A5046057366- Astro and Planetary Science
- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Astrophysics and Cosmic Phenomena
- Gamma-ray bursts and supernovae
- Astronomy and Astrophysical Research
- Galaxies: Formation, Evolution, Phenomena
- Astrophysical Phenomena and Observations
- Spacecraft and Cryogenic Technologies
- Pulsars and Gravitational Waves Research
- Scientific Computing and Data Management
- High-pressure geophysics and materials
- Computational Physics and Python Applications
- Laser-Plasma Interactions and Diagnostics
- Solar and Space Plasma Dynamics
- Neutrino Physics Research
- Methane Hydrates and Related Phenomena
- Space Satellite Systems and Control
- Spacecraft Dynamics and Control
- Molecular Spectroscopy and Structure
- Geophysics and Gravity Measurements
- Fluid Dynamics Simulations and Interactions
- Scientific Research and Discoveries
- Computational Fluid Dynamics and Aerodynamics
- Tropical and Extratropical Cyclones Research
Nicolaus Copernicus Astronomical Center
2001-2023
Nicolaus Copernicus University
2023
Polish Academy of Sciences
2023
Poznan Supercomputing and Networking Center
2013
University of Warsaw
2001
We have carried out a comparison study of hydrodynamical codes by investigating their performance in modelling interacting multiphase fluids. The two commonly used techniques grid and smoothed particle hydrodynamics (SPH) show striking differences ability to model processes that are fundamentally important across many areas astrophysics. Whilst Eulerian based methods able resolve treat dynamical instabilities, such as Kelvin–Helmholtz or Rayleigh–Taylor, these poorly not at all resolved...
We perform numerical simulations of a disc–planet system using various grid-based and smoothed particle hydrodynamics (SPH) codes. The tests are run for simple setup where Jupiter Neptune mass planets on circular orbit open gap in protoplanetary disc during few hundred orbital periods. compare the surface density contours, potential vorticity radial profiles at several times. gravitational torque time evolution analysed with high temporal resolution. There is overall consistency between...
We present simulations of the magnetized interstellar medium (ISM) in models massive star forming (40 Msun / yr) disk galaxies with high gas surface densities (~100 pc^2) similar to observed high-redshift disks. assume that type II supernovae deposit 10 per cent their energy into ISM as cosmic rays and neglect additional deposition thermal or momentum. With a typical Galactic diffusion coefficient for CRs (3e28 cm^2 s) we demonstrate this process alone can trigger local formation strong low...
We investigate streaming instability using two-fluid approximation (neutral gas and dust) in a quasi-global, unstratified protoplanetary disc, with the help of piernik code. compare amplification rate eigenmode numerical simulations, corresponding growth resulting from linear stability analysis full system Euler's equation including aerodynamic drag. Following Youdin & Goodman (2005), we show that (1) rapid dust clumping occurs due to difference azimuthal velocities dust, coupled by drag...
(abridged) We study the hydrodynamic evolution of a non-spherical core-collapse supernova in two spatial dimensions. find that our model displays strong tendency to expand toward pole. demonstrate this expansion is physical property low-mode, SASI instability. The leaves behind large lateral velocity gradient post shock layer which affects for minutes and hours later. This results prolate deformation ejecta fast advection Ni-rich material from moderate latitudes polar regions. effect might...
The Astropy Project (http://astropy.org) is, in its own words, "a community effort to develop a single core package for Astronomy Python and foster interoperability between astronomy packages." For five years this project has been managed, written, operated as grassroots, self-organized, almost entirely volunteer while the software is used by majority of astronomical community. Despite this, always remains day effectively unfunded. Further, contributors receive little or no formal...
We study the violent phase of merger massive binary white dwarf systems. Our aim is to characterize conditions for explosive burning occur, and identify a possible explosion mechanism Type Ia supernovae. The primary components our model systems are carbon–oxygen (C/O) dwarfs, while secondaries made either C/O or pure helium. account tidal effects in initial self-consistent way, consider initially well-separated with slow inspiral rates. evolution using an adaptive mesh refinement, reactive,...
ABSTRACT Feeding with gas in streams is well established to be an important galaxy growth mechanism. Using idealized set-up of isolated galaxy, we study the impact stream feeding (with 107 M⊙ Myr−1 rate) on star formation and outflows disc galaxies ∼1011 baryonic mass. The magnetohydrodynamical simulations are carried out piernik code include formation, feedback from supernova, cosmic ray advection diffusion, a uniform grid 195 pc spatial resolution. We find that introduction cold accreted...
We present hydrodynamical models of planetary nebulae with detached binary cores. The are obtained according to the interacting winds scenario. Slow AGB wind produced by means 3-D SPH simulations. results provide initial conditions for evolution a fast and rarefied injected into wind. In close binaries density distribution slow is significantly modified gravity secondary, resulting in an enhanced region orbital plane system, low regions elongated perpendicularly (we refer those effects as...
We study axisymmetric models of layered protoplanetary discs taking radiative transfer effects into account, and allowing for a residual viscosity in the dead zone. also explore effect different prescriptions. In addition to ring instability reported first paper series, we find an oscillatory zone, accompanied by variations accretion rate onto central star. provide simplified analytical description explaining mechanism oscillations. Finally, that enables stationary large regions discs. Based...
We investigate the motion of massless particles orbiting primary star in a close circular binary system with particular focus on gas drag effects. These are first calculations ranging size from 1 m to 10 km, which account for presence tidally perturbed gaseous disk. have found numerically that radial mass transport by tidal waves plays crucial role orbital evolution particles. In outer region disk, where its perturbation is strongest, migration rate particle all considered sizes enhanced...
Abstract We investigate the impact of gas accretion in streams on evolution disc galaxies, using magneto-hydrodynamic simulations including advection and anisotropic diffusion cosmic rays generated by supernovae as only source feedback. Stream has been suggested an important galaxy growth mechanism cosmological we vary their orientation angular momentum idealised setups. find that trigger formation galactic rings enhanced star formation. The rates consequently ray driven outflow are higher...
The slow and dense wind from a symbiotic red giant (RG) can be significantly deflected toward the orbital plane by gravitational pull of companion star. In such an environment, ionizing radiation creates highly asymmetric region. We present three-dimensional models regions in S-type systems, for which we calculate radio maps spectra. show that standard assumption spherically symmetric RG results wrong shapes, sizes spectra ionized regions, turn affects observational estimates separation mass...
We review recent results of SPH simulations gravitational instability in gaseous protoplanetary disks,emphasizing the role thermodynamics both isolated and binary systems. Contradictory appeared literature regarding disk fragmentation at tens AU from central star are likely due to different treatment radiation physics as well reflecting initial conditions. Further progress on subject requires extensive comparisons between codes with requirement that same conditions adopted. It is discussed...
The resolution criterion for self-gravity in AMR codes derived by Truelove et al. (1997) based on the Jeans length is a very robust one and thus quite popular. We believe that some configurations, such as self-gravitating discs, there are reasons to supplement it order properly resolve gravitational instabilities clump formation processes at reasonable computational costs.
We investigate numerically the orbital evolution of massive extrasolar planets within central cavities their parent protoplanetary discs. Assuming that they arrive at inner edge disc due to type II migration, we show spiral further in. find in magnetospheric more stop migrating a larger distance from disc. This effect may qualitatively explain correlation between masses and periods found for with P shorter than 5 days.
Feeding with gas in streams is predicted to be an important galaxy growth mechanism. Using idealised setup, we study the impact of stream feeding (with 10$^7$ M$_{\odot}$ Myr$^{-1}$ rate) on star formation and outflows disc galaxies $\sim$10$^{11}$ baryonic mass. The magneto-hydrodynamical simulations are carried out PIERNIK code include formation, feedback from supernova, cosmic ray advection diffusion. We find that accretion enhances galactic formation. Lower angular momentum result more...
We develop a new algorithm for the production and propagation of cosmic ray (CR) secondary elements within framework Cosmic Ray Energy SPectrum (CRESP) module Piernik MHD code (Ogrodnik et al. ApJS 253, 18, 2021). CRESP is based on piece-wise power-law (coarse-grained) method self-consistent numerically efficient in magnetized ISM galaxies. demonstrate capability our to model spectral evolution multiple CR species, including primary ones, as products obtained by spallation process. perform...
Galactic outflows and extended non-thermal emission due to Comic Ray (CR) electrons have been observed from many edge-on galaxies in the radio range of electromagnetic radiation, allowing us estimate strength vertical structure galactic magnetic field. We construct a global model NGC891 based on observational characteristics this galaxy. assume that large scales, dynamics magnetized ISM is driven by Cosmic Rays. apply coarse-grained momentum finite volume (CGMV), for solving Fokker–Planck CR...