CV Lattes
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Universidade de São Paulo (USP). Escola de Artes, Ciências e Humanidades (EACH) (Institutional affiliation from the last research proposal) Birthplace: Polônia
Professor Doctor (MS3) at University of São Paulo. Concluded his doctoral degree in 2006 in the area of Astronomy from Jagiellonian University in Cracow, Poland. Other postdoctoral fellowships include University of Wisconsin-Madison in the United States (2006-2009), the Institute of Astronomy, Geophysics and Atmospheric Sciences of University of São Paulo (2009-2012), The School of Arts, Sciences and Humanities of University of São Paulo (2013-2017), and University Cruzeiro do Sul (2015-2016). Research Assistant at Astronomical Observatory of Jagiellonian University in Cracow, Poland (2007-2010) and Visiting Researcher in the Department of Physics and Astronomy of McMaster University in Hamilton, Canada (2008). Works in the area of Astronomy, with the main interest in Numerical Modelling of classical and relativistic processes, processes related to turbulence and magnetic reconnection with applications in Plasma Astrophysics, High Energy Astrophysics, Space Climate, Interstellar Medium Evolution, Relativistic Jets and Intracluster Medium. (Source: Lattes Curriculum)
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Magnetized turbulence is ubiquitous in astrophysical plasmas and crucial for the formation of dense structures and stars, the stability of molecular clouds, the amplification of magnetic fields, magnetic reconnection, and the production and diffusion of cosmic rays. During the last decade it became clear, that the cascade of magnetized turbulence transferring energy from the large-scale m…
Magnetized turbulence is ubiquitous in astrophysical plasmas and crucial for the formation of dense structures and stars, the stability of molecular clouds, the amplification of magnetic fields, magnetic reconnection, and the production and diffusion of cosmic rays. During the last decade it became clear, that the cascade of magnetized turbulence transferring energy from the large-scale m…
Magnetic reconnection is a process that changes magnetic field topology in highly conducting fluids. Within the standard Sweet-Parker model, this process would be too slow to explain observations (e.g., solar flares). In reality, the process must be ubiquitous as astrophysical fluids are magnetized and motions of fluid elements necessarily entail crossing of magnetic frozen-in field line…
Nowadays in the astrophysical community, the problem of magnetic reconnection is approached using two different points of view, from the micro-physical scale using collisionless kinetic numerical studies, and from macroscopic magnetohydrodynamical fluid approximation studies, describing well the collisional media. Both approximations have their strong points, but also significant limits,…
| 2 / 2 | Ongoing grants |
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| 2 / 2 | Completed scholarships in Brazil |
| 6 / 6 | All research grants and scholarships |
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