prof. RNDr. Miloslav Druckmüller, CSc.

E-mail:   druckmuller@fme.vutbr.cz 
WWW:   http://www.zam.fme.vutbr.cz/~druck/
Dept.:   Institute of Mathematics
Dept. of Computer Graphics and Geometry
Position:   Head of Department
Room:   A1/1934
Phone:   +420 54114 2727
Dept.:   Institute of Mathematics
Dept. of Computer Graphics and Geometry
Position:   Professor
Room:   A1/1934
Phone:   +420 54114 2727

1591

Education and academic qualification

  • 1978, Finished study of Mathematics, Faculty of Natural Sciences UJEP (today Masaryk Univerzity) Brno
  • 1979, RNDr., Mathematics, Faculty of Natural Sciences UJEP (today Masaryk Univerzity) Brno
  • 1986, CSc., Process engineering, Faculty of Mechanical Engineering, Brno University of Technology,
  • Process engineering
  • 1995, Applied Mathematics, Doc., Faculty of Mechanical Engineering, Brno University of Technology, Applied mathematics
  • |2001, Prof.,Applied Mathematics, Faculty of Mechanical Engineering, Brno University of Technology,

Career overview

  • 1979 - 1982, asisstant, Institute of Mathematics, Faculty of Mechanical Engineering, Brno University of Technology
  • 1982 - 1995, lecturer, Institute of Mathematics, Faculty of Mechanical Engineering, Brno University of Technology
  • 1995 - 2001, asoc. prof., Institute of Mathematics, Faculty of Mechanical Engineering, Brno University of Technology
  • 2001 - to date, profesor, Ústav matematiky, Institute of Mathematics, Faculty of Mechanical Engineering, Brno University of Technology

Scientific activities

  • Numerical methods of image analysis a digital image processing
  • Computer graphics
  • Many-valued logic, fuzzy set theory, expert systems
  • Complex variable analysis
  • Orthogonal transforms and their application

University activities

  • 1990 - 2006, member of academic senate of Faculty of Mechanical Engineering, Brno University of Technology
  • 2003 - to date, member of Scientific convocation of Faculty of Mechanical Engineering, Brno University of Technology
  • 2006 - to date, member of Scientific convocation of Brno University of Technology
  • 2003 - to date, chairman of the branch convocation for PhD. study - Mathematical engineering

Sum of citations (without self-citations) indexed within ISI Web of Knowledge

248

Sum of other citations (without self-citations)

Supervised courses:

Publications:

  • HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.:
    EXPLORING THE PROMINENCE-CORONA CONNECTION AND ITS EXPANSION INTO THE OUTER CORONA USING TOTAL SOLAR ECLIPSE OBSERVATIONS,
    ASTROPHYSICAL JOURNAL, Vol.2014 793, (2014), No.2, pp.119-128, ISSN 0004-637X
    journal article
  • MORGAN, H.; DRUCKMÜLLER, M.:
    Multi-Scale Gaussian Normalization for Solar Image Processing Multi-Scale Gaussian Normalization for Solar Image Processing Multi-Scale Gaussian Normalization for Solar Image Processing,
    Solar Physics, Vol.2014 (289), (2014), No.8, pp.2945-2955, ISSN 0038-0938
    journal article
  • 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,
    Solar Physics, Vol.2014 (289), (2014), No.7, pp.2487-2501, ISSN 0038-0938
    journal article
  • DRUCKMÜLLER, M.; DRUCKMÜLLEROVÁ, H.:
    A Noise Adaptive Fuzzy Equalization Method with Variable Neighborhood for Processing of High Dynamic Range Images in Solar Corona Research,
    Lecture Notes in Computer Science, Vol.2014(8466), (2014), No.5, pp.262-271, ISSN 0302-9743, Springer
    journal article
  • DRUCKMÜLLER, M.; HABBAL, S.; ANIOL, P.; DING, A.; MORGAN, H.:
    Imaging Comet ISON C/2012 S1 in the Inner Corona at Perihelion,
    Astrophysical Journal Letters, Vol.2014( 784), (2014), No.2, pp.22-25, ISSN 2041-8205
    journal article
  • DRUCKMÜLLER, M.; HABBAL, S.; MORGAN, H.:
    Discovery of aNew Class of Coronal Structures in White Light Eclipse Images,
    ASTROPHYSICAL JOURNAL, Vol.2014 (785), (2014), No.1, pp.14-22, ISSN 0004-637X
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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,
    ASTROPHYSICAL JOURNAL, Vol.734, (2011), No.1, pp.120-137, ISSN 0004-637X, Chicago Journals
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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
    journal article
  • 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
    journal article

List of publications at Portal BUT

Abstracts of most important papers:

  • HABBAL, S.; MORGAN, H.; DRUCKMÜLLER, M.:
    EXPLORING THE PROMINENCE-CORONA CONNECTION AND ITS EXPANSION INTO THE OUTER CORONA USING TOTAL SOLAR ECLIPSE OBSERVATIONS,
    ASTROPHYSICAL JOURNAL, Vol.2014 793, (2014), No.2, pp.119-128, ISSN 0004-637X
    journal article

    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,
    ASTROPHYSICAL JOURNAL, Vol.2014 (785), (2014), No.1, pp.14-22, ISSN 0004-637X
    journal article

    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
    journal article

    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,
    ASTROPHYSICAL JOURNAL, Vol.734, (2011), No.1, pp.120-137, ISSN 0004-637X, Chicago Journals
    journal article

    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
    journal article

    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.