Institut für Physik und Astronomie
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Keywords
- diffusion (59)
- stars: massive (57)
- gamma rays: general (47)
- anomalous diffusion (46)
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- cosmic rays (44)
- stars: winds, outflows (42)
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- ISM: supernova remnants (37)
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- intergalactic medium (34)
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- acceleration of particles (33)
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- stars: mass-loss (33)
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- methods: numerical (31)
- stars: Wolf-Rayet (31)
- galaxies: active (28)
- astroparticle physics (25)
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- stars: magnetic field (24)
- turbulence (24)
- synchronization (23)
- subdwarfs (22)
- techniques: spectroscopic (22)
- binaries: close (21)
- galaxies: formation (21)
- stochastic processes (21)
- Synchronisation (20)
- stars: abundances (20)
- climate change (19)
- instabilities (19)
- magnetic fields (18)
- stars: fundamental parameters (18)
- data analysis (17)
- galaxies: evolution (17)
- Galaxy: halo (16)
- binaries: general (16)
- galaxies: jets (16)
- hydrodynamics (16)
- perovskite solar cells (16)
- MHD (15)
- magnetohydrodynamics (MHD) (15)
- Sun: corona (14)
- Sun: coronal mass ejections (CMEs) (14)
- Sun: flares (14)
- Sun: magnetic fields (14)
- Synchronization (14)
- methods: data analysis (14)
- relativistic processes (14)
- stars: neutron (14)
- white dwarfs (14)
- BL Lacertae objects: general (13)
- Datenanalyse (13)
- azobenzene (13)
- shock waves (13)
- surveys (13)
- Klimawandel (12)
- Sun: activity (12)
- binaries: spectroscopic (12)
- galaxies: ISM (12)
- galaxies: high-redshift (12)
- gravitational waves (12)
- methods: observational (12)
- radiative transfer (12)
- stars: variables: general (12)
- Galaxy: evolution (11)
- ISM: abundances (11)
- ISM: clouds (11)
- Kuramoto model (11)
- dark matter (11)
- dynamics (11)
- gamma rays: stars (11)
- Nichtlineare Dynamik (10)
- Sun: photosphere (10)
- chaos (10)
- gamma rays: ISM (10)
- gamma-ray burst: general (10)
- plasmas (10)
- polymers (10)
- radiation belts (10)
- spectroscopy (10)
- stars (10)
- stars: AGB and post-AGB (10)
- stars: winds (10)
- techniques: imaging spectroscopy (10)
- techniques: photometric (10)
- Chaos (9)
- ISM: structure (9)
- Spektroskopie (9)
- Sun: chromosphere (9)
- additive manufacturing (9)
- atmosphere (9)
- cosmology: observations (9)
- dark ages, reionization, first stars (9)
- galaxies: interactions (9)
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- model (9)
- nonlinear dynamics (9)
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- stars: kinematics and dynamics (9)
- thin films (9)
- waves (9)
- Astrophysik (8)
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- charge transport (8)
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- fractional Brownian motion (8)
- galaxies (8)
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- morphology (8)
- nanoparticles (8)
- noise (8)
- outflows (8)
- quasars: general (8)
- residual stress (8)
- solar cells (8)
- stars: activity (8)
- stars: emission-line, Be (8)
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- techniques: polarimetric (8)
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- Brownian motion (7)
- Hertzsprung-Russell and C-M diagrams (7)
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- binaries: eclipsing (7)
- catalogs (7)
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- first passage time (7)
- galaxies: abundances (7)
- hysteresis (7)
- machine learning (7)
- magnetism (7)
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- nonergodicity (7)
- numerical relativity (7)
- organic photovoltaics (7)
- photoelectron spectroscopy (7)
- photoluminescence (7)
- planets and satellites: rings (7)
- pulsars: general (7)
- solar wind (7)
- sunspots (7)
- surface (7)
- techniques: image processing (7)
- transport (7)
- ultrafast (7)
- Biophysik (6)
- Diffusion (6)
- H II regions (6)
- ISM: kinematics and dynamics (6)
- Kosmologie (6)
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- ageing (6)
- analysis (6)
- biophysics (6)
- computed tomography (6)
- diffuse radiation (6)
- dust, extinction (6)
- electrons (6)
- elementary particles (6)
- exoplanets (6)
- first-passage time (6)
- fluorescence (6)
- galaxy evolution (6)
- gamma-rays: general (6)
- general relativity (6)
- geometric Brownian motion (6)
- infrared: stars (6)
- massive stars (6)
- methods: analytical (6)
- molecular dynamics (6)
- molecular motors (6)
- networks (6)
- non-fullerene acceptors (6)
- oscillations (6)
- phase transition (6)
- piezoelectricity (6)
- planetary nebulae: general (6)
- polarization (6)
- recombination (6)
- scattering (6)
- star formation (6)
- stars: horizontal-branch (6)
- stars: late-type (6)
- stellar evolution (6)
- surface relief grating (6)
- synchrotron radiation (6)
- ultrafast dynamics (6)
- ARPES (5)
- Arctic (5)
- Coupled oscillators (5)
- Exoplaneten (5)
- Galaxy: center (5)
- Galaxy: structure (5)
- Gammastrahlungsastronomie (5)
- Greenland (5)
- ISM: jets and outflows (5)
- ISM: lines and bands (5)
- ISM: magnetic fields (5)
- Lidar (5)
- Oberfläche (5)
- Organic solar cells (5)
- Physik (5)
- Radiation belts (5)
- Residual stress (5)
- Resonant inelastic X-ray scattering (5)
- Stochastische Prozesse (5)
- Strahlungstransport (5)
- Ti-6Al-4V (5)
- Turbulenz (5)
- X-ray (5)
- X-ray spectroscopy (5)
- activity (5)
- black holes (5)
- charge generation (5)
- climate impacts (5)
- comets: general (5)
- complex systems (5)
- conjugated polymers (5)
- cosmology: theory (5)
- density (5)
- ferroelectret (5)
- films (5)
- galaxies: haloes (5)
- galaxies: halos (5)
- galaxies: nuclei (5)
- gamma-ray astronomy (5)
- graphene (5)
- history and philosophy of astronomy (5)
- integral field spectroscopy (5)
- komplexe Netzwerke (5)
- kosmische Strahlung (5)
- laser powder bed fusion (5)
- methods: statistical (5)
- microscopy (5)
- models (5)
- molekulare Motoren (5)
- organic semiconductors (5)
- particle-in-cell simulations (5)
- pattern formation (5)
- phase transitions (5)
- physics (5)
- planet-star interactions (5)
- planets and satellites: atmospheres (5)
- random diffusivity (5)
- reionization (5)
- simulation (5)
- stars: chemically peculiar (5)
- stars: distances (5)
- stars: formation (5)
- statistical physics (5)
- stellar activity (5)
- stochastic resetting (5)
- supergiants (5)
- supernovae: general (5)
- superstatistics (5)
- ultraviolet: ISM (5)
- voltage losses (5)
- Astronomie (4)
- Astroteilchenphysik (4)
- Atlantic meridional overturning circulation (4)
- Bose-Einstein condensation (4)
- Dictyostelium (4)
- Electrets (4)
- Ellipsometrie (4)
- Enceladus (4)
- FLASH (4)
- Ferroelectrets (4)
- Ferroelektrete (4)
- Fluoreszenz (4)
- Gitterdynamik (4)
- ISM: molecules (4)
- Langevin equation (4)
- Levy flights (4)
- Nanopartikel (4)
- Nanostruktur (4)
- Nonlinear Dynamics (4)
- Oberflächengitter (4)
- Phase (4)
- Physikdidaktik (4)
- Planetary rings (4)
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- Rashba effect (4)
- Rauschen (4)
- Röntgenspektroskopie (4)
- Simulation (4)
- Simulationen (4)
- Solar cells (4)
- Sterne (4)
- Sternentstehung (4)
- Sun (4)
- Teilchenbeschleunigung (4)
- Van Allen Probes (4)
- X-ray diffraction (4)
- X-ray emission spectroscopy (4)
- X-rays (4)
- Zeitreihenanalyse (4)
- accretion, accretion disks (4)
- adsorption (4)
- astronomy (4)
- astrophysical plasmas (4)
- bacteria (4)
- black hole physics (4)
- catalysis (4)
- charge-transfer (4)
- climate (4)
- conductivity (4)
- confinement (4)
- control (4)
- convection (4)
- cosmology (4)
- creep (4)
- dynamical systems (4)
- dynamo (4)
- dünne Schichten (4)
- electronic structure (4)
- electrostatic interactions (4)
- entanglement (4)
- errata, addenda (4)
- ferroelectrets (4)
- ferroelectric polymers (4)
- first-passage (4)
- galaxies: fundamental parameters (4)
- galaxies: star formation (4)
- global jets (4)
- globular clusters: general (4)
- gravity (4)
- group field theory (4)
- helical magnetic fields (4)
- impact (4)
- instability (4)
- large-scale structure of Universe (4)
- line: identification (4)
- magnetohydrodynamics (4)
- magnetostriction (4)
- membrane (4)
- microlensing (4)
- mid-temperature transition (4)
- mobility (4)
- modeling (4)
- neural networks (4)
- neutrinos (4)
- particle acceleration (4)
- perovskite (4)
- phase oscillators (4)
- phase separation (4)
- photovoltaics (4)
- physics education (4)
- polypropylene (4)
- power spectral analysis (4)
- prediction (4)
- quantum field theory (4)
- quantum gravity (4)
- random walks (4)
- relativistic jets (4)
- sea-level rise (4)
- stars: black holes (4)
- stars: low-mass (4)
- stars: magnetic fields (4)
- statistics (4)
- stellar physics (4)
- stellar winds (4)
- stochastic models (4)
- subdiffusion (4)
- supernova remnants (4)
- synthesis (4)
- temperature (4)
- thiouracil (4)
- ultrafast x-ray diffraction (4)
- 2D (3)
- 2D perovskites (3)
- AFM (3)
- AGN (3)
- Adhäsion (3)
- Adsorption (3)
- Aerosol (3)
- Aluminum alloys (3)
- Anomalous diffusion (3)
- Antarctica (3)
- Antarktis (3)
- Astrophotonik (3)
- Astrophysics (3)
- BL Lacertae objects: individual: Mrk 421 (3)
- BL Lacertae objects: individual: PKS 2155-304 (3)
- Bayesian inference (3)
- Chromosphere (3)
- Complex networks (3)
- Cosmic rays (3)
- Cosmology (3)
- Crystallization (3)
- Curie transition (3)
- DNA (3)
- Dark Matter (3)
- Datenassimilation (3)
- Debye screening (3)
- Dictyostelium discoideum (3)
- Dynamik (3)
- EMIC (3)
- Electrophoretic deposition (3)
- Fokker-Planck equation (3)
- Galaxienentwicklung (3)
- Galaxy: stellar content (3)
- Gammastrahlung (3)
- Genetic programming (3)
- Granulation (3)
- H.E.S.S. (3)
- Hilbert transform (3)
- Holocene (3)
- Hydrodynamik (3)
- ISM: bubbles (3)
- Instrumentation and data management (3)
- Integrated Assessment (3)
- Interstellar medium (3)
- Jets (3)
- Kalman filter (3)
- Klimatologie (3)
- Ladungstransport (3)
- Lasers (3)
- Lattice dynamics (3)
- Lehrkräftebildung (3)
- Levy walk (3)
- Levy walks (3)
- Lyapunov exponent (3)
- Magnetisierungsdynamik (3)
- Mars (3)
- Mittag-Leffler functions (3)
- Molekulardynamik (3)
- Motilität (3)
- NEXAFS (3)
- Netzwerke (3)
- Neutron diffraction (3)
- Nicht-Fulleren-Akzeptoren (3)
- OLED (3)
- Organische Solarzellen (3)
- Oszillatoren (3)
- Ozon (3)
- P(VDF-TrFE-CFE) terpolymer (3)
- Perovskites (3)
- Perowskit (3)
- Phase transitions (3)
- Phasenübergang (3)
- Photoelektronenspektroskopie (3)
- Photovoltaik (3)
- Physics Education (3)
- Plasmaphysik (3)
- Polyelektrolyte (3)
- Quantengravitation (3)
- Quantenoptik (3)
- Quasar (3)
- Rashba-Effekt (3)
- Reflexivität (3)
- Rekurrenzanalyse (3)
- Resonanzenergietransfer (3)
- Röntgenbeugung (3)
- STM (3)
- Saturn, Rings (3)
- Schwarze Löcher (3)
- Semiconductors (3)
- Sonnenkorona (3)
- Statistical and Nonlinear Physics (3)
- Sternaktivität (3)
- Sternwinde (3)
- Strahlungsgürtel (3)
- Sun: atmosphere (3)
- Sun: filaments (3)
- Sun: sunspots (3)
- Supernovaüberreste (3)
- Synchrotronstrahlung (3)
- Theorie (3)
- Thin films (3)
- Thiouracil (3)
- Transformation toughening (3)
- Ultrafast X-ray diffraction (3)
- Unsicherheitsanalyse (3)
- Wellenleiter (3)
- X-ray absorption spectroscopy (3)
- X-ray imaging (3)
- X-ray photoelectron spectroscopy (3)
- XPS (3)
- Zelladhäsion (3)
- accretion (3)
- active transport (3)
- aspect ratio (3)
- azobenzene surfactant (3)
- behavior (3)
- biological physics (3)
- brushes (3)
- carbon nitride (3)
- catalogues (3)
- cell adhesion (3)
- charge storage (3)
- charge transfer (3)
- chemical modification (3)
- chimera state (3)
- chimera states (3)
- comets: individual: 67P/Churyumov-Gerasimenko (3)
- complementarity (3)
- continuous time random walk (3)
- coupled rotators (3)
- critical avalanche dynamics (3)
- critical phenomena (3)
- cylindrical geometry (3)
- damage (3)
- dark ages (3)
- dark matter theory (3)
- data assimilation (3)
- dielectric relaxation spectroscopy (3)
- diffraction (3)
- diffusing diffusivity (3)
- doping (3)
- dust (3)
- efficiency (3)
- electromagnetic radiation (3)
- electrostatics (3)
- ellipsometry (3)
- energy (3)
- equation of state (3)
- filaments (3)
- financial time series (3)
- first stars (3)
- first-hitting time (3)
- flares (3)
- galaxies: individual: LMC (3)
- galaxies: magnetic fields (3)
- galaxy structure (3)
- genomic DNA conformation (3)
- global surface warming (3)
- globular clusters: individual: NGC 6397 (3)
- hypersound (3)
- individual (3)
- infrared: diffuse background (3)
- inorganic perovskites (3)
- interactions (3)
- interface engineering (3)
- interfaces (3)
- intergalaktisches Medium (3)
- iron (3)
- kinetic instabilities (3)
- laser pulses (3)
- lattice dynamics (3)
- lidar (3)
- line: profiles (3)
- linearized gravity (3)
- magnetic reconnection (3)
- magnetoconvection (3)
- massereiche Sterne (3)
- mechanical properties (3)
- memory and delay (3)
- metal (3)
- molecular doping (3)
- nanoscale heat transfer (3)
- nanostructure (3)
- network (3)
- neuronal networks (3)
- neutron stars (3)
- nitrogen (3)
- noisy systems (3)
- non-equilibrium (3)
- nonfullerene acceptors (3)
- nonlinear time series analysis (3)
- nonradiative voltage losses (3)
- nucleobases (3)
- numerical simulations (3)
- ocean heat uptake (3)
- open-circuit voltage (3)
- optical manipulation (3)
- optical spectroscopy (3)
- optics (3)
- organic electronics (3)
- organic solar cell (3)
- organische Halbleiter (3)
- organische Solarzellen (3)
- particles (3)
- photocatalysis (3)
- photocurrent generation (3)
- photoelectron (3)
- photosensitive surfactants (3)
- photovoltaic devices (3)
- piezoelectret (3)
- piezoelectrets (3)
- pitch angle (3)
- planetary rings (3)
- planets and satellites: individual (Saturn) (3)
- plasma physics (3)
- plasmonics (3)
- polyelectrolyte adsorption (3)
- polyelectrolytes (3)
- polymer (3)
- polymer solar cells (3)
- porosity (3)
- power spectrum (3)
- pp-wave solutions (3)
- processing (3)
- projections (3)
- protein folding (3)
- protein search (3)
- quantum friction (3)
- quantum optics (3)
- quantum thermodynamics (3)
- quasar (3)
- quasars (3)
- quasi-Fermi level splitting (3)
- radio continuum: stars (3)
- random walk (3)
- recurrence (3)
- recurrence analysis (3)
- recurrence plot (3)
- resonant energy transfer (3)
- ring current (3)
- rotation (3)
- roughness (3)
- scaled Brownian motion (3)
- schwarze Löcher (3)
- silicon (3)
- simulations (3)
- spectra (3)
- splitting (3)
- stability (3)
- stars: (3)
- stars: coronae (3)
- stars: mass loss (3)
- stars: oscillations (3)
- stars: pre-main sequence (3)
- starspots (3)
- statistical models (3)
- statistische Modelle (3)
- stellar populations (3)
- stochastic processes (theory) (3)
- stochastic resonance (3)
- stochastische Prozesse (3)
- sulfur (3)
- surface treatment (3)
- surface-relief gratings (3)
- synchronization transition (3)
- synchrotron X-ray diffraction (3)
- temperature dependence (3)
- texture (3)
- time averaging (3)
- time series analysis (3)
- titanium dioxide (3)
- tropical cyclones (3)
- ultrafast X-ray diffraction (3)
- ultraschnell (3)
- ultraviolet: galaxies (3)
- uncertainty analysis (3)
- vulnerability (3)
- waveguides (3)
- wetting (3)
- x-ray diffraction (3)
- 1D (2)
- 3D (2)
- 4 (2)
- 4-nitrobenzenethiol (2)
- AG (2)
- AU (2)
- Accretion (2)
- Active Galactic Nuclei (2)
- Active regions, magnetic fields (2)
- Additive manufacturing (2)
- Adhesion (2)
- Aerosole (2)
- Akkretion (2)
- Allgemeine Relativitätstheorie (2)
- Amazon rainforest (2)
- Anfangsdaten (2)
- Anisotropie (2)
- Anisotropy (2)
- Antarctic (2)
- Anthropogene Klimaänderung (2)
- Antibiotics (2)
- Atmosphere (2)
- Atmosphärendynamik (2)
- Atmosphärenmodellierung (2)
- Auger electron spectroscopy (2)
- Auger–Meitner (2)
- Azobenzene containing cationic surfactants (2)
- BL Lacertae objects: individual (2)
- BL Lacertae objects: individual (Mrk 501) (2)
- BL Lacertae objects: individual: Mrk 501 (2)
- Bacterial biofilms (2)
- Bakterien (2)
- Bayesian estimation (2)
- Benetzung (2)
- Biofilms (2)
- Biological defense mechanisms (2)
- Blazar (2)
- Blocking (2)
- Boltzmann distribution (2)
- Bose-Einstein condensate (2)
- Bragg peak (2)
- Brillouin scattering (2)
- Brownian yet non-Gaussian diffusion (2)
- Capacitive sensor (2)
- Casimir effect (2)
- Casimir-Polder interaction (2)
- Cassini (2)
- Cations (2)
- Ceramics (2)
- Charge recombination (2)
- Chebyshev inequality (2)
- Chemotaxis (2)
- Climate Change (2)
- Climate change (2)
- Coherence (2)
- Collisional physics (2)
- Comb model (2)
- Comets (2)
- Complementarity (2)
- Computed tomography (2)
- Computertomographie (2)
- Convolutional neural networks (2)
- Corona, active (2)
- Coster–Kronig (2)
- Crab Nebula (2)
- Crack deflection (2)
- Cystic fibrosis (2)
- DFT (2)
- Dark matter (2)
- Deep learning (2)
- Dielectric Relaxation Spectroscopy (DRS) (2)
- Dielectric materials (2)
- Differential Scanning Calorimetry (DSC) (2)
- Disorder (2)
- Displays (2)
- Donor-Acceptor (DA) interface (2)
- Donor-acceptor copolymers (2)
- Doping (2)
- Dunkle Materie (2)
- Dust (2)
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- Dynamische Systeme (2)
- Dynamo (2)
- Eigenspannung (2)
- Electrical properties and parameters (2)
- Electron spectroscopy (2)
- Electronic and spintronic devices (2)
- Elektret (2)
- Elektronenbeschleunigung (2)
- Embedding (2)
- Entscheidung bei Unsicherheit (2)
- Entstehung der Milchstraße (2)
- Equilibrium-line altitudes (2)
- Erdbeben (2)
- Extremereignisse (2)
- Fachwissen (2)
- Fermi (2)
- Fernerkundung (2)
- Ferroelektret (2)
- Ferroelektrika (2)
- Filament (2)
- Filamente (2)
- Fox H-function (2)
- Fractional moments (2)
- Freie-Elektronen-Laser (2)
- Frequenzkonversion (2)
- Galactic center (2)
- Galaktische Archäologie (2)
- Galaxie (2)
- Galaxienhaufen (2)
- Galaxy: formation (2)
- Galaxy: general (2)
- Galaxy: kinematics and dynamics (2)
- Gamma-ray astronomy (2)
- Gammaastronomie (2)
- Gas phase (2)
- Gaussian processes (2)
- Gold (2)
- Graphen (2)
- Graphene (2)
- Gravitationslinsen (2)
- Gravitationslinseneffekt (2)
- Grenzschicht (2)
- Gyrochronologie (2)
- H.E.S.S (2)
- HII regions (2)
- Hertzsprung-Russell and colour-magnitude diagrams (2)
- Hochdruck (2)
- Hong-Ou-Mandel effect (2)
- Hydraulic models (2)
- Hydraulic networks (2)
- Hydrodynamics (2)
- Hydrogel (2)
- Hysterese (2)
- Hysteresis (2)
- IACT (2)
- ISM (2)
- ISM: individual objects: G338.3-0.0 (2)
- ISOS-L-1I protocol (2)
- In-situ Experimente (2)
- Indian Monsoon (2)
- Indian summer monsoon (2)
- Indischer Monsun (2)
- Inner magnetosphere (2)
- Instrumentation (2)
- Integral field spectroscopy (2)
- Integralfieldspektroskopie (2)
- Integrierte Bewertung (2)
- Intergalactic Medium (2)
- Intergalaktisches Medium (2)
- Irradiation (2)
- Keimbildung (2)
- Klima (2)
- Kolloides System (2)
- Kompensatoren (2)
- Komplexe Systeme (2)
- Kopplung (2)
- Kp index (2)
- Krebsnebel (2)
- Kuramoto (2)
- Kuramoto-Modell (2)
- L-Asterisk (2)
- LDPE nanocomposites (2)
- Laboratory astrophysics (2)
- Laser powder bed fusion (2)
- Laserstrahlschmelzen (2)
- Lokalisierung (2)
- Lévy flights (2)
- Lévy walks (2)
- Löschkurve (2)
- MU-M (2)
- Machine learning (2)
- Magellansche Wolken (2)
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Institute
- Institut für Physik und Astronomie (5515)
- Extern (67)
- Interdisziplinäres Zentrum für Dynamik komplexer Systeme (38)
- Institut für Chemie (18)
- Institut für Geowissenschaften (12)
- Department Psychologie (9)
- Mathematisch-Naturwissenschaftliche Fakultät (7)
- Potsdam Institute for Climate Impact Research (PIK) e. V. (7)
- Institut für Biochemie und Biologie (5)
- Zentrum für Lehrerbildung und Bildungsforschung (ZeLB) (4)
Solar filaments often erupt partially. Although how they split remains elusive, the splitting process has the potential of revealing the filament structure and eruption mechanism. Here we investigate the pre-eruption splitting of an apparently single filament and its subsequent partial eruption on 2012 September 27. The evolution is characterized by three stages with distinct dynamics. During the quasi-static stage, the splitting proceeds gradually for about 1.5 hr, with the upper branch rising at a few kilometers per second and displaying swirling motions about its axis. During the precursor stage that lasts for about 10 minutes, the upper branch rises at tens of kilometers per second, with a pair of conjugated dimming regions starting to develop at its footpoints; with the swirling motions turning chaotic, the axis of the upper branch whips southward, which drives an arc-shaped extreme-ultraviolet front propagating in a similar direction. During the eruption stage, the upper branch erupts with the onset of a C3.7-class two-ribbon flare, while the lower branch remains stable. Judging from the well-separated footpoints of the upper branch from those of the lower one, we suggest that the pre-eruption filament processes a double-decker structure composed of two distinct flux bundles, whose formation is associated with gradual magnetic flux cancellations and converging photospheric flows around the polarity inversion line.
We have directly resolved in the present work the interfacial composition during and after the interactions of a saturated atmosphere of oil vapor with soluble surfactant solutions at a planar water/air interface for the first time. Experiments were conducted on interactions of hexane vapor with solutions of alkyltrimethylammonium bromides and sodium dodecyl sulfate to observe the balance between cooperativity and competition of the components at the interface.
In all cases, hexane adsorption was strongly enhanced by the presence of the surfactant, even at bulk surfactant concentrations four orders of magnitude below the critical micelle concentration. Cooperativity of the surfactant adsorption was observed only for sodium dodecyl sulfate at intermediate bulk concentrations, yet for all four systems, competition set in at higher concentrations, as hexane adsorption reduced the surfactant surface excess. The data fully supported the complete removal of hexane from the interface following venting of the system to remove the saturated atmosphere of oil vapor.
These results help to identify future experiments that would elaborate and could explain the cooperativity of surfactant adsorption, such as on cationic surfactants with short alkyl chains and a broader series of anionic surfactants. This work holds relevance for oil recovery applications with foam, where there is a gas phase saturated with oil vapor.
Scanning manufacturing parameters determining the residual stress state in LPBF IN718 small parts
(2021)
The influence of scan strategy on the residual stress (RS) state of an as-built IN718 alloy produced by means of laser powder bed fusion (LPBF) is investigated. Two scan vector rotations (90 degrees-alternation and 67 degrees-rotation), each produced following two different scan vector lengths (long and short), are used to manufacture four rectangular prisms. Neutron diffraction (ND) and laboratory X-ray diffraction (XRD) techniques are used to map the bulk and surface RS state, respectively. The distortion induced upon removal from the baseplate is measured via profilometry. XRD measurements show that the two long scan vector strategies lead to higher RS when compared with the equivalent short scan vector strategies. Also, the 67 degrees-rotation strategies generate lower RS than their 90 degrees-alternation counterparts. Due to the lack of reliable stress-free d0 references, the ND results are analyzed using von Mises stress. In general, ND results show significant RS spatial non-uniformity. A comparison between ND and distortion results indicates that the RS component parallel to the building direction (Z-axis) has a predominant role in the Z-displacement. The use of a stress balance scheme allows to discuss the d0 variability along the length of the specimens, as well as examine the absolute RS state.
Fractional Brownian motion, a Gaussian non-Markovian self-similar process with stationary long-correlated increments, has been identified to give rise to the anomalous diffusion behavior in a great variety of physical systems. The correlation and diffusion properties of this random motion are fully characterized by its index of self-similarity or the Hurst exponent.
However, recent single-particle tracking experiments in biological cells revealed highly complicated anomalous diffusion phenomena that cannot be attributed to a class of self-similar random processes.
Inspired by these observations, we here study the process that preserves the properties of the fractional Brownian motion at a single trajectory level; however, the Hurst index randomly changes from trajectory to trajectory.
We provide a general mathematical framework for analytical, numerical, and statistical analysis of the fractional Brownian motion with the random Hurst exponent.
The explicit formulas for probability density function, mean-squared displacement, and autocovariance function of the increments are presented for three generic distributions of the Hurst exponent, namely, two-point, uniform, and beta distributions.
The important features of the process studied here are accelerating diffusion and persistence transition, which we demonstrate analytically and numerically.
Cosmic-ray (CR) diffusion is the result of the interaction of such charged particles against magnetic fluctuations. These fluctuations originate from large-scale turbulence cascading toward smaller spatial scales, decomposed into three different modes, as described by magnetohydrodynamics (MHD) theory.
As a consequence, the description of particle diffusion strongly depends on the model describing the injected turbulence.
Moreover, the amount of energy assigned to each of the three modes is, in general, not equally divided, which implies that diffusion properties might be different from one region to another.
Here, motivated by the detection of different MHD modes inside the Cygnus-X star-forming region, we study the 3D transport of CRs injected by two prominent sources within a two-zone model that represents the distribution of the modes.
Then, by convolving the propagated CR distribution with the neutral gas, we are able to explain the 𝛾-ray diffuse emission in the region, observed by the Fermi-LAT and HAWC Collaborations.
Such a result represents an important step in the long-standing problem of connecting the CR observables with the microphysics of particle transport.
Galaxy morphology is a fossil record of how galaxies formed and evolved and can be regarded as a function of the dynamical state of a galaxy. It encodes the physical processes that dominate its evolutionary history, and is strongly aligned with physical properties like stellar mass, star formation rate and local environment. At a distance of ∼50 and 60 kpc, the Magellanic Clouds represent the nearest interacting pair of dwarf irregular galaxies to the Milky Way, rendering them an important test bed for galaxy morphology in the context of galaxy interactions and the effect of the local environment in which they reside. The Large Magellanic Cloud is classified as the prototype for Magellanic Spiral galaxies, with one prominent spiral arm, an offset bar and an inclined rotating disc while the Small Magellanic Cloud is classified as a dwarf Irregular galaxy and is known for its unstructured shape and large depth across the line–of–sight. Resolved stellar populations are powerful probes of a wide range of astrophysical phenomena, the proximity of the Magellanic Clouds allows us to resolve their stellar populations to individual stars that share coherent chemical and age distributions. The coherent properties of resolved stellar populations enable us to analyse them as a function of position within the Magellanic Clouds, offering a picture of the growth of the galaxies’ substructures over time and yielding a comprehensive view of their morphology. Furthermore, investigating the kinematics of the Magellanic Clouds offers valuable insights into their dynamics and evolutionary history. By studying the motions and velocities of stars within these galaxies, we can trace their past interactions, with the Milky Way or with each other and unravel the complex interplay of forces that have influenced the Magellanic Clouds’ formation and evolution.
In Chapter 2, the VISTA survey of the Magellanic Clouds was employed to generate unprecedented high-resolution morphological maps of the Magellanic Clouds in the near-infrared. Utilising colour-magnitude diagrams and theoretical evolutionary models to segregate stellar populations, this approach enabled a comprehensive age tomography of the galaxies. It revealed previously uncharacterised features in their central regions at spatial resolutions of 0.13 kpc (Large Magellanic Cloud) and 0.16 kpc (Small Magellanic Cloud), the findings showcased the impact of tidal interactions on their inner regions. Notably, the study highlighted the enhanced coherent structures in the Large Magellanic Cloud, shedding light on the significant role of the recent Magellanic Clouds’ interaction 200 Myr ago in shaping many of the fine structures. The Small Magellanic Cloud revealed asymmetry in younger populations and irregularities in intermediate-age ones, pointing towards the influence of past tidal interactions.
In Chapter 3, an examination of the outskirts of the Magellanic Clouds led to the identification of new substructures through the use of near-infrared photometry from the VISTA Hemisphere Survey and multi-dimensional phase-space information from Gaia. The distances and proper motions of these substructures were investigated. This analysis revealed the impact of past Magellanic Clouds’ interactions and the influence of the Milky Way’s tidal field on the morphology and kinematics of the Magellanic Clouds. A bi-modal distance distribution was identified within the luminosity function of the red clump stars in the Small Magellanic Cloud, notably in its eastern regions, with the foreground substructure being attributed to the Magellanic Clouds’ interaction around 200 Myr ago. Furthermore, associations with the Counter Bridge and Old Bridge were uncovered through the detection of background and foreground structures in various regions of the SMC.
In chapter 4, a detailed kinematic analysis of the Small Magellanic Cloud was conducted using spectra from the European Southern Observatory Science Archive Facility. The study reveals distinct kinematics in the Wing and bar regions, attributed to interactions with the Large Magellanic Cloud and variations in star formation history. Notably, velocity disparities are observed in the bar’s young main sequence stars, aligning with specific star-forming episodes, and suggesting potential galactic stretching or tidal stripping, as corroborated by proper motion studies.
We investigate the failed partial eruption of a filament system in NOAA AR 12104 on 2014 July 5, using multiwavelength EUV, magnetogram, and H alpha observations, as well as magnetic field modeling. The filament system consists of two almost co-spatial segments with different end points, both resembling a C shape. Following an ejection and a precursor flare related to flux cancellation, only the upper segment rises and then displays a prominent twisted structure, while rolling over toward its footpoints. The lower segment remains undisturbed, indicating that the system possesses a double-decker structure. The erupted segment ends up with a reverse-C shape, with material draining toward its footpoints, while losing its twist. Using the flux rope insertion method, we construct a model of the source region that qualitatively reproduces key elements of the observed evolution. At the eruption onset, the model consists of a flux rope atop a flux bundle with negligible twist, which is consistent with the observational interpretation that the filament possesses a double-decker structure. The flux rope reaches the critical height of the torus instability during its initial relaxation, while the lower flux bundle remains in stable equilibrium. The eruption terminates when the flux rope reaches a dome-shaped quasi-separatrix layer that is reminiscent of a magnetic fan surface, although no magnetic null is found. The flux rope is destroyed by reconnection with the confining overlying flux above the dome, transferring its twist in the process.
Synthesis of organic-inorganic hybrids based on the conjugated polymer P3HT and mesoporous silicon
(2022)
Organic-inorganic hybrids are a class of functional materials that combine favorable properties of their constituents to achieve an overall improved performance for a wide range of applications. This article presents the synthesis route for P3HT-porous silicon hybrids for thermoelectric applications. The conjugated polymer P3HT is incorporated into the porous silicon matrix by means of melt infiltration. Gravimetry, sorption isotherms and energy dispersive X-ray spectroscopy (EDX) mapping indicate that the organic molecules occupy more than 50% of the void space in the inorganic host. We demonstrate that subsequent diffusion-based doping of the confined polymer in a FeCl3 solution increases the electrical conductivity of the hybrid by five orders of magnitude compared to the empty porous silicon host.
This article presents inelastic thermal neutron scattering experiments probing the phonon dispersion in mesoporous silicon with pores 8 nm across. Scattering studies reveal the energy-momentum relation for transverse and longitudinal phonons along the high symmetry directions , and in the Brillouin zone. The dispersion up to phonon energies of 35 meV unambiguously proves that the phonon group velocities in highly-crystalline silicon are not modified by nanostructuring down to sub-10 nanometer length scales. On these length scales, there is apparently no effect of structuring on the elastic moduli of mesoporous silicon. No evidence can be found for phonon-softening in topologically complex, geometrically disordered mesoporous silicon putting it in contrast to silicon nanotubes and nanoribbons.
The use of post-processing heat treatments is often considered a necessary approach to relax high-magnitude residual stresses (RS) formed during the layerwise additive manufacturing laser powder bed fusion (LPBF). In this work, three heat treatment strategies using temperatures of 450 degrees C, 800 degrees C, and 900 degrees C are applied to austenitic stainless steel 316L samples manufactured by LPBF. These temperatures encompass the suggested lower and upper bounds of heat treatment temperatures of conventionally processed 316L. The relaxation of the RS is characterized by neutron diffraction (ND), and the associated changes of the microstructure are analyzed using electron backscattered diffraction (EBSD) and scanning electron microscopy (SEM). The lower bound heat treatment variant of 450 degrees C for 4 hours exhibited high tensile and compressive RS. When applying subsequent heat treatments, we show that stress gradients are still observed after applying 800 degrees C for 1 hour but almost completely vanish when applying 900 degrees C for 1 hour. The observed near complete relaxation of the RS appears to be closely related to the evolution of the characteristic subgrain solidification cellular microstructure.
We consider sedimented at a solid wall particles that are immersed in water containing small additives of photosensitive ionic surfactants. It is shown that illumination with an appropriate wavelength, a beam intensity profile, shape and size could lead to a variety of dynamic, both unsteady and steady state, configurations of particles. These dynamic, well-controlled and switchable particle patterns at the wall are due to an emerging diffusio-osmotic flow that takes its origin in the adjacent to the wall electrostatic diffuse layer, where the concentration gradients of surfactant are induced by light. The conventional nonporous particles are passive and can move only with already generated flow. However, porous colloids actively participate themselves in the flow generation mechanism at the wall, which also sets their interactions that can be very long ranged. This light-induced diffusio-osmosis opens novel avenues to manipulate colloidal particles and assemble them to various patterns. We show in particular how to create and split optically the confined regions of particles of tunable size and shape, where well-controlled flow-induced forces on the colloids could result in their crystalline packing, formation of dilute lattices of well-separated particles, and other states.
On the effects of disorder on the ability of oscillatory or directional dynamics to synchronize
(2024)
In this thesis I present a collection of publications of my work, containing analytic results and observations in numerical experiments on the effects of various inhomogeneities, on the ability of coupled oscillators to synchronize their collective dynamics. Most of these works are concerned with the effects of Gaussian and non-Gaussian noise acting on the phase of autonomous oscillators (Secs. 2.1-2.4) or on the direction of higher dimensional state vectors (Secs. 2.5,2.6). I obtain exact and approximate solutions to the non-linear equations governing the distributions of phases, or perform linear stability analysis of the uniform distribution to obtain the transition point from a completely disordered state to partial order or more complicated collective behavior. Other inhomogeneities, that can affect synchronization of coupled oscillators, are irregular, chaotic oscillations or a complex, and possibly random structure in the coupling network. In Section 2.9 I present a new method to define the phase- and frequency linear response function for chaotic oscillators. In Sections 2.4, 2.7 and 2.8 I study synchronization in complex networks of coupled oscillators. Each section in Chapter 2 - Manuscripts, is devoted to one research paper and begins with a list of the main results, a description of my contributions to the work and a short account of the scientific context, i.e. the questions and challenges which started the research and the relation of the work to my other research projects. The manuscripts in this thesis are reproductions of the arXiv versions, i.e. preprints under the creative commons licence.
Materials realizing the XY model in two dimensions are sparse.
Here we use neutron triple-axis spectroscopy to investigate the critical static and dynamical magnetic fluctuations in the square-lattice antiferromagnets Ca2RuO4 and Ca3Ru2O7.
We probe the temperature dependence of the antiferromagnetic Bragg intensity, the Q width, the amplitude, and the energy width of the magnetic diffuse scattering in the vicinity of the Neel temperature T-N to determine the critical behavior of the magnetic order parameter M, correlation length xi, susceptibility chi, and the characteristic energy Gamma with the corresponding critical exponents beta, nu, gamma, and z, respectively.
We find that the critical behaviors of the single-layer compound Ca2RuO4 follow universal scaling laws that are compatible with predictions of the two-dimensional (2D) XY model.
The bilayer compound Ca3Ru2O7 is only partly consistent with the 2D XY theory and best described by the three-dimensional (3D) Ising model, which is likely a consequence of the intrabilayer exchange interactions in combination with an orthorhombic single-ion anisotropy.
Hence, our results suggest that layered ruthenates are promising solid-state platforms for research on the 2D XY model and the effects of 3D interactions and additional spin-space anisotropies on the magnetic fluctuations.
In star-forming galaxies, the far-infrared (FIR) and radio-continuum luminosities obey a tight empirical relation over a large range of star-formation rates (SFR).
To understand the physics, we examine magnetohydrodynamic galaxy simulations, which follow the genesis of cosmic ray (CR) protons at supernovae and their advective and anisotropic diffusive transport.
We show that gravitational collapse of the proto-galaxy generates a corrugated accretion shock, which injects turbulence and drives a small-scale magnetic dynamo. As the shock propagates outwards and the associated turbulence decays, the large velocity shear between the supersonically rotating cool disc with respect to the (partially) pressure-supported hot circumgalactic medium excites Kelvin-Helmholtz surface and body modes.
Those interact non-linearly, inject additional turbulence and continuously drive multiple small-scale dynamos, which exponentially amplify weak seed magnetic fields.
After saturation at small scales, they grow in scale to reach equipartition with thermal and CR energies in Milky Way-mass galaxies. In small galaxies, the magnetic energy saturates at the turbulent energy while it fails to reach equipartition with thermal and CR energies.
We solve for steady-state spectra of CR protons, secondary electrons/positrons from hadronic CR-proton interactions with the interstellar medium, and primary shock-accelerated electrons at supernovae.
The radio-synchrotron emission is dominated by primary electrons, irradiates the magnetized disc and bulge of our simulated Milky Way-mass galaxy and weakly traces bubble-shaped magnetically loaded outflows.
Our star-forming and star-bursting galaxies with saturated magnetic fields match the global FIR-radio correlation (FRC) across four orders of magnitude. Its intrinsic scatter arises due to (i) different magnetic saturation levels that result from different seed magnetic fields, (ii) different radio synchrotron luminosities for different specific SFRs at fixed SFR, and (iii) a varying radio intensity with galactic inclination.
In agreement with observations, several 100-pc-sized regions within star-forming galaxies also obey the FRC, while the centres of starbursts substantially exceed the FRC.
In this topical review, we give an overview of the structure and dynamics of a single polymer chain in active baths, Gaussian or non-Gaussian.
The review begins with the discussion of single flexible or semiflexible linear polymer chains subjected to two noises, thermal and active.
The active noise has either Gaussian or non-Gaussian distribution but has a memory, accounting for the persistent motion of the active bath particles. This finite persistence makes the reconfiguration dynamics of the chain slow as compared to the purely thermal case and the chain swells.
The active noise also results superdiffusive or ballistic motion of the tagged monomer. We present all the calculations in details but mainly focus on the analytically exact or almost exact results on the topic, as obtained from our group in recent years.
In addition, we briefly mention important works of other groups and include some of our new results. The review concludes with pointing out the implications of polymer chains in active bath in biologically relevant context and its future directions.
How predictable is the next move of an animal? Specifically, which factors govern the short- and long-term motion patterns and the overall dynamics of land-bound, plant-eating animals in general and ruminants in particular? To answer this question, we here study the movement dynamics of springbok antelopes Antidorcas marsupialis. We propose several complementary statistical-analysis techniques combined with machine-learning approaches to analyze—across multiple time scales—the springbok motion recorded in long-term GPS tracking of collared springboks at a private wildlife reserve in Namibia. As a result, we are able to predict the springbok movement within the next hour with a certainty of about 20%. The remaining about 80% are stochastic in nature and are induced by unaccounted factors in the modeling algorithm and by individual behavioral features of springboks. We find that directedness of motion contributes approximately 17% to this predicted fraction. We find that the measure for directedeness is strongly dependent on the daily cycle of springbok activity. The previously known daily affinity of springboks to their water points, as predicted from our machine-learning algorithm, overall accounts for only about 3% of this predicted deterministic component of springbok motion. Moreover, the resting points are found to affect the motion of springboks at least as much as the formally studied effects of water points. The generality of these statements for the motion patterns and their underlying behavioral reasons for other ruminants can be examined on the basis of our statistical-analysis tools in the future.
We propose a generalization of the widely used fractional Brownian motion (FBM), memory-multi-FBM (MMFBM), to describe viscoelastic or persistent anomalous diffusion with time-dependent memory exponent α(t ) in a changing environment. In MMFBM the built-in, long-range memory is continuously modulated by α(t ). We derive the essential statistical properties of MMFBM such as its response function, mean-squared displacement (MSD), autocovariance function, and Gaussian distribution. In contrast to existing forms of FBM with time-varying memory exponents but a reset memory structure, the instantaneous dynamic of MMFBM is influenced by the process history, e.g., we show that after a steplike change of α(t ) the scaling exponent of the MSD after the α step may be determined by the value of α(t ) before the change. MMFBM is a versatile and useful process for correlated physical systems with nonequilibrium initial conditions in a changing environment.
We present real-world data processing on measured electron time-of-flight data via neural networks. Specifically, the use of disentangled variational autoencoders on data from a diagnostic instrument for online wavelength monitoring at the free electron laser FLASH in Hamburg. Without a-priori knowledge the network is able to find representations of single-shot FEL spectra, which have a low signal-to-noise ratio. This reveals, in a directly human-interpretable way, crucial information about the photon properties. The central photon energy and the intensity as well as very detector-specific features are identified. The network is also capable of data cleaning, i.e. denoising, as well as the removal of artefacts. In the reconstruction, this allows for identification of signatures with very low intensity which are hardly recognisable in the raw data. In this particular case, the network enhances the quality of the diagnostic analysis at FLASH. However, this unsupervised method also has the potential to improve the analysis of other similar types of spectroscopy data.
In recurrence analysis, the tau-recurrence rate encodes the periods of the cycles of the underlying high-dimensional time series. It, thus, plays a similar role to the autocorrelation for scalar time-series in encoding temporal correlations.
However, its Fourier decomposition does not have a clean interpretation. Thus, there is no satisfactory analogue to the power spectrum in recurrence analysis.
We introduce a novel method to decompose the tau-recurrence rate using an over-complete basis of Dirac combs together with sparsity regularization.
We show that this decomposition, the inter-spike spectrum, naturally provides an analogue to the power spectrum for recurrence analysis in the sense that it reveals the dominant periodicities of the underlying time series.
We show that the inter-spike spectrum correctly identifies patterns and transitions in the underlying system in a wide variety of examples and is robust to measurement noise.
Organic thin films are widely used in organic electronics and coatings. Such films often feature film-depth dependent variations of composition and optoelectronic properties. State-of-the-art depth profiling methods such as mass spectroscopy and photoelectron spectroscopy rely on non-intrinsic species (vaporized ions, etching-induced surface defects), which are chemically and functionally different from the original materials. Here we introduce an easily-accessible and generally applicable depth profiling method: film-depth-dependent infrared (FDD-IR) spectroscopy profilometry based on directly measuring the intrinsic material after incremental surface-selective etching by a soft plasma, to study the material variations along the surface-normal direction. This depth profiling uses characteristic vibrational signatures of the involved compounds, and can be used for both conjugated and non-conjugated, neutral and ionic materials. A film-depth resolution of one nanometer is achieved. We demonstrate the application of this method for investigation of device-relevant thin films, including organic field-effect transistors and organic photovoltaic cells, as well as ionized dopant distributions in doped semiconductors.