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Monika
Moscibrodzka Astrophysicist enjoying numerical astrophysics, modeling fluid dynamics, imaging black hole shadows, chasing accelerated particles 


Here I list four main research projects that I'm leading or I'm involved in. Astronomy/physics students who would like to work with me on any of the listed topics are welcome to contact me. 1. Hunting for Black Hole Shadows in the Centers of the Milky Way and M87 Galaxy
Both observationally and theoretically, the study of gas flows near black holes is on the verge of a breakthrough. Observationally, the Event Horizon Telescope will soon make for the first time resolved images of the black holes at event horizon scales in the centers of the Milky Way and the M87 galaxy. I am involved in all these efforts through the ERC Black Hole Camera collaboration. This is not a real picture of a black hole shadow. This is a theoretical prediction of apperance of the black hole event horizon in the center of the Milky Way at mm wavelength at which EHT operates. See one of my articles in Astronomy and Astrophysics for more details. 2. Constraining Physics of Accretion and Jets in Low Luminosity Active Galactic Nuclei
Recent improvements in theoretical modeling for the first time allow for realistic and detailed predictions of the observational signatures of accretion flows and jets near a black hole. High performance computations allow us now to follow the dynamics of plasma and magnetic fields in the vicinity of the black hole in great detail. However, coupling these simulations properly to observations via radiation remained a problem for a long time. The main source of uncertainty is the thermodynamics of radiating electrons. I have recently found a natural way to parametrize the electron thermodynamics which properly recovers the basic observational characteristics of black hole systems. Movie Click on the figure above to follow the evolution of realistic model of accreting black hole as seen by observer on earth. The movie starts when the black hole is surrounded by a ring of magnetized plasma. Due to viscous forces caused by magnetic turbulence the plasma looses angular momentum and falls onto the black hole event horizon. In a later stage a relativistic jet is formed. The movie is a result of combing 3D general relativistic MHD simulations of fluid dynamics around Kerr black hole (with HARM3D code) with general relativistic radiative transfer model. We will confront this and other models of accretion with various radio/millimeter VLBI and high energy (like in Near Infrared and Xray bands) observations and estimate the properties of plasma and black hole spin in aforementioned astrophysical systems. 3. Covariant Polarized Radiative Transfer
To confront MHD accretion theory with astrophysical observations a good model of radiative transfer is required. I have developed and codeveloped (with graduate students) a few various stateoftheart codes for simulating radiative transfer through astrophysical plasma in strong gravitational field. My latest development is ipole  a semianalytic, covariant (i.e., independent of geometry of spacetime) general relativistic code for polarized radiative transport. My code is public and free to use, it will be available here. The code documentation is published in Monthly Notices of Royal Astronomical Society. How a magnetized accretion flow onto a black hole looks like in polarized light? The figure below shows one of the World most accurate images of that based on ipole calculation. The information about geometry of magnetic fields is in polarized component of radiation (Stokes Q, U, and V). Modeling the polarized electromagnetic counterparts of accreting black holes is the most promissing way to learn about magnetizm of compact objects. This study is crucial to find out, for example, how relativistic jets, that we do observe in many astrophysical systems, are launched and powered. 4. Radiationdriven Outflows from Active Galactic Nuclei


