Welcome and opening

• Debora Lančová (Institute of Physics, Silesian University in Opava)
• Jiri Svoboda (Czech Academy of Sciences)
• Michal Dovčiak (Astronomický ústav AV ČR, v.v.i.)

Accretion Processes around Black Holes in XRB and AGN (Thermal Radiation, Reprocessing in the X-ray corona and from disc reflection)

• Jiri Horak (Astronomical Institute ASCR, Prague)

Non-thermal X-ray emission

• Anabella Araudo (FZU - Institute of Physics of the Czech Academy of Sciences & Astronomical Institute of the Czech Academy of Sciences)

X-ray Astronomy: past, present and future

• Giorgio Matt

After a brief review of the history of X-ray Astronomy, I will describe the present major X-ray facilities and discuss the future directions of X-ray astronomy: high energy resolution and polarimetry.

Radiative transfer codes TITAN & CLOUDY

• Agata Rozanska

STOKES

• Frederic Marin

MONK

• Wenda Zhang

Create a model output with a radiative transfer code TITAN or MONK

• Rozanska Agata
• Michal Bursa (ASU)

Relativistic thermal radiation

• Michal Bursa (ASU)

Relativistic reflection models (KY code)

• Michal Dovčiak (Astronomický ústav AV ČR, v.v.i.)

XSPEC - Implementation of table and analytical models

• Michal Dovčiak (Astronomický ústav AV ČR, v.v.i.)

Higher order images with Fe Kα-lines from relativistic discs and Introduction to ISSI, Bern

• Maurizio Falanga

In my first talk I present a study of the contributions to the relativistic Fe K α line profile from higher order images (HOIs) produced by strongly deflected rays from the disc which cross the plunging region, located between the innermost stable circular orbit (ISCO) radius and the event horizon of a Kerr black hole. We investigate the characteristics features imprinted by the HOIs in the line profile for different black hole spins, disc emissivity laws, and inclinations. We find that they extend from the red wing of the profile up to energies slightly lower than those of the blue peak, adding ∼0.4-1.3 per cent to the total line flux. The contribution to the specific flux is often in the ∼1 to 7 per cent range, with the highest values attained for low and negative spin (a ≲ 0.3) black holes surrounded by intermediate inclination angle (i ∼ 40°) discs. The results are applied to observe HOI in Large Area Detecto missions like eXTP. In my second talk I will introduce the International Space Science Institute in Bern, Switzerland. ISSI is an institute of excellence aiming to serve the different space science communities as an international and multi-disciplinary platform. Everybody can apply with a proposal to one of the ISSI study tools, if approved, ISSI is financially supposing the scientific project to be partially carried out at its premises as a visiting scientist.

Build your model with the table created on Day 2 into the Xspec

• Michal Bursa (ASU)
• Michal Dovčiak (Astronomický ústav AV ČR, v.v.i.)

High-resolution X-ray spectra of AGN clusters & XRISM

• Norbert Werner

Data simulations with ATHENA/X-IFU

• Elias Kammoun

Data simulations with eXTP - how to simulate X-ray background

• Alessandra de Rosa

Statistical tools for X-ray spectral fitting

• Peter Boorman (Astronomical Institute of the Czech Academy of Sciences)

Simulate data with your created models for your ATHENA X-IFU or eXTP mission

• Elias Kammoun
• Jiri Svoboda (Czech Academy of Sciences)

Timing and Reverberation Techniques

• Iossif Papadakis

General relativistic magnetohydrodynamical simulations with HARM

• Petra Suková (ASU CAS)

I will present the basic usage of the GRMHD code HARM with some examples.

The magic R in GRRMHD

• Debora Lančová (Institute of Physics, Silesian University in Opava)

The redundant R in GRRHMD stands for Radiation - in this short talk I will present how it works in the Koral code, why we want to use it and shortly what are other ways how to implement radiation in MHD codes.

Concluding remarks

• Debora Lančová (Institute of Physics, Silesian University in Opava)
• Michal Dovčiak (Astronomický ústav AV ČR, v.v.i.)
• Jiri Svoboda (Czech Academy of Sciences)