Wintersemester 2024/2025

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Observational methods using photons (from gamma rays to radio), gravitational waves, other particles, and in-situ exploration

Informationen zur Veranstaltung

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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. 23rd - Oct. 11th, 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, 23.09. - 11.10.2024 (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)

Exercises are planned for:
Monday, Sep 23, Wednesday, Sep 27, Friday, Sep 29, Wednesday, October 4 (for part I)
Friday, Oct 6, Monday, Oct 9, Wednesday, Oct 11, Friday, Oct 13 (for part II)

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

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CONTENT: 
Diurnal and annual motions, precession and nutation, sidereal and solar time clocks, Earth-sky trajectory of a planet from its orbital elements

https://wwwstaff.ari.uni-heidelberg.de/mitarbeiter/gparm/celmech.html


COURSE SLIDES: via Moodle.  The `Enrolment key' (`Einschreibeschluessel') will be provided during the first lecture.  It will NOT be provided by email. 


REMARK:
Lecture room to be ventilated regularly.  Please dress up accordingly.

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Lecture on the formation of stars and planets. 
More details can be found on the course website (see link below).

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The diverse astronomical and astrophysical distance determination methods will be introduced and illustrated with examples, covering all distance ranges from parallax measurements of nearby stars to cosmological methods.

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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.

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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 their stellar populations (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.

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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

Informationen zur Veranstaltung

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

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

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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.

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- 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.

Lehrziel

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).

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The physics of the Universe during the Dark Ages between recombination and reionization.

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- 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

Informationen zur Veranstaltung

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• 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

Lehrziel

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

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

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Biospectrscopy
Lasers in Medicine

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Siehe Webseite:

https://www.kip.uni-heidelberg.de/cmm/teaching/2025/ecm

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- 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)

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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.

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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.

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Comprehensive knwoledge about various atmospheric remote sensing rechniques

Informationen zur Veranstaltung

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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.

Lehrziel

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.

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- 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

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• 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.

Lehrziel

After completing the course the students ż 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 ż have acquired the necessary mathematical knowledge and competence for an in-depth understanding of this research field, ż 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, ż are able to broaden their knowledge and competence in this field of theoretical physics on their own by a systematical study of the literature.

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• Quantizing scalar fields
• Interacting fields, S-matrix
• Feynman rules, cross sections
• Quantizing spin 1/2 fields
• Dirac equation
• Quantizing spin 1 fields
• Maxwell equations
• Coupling to Dirac fermions
• Quantum Electrodynamics
• QED processes at tree level
• Radiative corrections
• Classical non-abelian gauge theory

Lehrziel

After completing the course the students ż have a thorough knowledge and understanding of relativistic field equations and the theory of free quantum fields, ż will be able to use Feynman rules to calculate on the tree level scattering amplitudes and cross sections for ż4-theory and for simple reactions in QED, ż have acquired the necessary mathematical knowledge and competence for an in-depth understanding of this research field, ż 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, ż are able to broaden their knowledge and competence in this field of theoretical physics on their own by a systematical study of the literature.

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For details about content and exercises see
https://www.mpi-hd.mpg.de/manitop/StandardModel2/index.html

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

Informationen zur Veranstaltung

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Time: Wed 14:15-16:00, Place: Phil.Weg 12 / gHS

Contents:

We will give an introduction to classical non-equilibrium physics, both on the macroscopic (thermodynamic) and the microscopic (kinetic) level.

We will start by generalizing equilibrium thermodynamics to spatial degrees of freedom. By allowing for small currents (of heat or particles, for instance), the theory of linearly irreversible thermodynamics will be developed. A major insight will be the occurrence of cross-coupling effects, like the Peltier and Soret effect, obeying important symmetries (Onsager relations, Nobel Prize in Chemistry 1968). The occurrence of instabilities (I. Prigogine, Nobel Prize in Chemistry 1977) will also be discussed.

We will then switch to the microscopic scale and motivate the famous Boltzmann equation, the foundation of transport theory. We will solve it by several approximation methods and use it to derive macroscopic balance equations, yielding a microscopic foundation of the processes described in the first part of the lecture.

Finally, we make a close connection to equilibrium statistical physics, by discussing linear response theory and deriving the fluctuation-dissipation theorem. The main insight will be that the response of a system to a small perturbation, i.e. the outcome of a non-equilibrium situation, can be calculated within equilibrium theory.

If time permits, at the end we will discuss few current research topics, like the use of Boltzmann-type equations in the modeling of 'active' systems (collective motion of animals, dynamics of cellular extracts) and the occurrence of nonequilibrium phase transitions in boundary-driven transport (asymmetric exclusion processes).

Informationen zur Veranstaltung

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see https://uebungen.physik.uni-heidelberg.de/vorlesung/20242/1925

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We review the Peccei-Quinn mechanism to generate out of a massless U(1)_A Goldstone boson a massive one. The Veneziano-Witten formula is reviewed. Then we compute the axion mass for the deconfining phase of an SU(2) Yang-Mills theory. For the confining phase phenomenological extractions are used within the fuzzy dark matter paradigm. We then address the question how ultralight axions may determine the dark sector of the cosmological model and how one can extract specific cosmological parameters.

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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.

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- 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

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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.

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

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20 Beobachtungsabende nach Vereinbarung