A5084402507- Solar and Space Plasma Dynamics
- Ionosphere and magnetosphere dynamics
- Stellar, planetary, and galactic studies
- Geomagnetism and Paleomagnetism Studies
- Geophysics and Gravity Measurements
- Astro and Planetary Science
- Gamma-ray bursts and supernovae
- Oil, Gas, and Environmental Issues
- Superconducting Materials and Applications
- Solar Energy Systems and Technologies
- Meteorological Phenomena and Simulations
- Spacecraft and Cryogenic Technologies
- Solar Thermal and Photovoltaic Systems
- Computational Fluid Dynamics and Aerodynamics
- Advanced Power Generation Technologies
- Silicon Carbide Semiconductor Technologies
- Medical Imaging Techniques and Applications
- Landslides and related hazards
- Particle Accelerators and Free-Electron Lasers
- Advanced X-ray and CT Imaging
- Photovoltaic System Optimization Techniques
University of Wrocław
2005-2023
Astronomical Institute of the Slovak Academy of Sciences
2023
High Altitude Observatory
2013
We present a statistical analysis of 66 days observations quiescent (non-erupting) coronal cavities and associated velocity thermal structures. find that nested rings LOS-oriented are common in occurrence spatially well correlated with observed emission. the majority possess multiple rings, range on order several $km/sec$. tops prominences lie systematically below cavity center location largest Doppler velocity. Finally, we use DEM to consider temperature structure two relation cavity,...
It is well known that there a temporal relationship between coronal mass ejections (CMEs) and associated flares. The duration of the acceleration phase related to rise flare. We investigate CMEs with slow long events (LDEs), i.e. flares rising phase. determined relationships analyzed CME kinematics in detail. parameters (GOES flux, phase) show strong correlations (velocity, during main phase, phase). These confirm relation LDEs CMEs. also CMEs, velocity, an height at end are characterized by...
Abstract Solar coronal cavities are regions of rarefied density and elliptical cross-section. The Coronal Multi-channel Polarimeter (CoMP) obtains daily full-Sun observations in linear polarization, allowing a systematic analysis the magnetic field polar-crown prominence cavities. These commonly possess characteristic “lagomorphic” signature polarization that may be explained by flux-rope model. We analyze spatial relation between EUV cavity CoMP signature.
Slow long-duration events (SLDEs) are flares characterized by the long duration of their rising phase. In many such cases impulsive phase is weak without typical short-lasting pulses. Instead, smooth, long-lasting hard X-ray (HXR) emission observed. We analyzed and morphology six selected SLDEs. our analysis we utilized data from RHESSI GOES satellites. The physical parameters HXR sources were obtained imaging spectroscopy used for energy balance analysis. characteristic decay time heating...
Context: The Yohkoh/HXT observations of Long Duration Events (LDEs) showed that the HXR emission (14-23 keV) is present for tens minutes after flare maximum. Hence, some heating process expected to exist during time. better energy resolution RHESSI compared HXT allow us analyse LDEs in more comprehensive way. Aims: We selected three observed by answer questions how long can be present, where it emitted, what its nature and much should released sustain emission. Methods: used data reconstruct...
In a standard method of determining electron density for soft X-ray (SXR) flare kernels it is necessary to assume what the extension kernel along line sight. This source significant uncertainty obtained densities. our previous paper (Bak-Steslicka and Jakimiec, 2005) we have worked out another deriving density, in which not The point that many flares, during their decay phase, evolve sequence steady-state models [quasi-steady-state (QSS) evolution] then scaling law, derived models, can be...
Whitepaper #127 in the Decadal Survey for Solar and Space Physics (Heliophysics) 2024-2033. Main topics: basic research. Additional ground-based missions/projects; solar physics; space-based user-need-driven space weather
Abstract Quiescent coronal cavities can provide insight into solar magnetic fields. They are observed in the emission lines both polarized and unpolarized light. In total linear polarization fraction ( L / I ), they often possess a “lagomorphic,” or “rabbit-shaped,” structure that reflects underlying field configuration. We studied quiescent between 2012 2018 by Coronal Multichannel Polarimeter (CoMP). The majority of our study had characteristic lagomorphic polarization. additionally...
Magnetism defines the complex and dynamic solar corona. Coronal mass ejections (CMEs) are thought to be caused by stresses, twists, tangles in coronal magnetic fields that build up energy ultimately erupt, hurling plasma into interplanetary space. Even ever-present wind possesses a three-dimensional morphology shaped global field, forming geoeffective corotating interaction regions. CME evolution structure of depend intimately on so comprehensive observations magnetothermal atmosphere...
We analyse the observational characteristics for a set of Long Duration Events (LDE) using Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). Excellent energy resolution (1 keV) HXR images reconstructed with RHESSI allowed us to perform imaging spectroscopy coronal loop top sources (LTS) observed hours after maximum flare. found that are large structures. The diameter an LTS is changing time and energy. temperature component can be few dozen maximum. For some intervals clear...
It is well known, that there temporal relationship between CMEs and associated flares. The duration of the acceleration phase related to rise a flare. We investigated with long flares slow (slow LDE). These are characterized by high velocity (v>1000 km/s) during propagation low average main, prolongated, phase. accelerated until height $> 5 R_\odot$, which higher value than in typical impulsive CMEs. LDEs have characteristics both classes CMEs, i.e. eruptive prominences.
As it was shown by many authors, a slow decrease in X-rays observed during the decay phase of long duration flares (LDE) can be explained only magnetic reconnection and energy release ceaselessly ongoing coronal part flare. Using RHESSI data we try to answer two following questions. How effective are these processes at LDEs how precisely rate calculated based on data? To questions images selected their were reconstructed. Physical parameters flare sources obtained from image spectral...
Whitepaper #047 in the Decadal Survey for Solar and Space Physics (Heliophysics) 2024-2033. Main topics: basic research. Additional solar physics; space-based missions/projects; user-need-driven space weather