.

Goal

Students achieve an advanced understanding of the climate system and the methods to study it, including its changes in the past and the modern human impact on it. They are able to solve advanced problems and interpret the results in the context of current research questions and societal implications. They can competently and critically assess the public discourse on climate change on the basis of the current scientific literature. They have developed a knowledge base that enables them to conduct independent master research projects in physics of climate.

Content

- Stratification and circulation of lakes, Navier Stokes – eq.
– solutes, solubility, electrical conductivity
– density, stability and mixing, deep water renewal
– surface waves, seiche, interfacial waves
– internal waves
- properties of internal waves
- Permanent stratification, meromixis, climate sensitivity
- Turbulence I: Introduction to turbulence
- Turbulence II: Spectral characteristics and measurements
- Turbulence III: Momentum and mass transport in turbulent boundary layers
- Turbulence IV: Living in turbulence: biological – physical interactions 
- tracers in aquatic environments

Content

1-week block lecture, language: English, Mar. 2 - 6, 2026, IUP - INF229, first floor (R108), lecturer: Dr. Jochen Landgraf

The lecture will cover the principles of radiative transfer with a focus on the Earth's atmosphere including a discussion of electromagnetic waves, radiometric quantities and polarization, absorption and emission by molecules, scattering by molecules and particles, radiative transfer equation and solution methods for the Earth's atmosphere, remote sensing applications.

Content

• Foundations of statistics, information, entropy
• Statistical description of physical systems
• Ensembles, density of states
• Irreversibility
• State variables, ideal and real gases, thermodynamic potentials, the fundamental laws of thermodynamics,
• Material constants, equilibrium of phases and chemical equilibrium, law of mass action, ideal solutions
• Fermi- and Bose-statistics, ideal quantum gases
• Phase transitions, critical phenomena (Ising model)
• Transport theory (linear response, transport equations, master equation, Boltzmann equation, diffusion)
• The theory of the solid state as an example for a non-relativistic field theory
• Applications, for example specific heat of solids, thermodynamics of the early universe etc.

Goal

After completing the course the students ¿ have a thorough knowledge and understanding of the laws of thermodynamics and of the description of ensembles in the framework of classical and quantum statistics and there applications to phase transitions, condensed matter, plasma and astrophysics ¿ have acquired the necessary mathematical knowledge and competence for an in-depth understanding of this research field, ¿ have advanced competence in the fields of theoretical physics covered by this course, i.e. the ability to analyze physical phenomena using the acquired concepts and techniques, to formulate models and find solutions to specific problems, and to interpret the solutions physically and communicate them efficiently, ¿ are able to broaden their knowledge and competence in this field of theoretical physics on their own by a systematical study of the literature.

Content

• Quantizing scalar fields
• Canonical quantization and path-integral quantization
• Radiative corrections, renormalization
• Quantizing spin 1 fields
• Dirac equation
• Quantizing spin 1/2 fields
• Interacting fields, S-matrix
• Feynman rules, cross sections
• Quantum Electrodynamics, QED processes at tree level

Goal

After completing the course the students ¿ have a thorough knowledge and understanding of relativistic field equations and the theory of free quantum fields, ¿ will be able to use Feynman rules to calculate on the tree level scattering amplitudes and cross sections for ¿4-theory and for simple reactions in QED, ¿ have acquired the necessary mathematical knowledge and competence for an in-depth understanding of this research field, ¿ have advanced competence in the fields of theoretical physics covered by this course, i.e. the ability to analyze physical phenomena using the acquired concepts and techniques, to formulate models and find solutions to specific problems, and to interpret the solutions physically and communicate them efficiently, ¿ are able to broaden their knowledge and competence in this field of theoretical physics on their own by a systematical study of the literature.

Content

Condensed Matter Theory I:
The complexity of 1023 particles interacting with each other in a solid give rise to many emergent phenomena one would not predict from the simple interactions between two electrons. In this lecture we will, starting from simple models and theories work our way into the contemporary theory of many particle physics. 
 
The lecture follows for a large part the textbook of Ashcroft and Mermin, with one big difference. The aforementioned text-book is based on a text over 50 years old. During the last decades new methods have emerged, often removing the need to know the full wave-function of the system to answer the problem, by using Green's functions. Whenever possible the later will be used within this lecture.
 
Concepts of many particle systems discused are:
The Drude Theory of Metals
The Sommerfeld Theory of Metals
Electrons in a periodic potential
Tight binding
Band-structure, Fermi-surface, Density of states, Metals, Insulators, Semiconductors
Semiconductor physics
Surface states
Phonons and disorder
Relativistic corrections - spin-orbit coupling
Phase transitions and topology
Response functions
Theoretical / Mathematical tools used will be
Second quantization
Green's functions (on an independent particle level)
Self energy (for surface states and disorder)
Levels of theory discussed will be
Mean-field theory
Hartree-Fock
Density functional theory

Content

For details about content and exercises see
https://www.mpi-hd.mpg.de/manitop/ParticlePhysics3/index.html

Content

All relevant information can be found under
https://www.thphys.uni-heidelberg.de/~hebecker/Strings/strings.html

Course Information

Content

This advanced theory lecture builds on the statistical physics course (MKTP1) and introduces paradigmatic models of statistical physics and their critical properties near phase transitions.  In particular, we shall discuss the Heisenberg and O(N) vector models, the nonlinear sigma model, the XY model, the Sine-Gordon model, and the spherical model.  By computing their critical behavior, one can understand the phase transitions in many different systems in statistical physics, condensed matter physics and beyond, which belong to the same universality classes.  We will use field theoretic methods and introduce renormalization, epsilon expansion, and duality transformation.

Contents:

1. Landau theory and O(N) vector model
2. Renormalization group and universality
3. Nonlinear sigma model and epsilon expansion
4. Topological excitations in the XY and Sine-Gordon models and the Berezinskii-Kosterlitz-Thouless transition
5. Spherical model and quantum phase transitions
6. Disordered systems
7. Random walks
8. Critical dynamics

Content

After a (condensed) review of the Standard Model of Particle Physics and of features of nature that we do not yet understand, I will present ways to extend the SM at high energies and (theoretical and experimental) guidance we have on our road to find out how nature could look like at shortest distances.

Topics covered in the lecture include Electroweak Symmetry Breaking and its Dynamics, Models of a Composite Higgs, Supersymmetry, Extra Dimensions, and further approaches to understand the puzzling hierarchies we observe in nature. Moreover, I will discuss Effective Field Theory, Flavor Physics & Neutrino Masses, Dark Matter, Baryogenesis and other aspects of Cosmology, as well as the Strong CP Problem and Axions.

Content

- Basic concepts of numerical simulations, continuous and discrete simulations
- Discretization or ordinary differential equations, integration schemes of different order
- N-Body problems, molecular dynamics, collisionless systems
- Discretization of partial differential equations
- Finite element and finite volume methods
- Lattice methods
- Adaptive mesh refinement and multi-grid methods
- Matrix solvers and FFT methods
- Monte Carlo methods, Markov Chains, applications in statistical physics

Goal

After completion of this module, the students are endowed with the capacity to identify and classify numerical problems. They have reached active understanding of applicable numerical methods and algorithms. They are able to solve basic physical problems with adequate numerical techniques and to recognize the range of validity of numerical solutions.

Content

The non-thermal radiation that we observe from astrophysical sources points to the presence of very energetic particles (electrons or protons) within these sources. This seminar aims to give insights into source characteristics and processes, facilitating efficient particle acceleration. A specific focus will be given to physical concepts and astrophysical contexts, including a discussion of selective highlight results.

Goal

This seminar aims to give insights into source characteristics and processes, facilitating efficient particle acceleration.

Content

Students present recent papers. https://sciai-lab.org/teaching/journal-club/

Content

Durchführung von mehreren astrophysikalischen Versuchen je nach Kenntnisstand innerhalb einer Woche. Diese decken grosse Gebiete in der Astronomie ab. Dauer pro Versuch 1-1.5 Tage. Kein separates Protokoll oder Hausarbeit notwendig.

Goal

Selbstständige Bearbeitung experimenteller Fragestellungen. Kennenlernen und Vertiefung diverser astronomischer moderner Tools wie zB Datenreduktion, virtuelles Observatorium, Interpretation diagnostischer Diagramme.