prof. RNDr. Miloslav Druckmüller, CSc.
E-mail:   druckmuller@fme.vutbr.cz  Osobní stránka:   http://www.zam.fme.vutbr.cz/~druck/ Pracoviště:   Ústav matematiky odbor počítačové grafiky a geometrie Zařazení:   Profesor Místnost:   A1/1934

Aktuálně garantované předměty:

• Aplikace Fourierovy analýzy (SF0)
• Aplikace vícehodnotové logiky (SAL)
• Aplikace vícehodnotové logiky (SAL)
• Aplikace vícehodnotové logiky (SAL-A)
• Funkce komplexní proměnné (SKF)
• Funkce komplexní proměnné (SKF-A)
• Matematika - Vybrané statě (RMA)
• Numerické metody analýzy obrazů (TNM)
• Numerické metody analýzy obrazů (TNM-A)
• Počítačové metody zpracování obrazů (9MZO)
• Programování v Delphi (0PD)
• Průmyslový projekt (N-MAI) (0PPS)
• Průmyslový projekt (N-MAI) (0PPS-A)
• Technické aplikace metod umělé inteligence (RUI)
• Vybrané kapitoly z matematiky I (T1K)
• Vybrané kapitoly z matematiky II (T2K)

Vybrané publikace:

• HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.:
  EXPLORING THE PROMINENCE-CORONA CONNECTION AND ITS EXPANSION INTO THE OUTER CORONA USING TOTAL SOLAR ECLIPSE OBSERVATIONS
  článek v časopise ve Web of Science, Jimp
• MORGAN, H.; DRUCKMÜLLER, M.:
  Multi-Scale Gaussian Normalization for Solar Image Processing, Springer
  článek v časopise ve Web of Science, Jimp
• JEJCIC, S.; PETR HEINZEL, P.; ZAPIOR, M.; DRUCKMÜLLER, M.; STANISLAV, G.; KOTRČ, P.:
  Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence Multi-Wavelength Eclipse Observations of a Quiescent Prominence
  článek v časopise ve Web of Science, Jimp
• DRUCKMÜLLER, M.; DRUCKMÜLLEROVÁ, H.:
  A Noise Adaptive Fuzzy Equalization Method with Variable Neighborhood for Processing of High Dynamic Range Images in Solar Corona Research, Springer
  článek v časopise ve Web of Science, Jimp
• DRUCKMÜLLER, M.; HABBAL, S.; ANIOL, P.; DING, A.; MORGAN, H.:
  Imaging Comet ISON C/2012 S1 in the Inner Corona at Perihelion
  článek v časopise ve Web of Science, Jimp
• DRUCKMÜLLER, M.; HABBAL, S.; MORGAN, H.:
  Discovery of aNew Class of Coronal Structures in White Light Eclipse Images
  článek v časopise ve Web of Science, Jimp
• DRUCKMÜLLER, M.:
  A Noise Adaptive Fuzzy Equalization Method for Processing of Extreme Ultraviolet Images SOLAR EXTREME ULTRAVIOLET IMAGES,
  ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol.2013 (207), (2013), No.1, pp.25-29, ISSN 0067-0049
  článek v časopise - ostatní, Jost
• HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.; DING, A.; COOPER, J.; DAW, A.; SITTLER, E.:
  Probing the Fundamental Physics of the Solar Corona with Lunar Solar Occultation Observations,
  Solar Physics, Vol.2013 (285), (2013), No.1-2, pp.9-24, ISSN 0038-0938, Springer
  článek v časopise - ostatní, Jost
• HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; DING, A.; JOHNSON, J.; DRUCKMÜLLEROVÁ, H.; DAW, A.; ARNDT, M.; DIETZEL, M.; SAKEN, J.:
  THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11, Chicago Journals
  článek v časopise ve Web of Science, Jimp
• HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; DING, A.; JOHNSON, J.; DRUCKMÜLLEROVÁ, H.; DAW, A.; ARNDT, M.:
  The Coronal Imprints of Eruptive Prominences and CMEs as Revealed by the Total Solar Eclipse Observations of 11 July 2010,
  Bulletin of the American Astronomical Society, Vol.2011 (43), (2011), No.1, pp.1-5, ISSN 0002-7537, AAS USA
  článek v časopise - ostatní, Jost
• HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; SCHOLL, I.; RUŠIN, V.; DAW, A.; JOHNSON, J.; ARNDT, M.:
  Total Solar Eclipse Observations of Hot Prominence Shrouds,
  ASTROPHYSICAL JOURNAL, Vol.2010 (719), (2010), No.2, pp.1362-1369, ISSN 0004-637X
  článek v časopise - ostatní, Jost
• HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.; DING, A.:
  On the Constancy of the Electron Temperature in the Expanding Corona Throughout Solar Cycle 23,
  ASTROPHYSICAL JOURNAL, Vol.2010 (711), (2010), No.2, pp.75-78, ISSN 0004-637X
  článek v časopise - ostatní, Jost
• HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; DAW, A.; JOHNSON, J.; DING, A.; ARNDT, M.; ESSER, R.; RUŠIN, V.; SCHOLL, I.:
  Mapping the Distribution of Electron Temperature and Fe Charge States in the Corona with Total Solar Eclipse Observations,
  ASTROPHYSICAL JOURNAL, Vol.2010(708), (2009), No.2, pp.1650-1662, ISSN 0004-637X
  článek v časopise - ostatní, Jost
• DRUCKMÜLLER, M.:
  Phase Correlation Method for the Alignment of Total Solar Eclipse Images,
  ASTROPHYSICAL JOURNAL, Vol.2009(706), (2009), No.2, pp.1605-1608, ISSN 0004-637X
  článek v časopise - ostatní, Jost
• DRUCKMÜLLER, M.; KLVAŇA, M.; DRUCKMÜLLEROVÁ, Z.:
  Solar Spectra Analysis Based on the Statistical Moment Method,
  Cent. Eur. Astrophys. Bull, Vol.31, (2007), No.1, pp.297-307, ISSN 1845-8319
  článek v časopise - ostatní, Jost
• Hajek d., Kubesova h., Vyzula r., Mayer J., Druckmüller M., Tomiska M., Vasku A.:
  Bone marrow as multidimensional orbit oscillator after autologous bone marrow transplantation,
  Stem Cells, Vol.1999, (1999), No.17, pp.25-30, ISSN 1066-5099, AlphaMed Press
  článek v časopise - ostatní, Jost

Seznam publikací na portálu VUT

Anotace nejvýznamnějších prací:

• HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.:
  EXPLORING THE PROMINENCE-CORONA CONNECTION AND ITS EXPANSION INTO THE OUTER CORONA USING TOTAL SOLAR ECLIPSE OBSERVATIONS
  článek v časopise ve Web of Science, Jimp
  Prominences constitute the most complex magnetic structures in the solar corona. The ubiquitous presence of their seemingly confined dense and cool plasma in an otherwise million-degree environment remains a puzzle. Using a decade of white light total solar eclipse observations, we show how these images reveal an intricate relationship between prominences and coronal structures both in their immediate vicinity, known as coronal cavities, and in the extended corona out to several solar radii. Observations of suspended prominences and twisted helical structures spanning several solar radii are central to these findings. The different manifestations of the prominence-corona interface that emerge from this study underscore the fundamental role played by prominences in defining and controlling the complex expansion and dynamic behavior of the solar magnetic field in the neighborhood of magnetic polarity reversal regions. This study suggests that the unraveling of prominences and the outward expansion of the helical twisted field lines linked to them could be the solar origin of twisted magnetic flux ropes detected in interplanetary space, and of the mechanism by which the Sun sheds its magnetic helicity. This work also underscores the likely role of the prominence-corona interface as a source of the slow solar wind.
• DRUCKMÜLLER, M.; HABBAL, S.; MORGAN, H.:
  Discovery of aNew Class of Coronal Structures in White Light Eclipse Images
  článek v časopise ve Web of Science, Jimp
  White light images of the solar corona, taken during total solar eclipses, capture the complex dynamic relationship between the coronal plasma and the magnetic field. This relationship can be recorded on timescales of seconds to minutes, within a few solar radii above the solar surface. Rays, large-scale loops, and streamers, which are the brightest structures in these images, have shaped current models of the coronal magnetic field and solar wind flow. We show in this work how the application of novel image processing techniques to unique high-resolution white light eclipse images reveals the presence of a new class of structures, reminiscent of smoke rings, faint nested expanding loops, expanding bubbles, and twisted helical structures. These features are interpreted as snapshots of the dynamical evolution of instabilities developing at prominence-corona interfaces and propagating outward with the solar wind.
• DRUCKMÜLLER, M.:
  A Noise Adaptive Fuzzy Equalization Method for Processing of Extreme Ultraviolet Images SOLAR EXTREME ULTRAVIOLET IMAGES,
  ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol.2013 (207), (2013), No.1, pp.25-29, ISSN 0067-0049
  článek v časopise - ostatní, Jost
  A new image enhancement tool ideally suited for the visualization of fine structures in extreme ultraviolet images of the corona is presented in this paper. The Noise Adaptive Fuzzy Equalization method is particularly suited for the exceptionally high dynamic range images from the Atmospheric Imaging Assembly instrument on the Solar Dynamics Observatory. This method produces artifact-free images and gives significantly better results than methods based on convolution or Fourier transform which are often used for that purpose.
• HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; DING, A.; JOHNSON, J.; DRUCKMÜLLEROVÁ, H.; DAW, A.; ARNDT, M.; DIETZEL, M.; SAKEN, J.:
  THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11, Chicago Journals
  článek v časopise ve Web of Science, Jimp
  We report on the first multi-wavelength coronal observations, taken simultaneously in white light, H alpha 656.3 nm, Fe ix 435.9 nm, Fe x 637.4 nm, Fe xi 789.2 nm, Fe xiii 1074.7 nm, Fe xiv 530.3 nm, and Ni xv 670.2 nm, during the total solar eclipse of 2010 July 11 from the atoll of Tatakoto in French Polynesia. The data enabled temperature differentiations as low as 0.2 x 106 K. The first-ever images of the corona in Fe ix and Ni xv showed that there was very little plasma below 5 x 105 K and above 2.5 x 106 K. The suite of multi-wavelength observations also showed that open field lines have an electron temperature near 1x106 K, while the hottest, 2x106 K, plasma resides in intricate loops forming the bulges of streamers, also known as cavities, as discovered in our previous eclipse observations. The eclipse images also revealed unusual coronal structures, in the form of ripples and streaks, produced by the passage of coronal mass ejections and eruptive prominences prior to totality, which could be identified with distinct temperatures for the first time. These trails were most prominent at 106 K. Simultaneous Fe x 17.4 nm observations from Proba2/SWAP provided the first opportunity to compare Fe x emission at 637.4 nm with its extreme-ultraviolet (EUV) counterpart. This comparison demonstrated the unique diagnostic capabilities of the coronal forbidden lines for exploring the evolution of the coronal magnetic field and the thermodynamics of the coronal plasma, in comparison with their EUV counterparts in the distance range of 1-3R. These diagnostics are currently missing from present space-borne and ground-based observatories.
• HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.; DING, A.:
  On the Constancy of the Electron Temperature in the Expanding Corona Throughout Solar Cycle 23,
  ASTROPHYSICAL JOURNAL, Vol.2010 (711), (2010), No.2, pp.75-78, ISSN 0004-637X
  článek v časopise - ostatní, Jost
  A recent analysis of Fe emission lines observed during the total solar eclipses of 2006 March 29 and 2008 August 1 established the first empirical link between the electron temperature in the expanding corona and Fe charge states measured in interplanetary space. In this Letter, we use this link to infer this temperature throughout solar cycle 23 from in situ charge state measurements from the Solar Wind Ion Composition Spectrometer (SWICS) on the Advanced Composition Explorer (ACE) and on Ulysses. The distribution of the SWICS/ACE Fe charge states, which span cycle 23 from 1998 to 2009, is skewed with a peak centered on Fe8+, Fe9+, and Fe10+ and a tail spanning Fe12+ to Fe20+. An iterative process based on this distribution and on the Fe ion fraction as a function of electron temperature yields a narrow peak at 1.1 E6 K. The tail in the measured charge state distribution is attributed to the sporadic release of material hotter than 2 E6 K from closed magnetic structures within the bulges of streamers. The Fe Ulysses charge state measurements between 1992 and 1997 from cycle 22 peaked at Fe11+, indicative of a slightly higher temperature of 1.5 E6 K. The relative constancy of the electron temperature in the expanding corona throughout solar cycle 23 points to the presence of an unknown mechanism regulating the energy input to electrons in the acceleration region of the solar wind at all latitudes during this cycle.