Transcript
![Page 1: Sven De Rijcke, Bert Vandenbroucke , NN Ghent University · • WP5: radiation & dynamics Benefit from collaborations with groups working on (solar) plasma physics, radiative transfer,](https://reader035.vdocuments.us/reader035/viewer/2022071003/5fc01055d7f5205dbd7b8dc0/html5/thumbnails/1.jpg)
Sven De Rijcke, Bert Vandenbroucke, NN
Ghent University
![Page 2: Sven De Rijcke, Bert Vandenbroucke , NN Ghent University · • WP5: radiation & dynamics Benefit from collaborations with groups working on (solar) plasma physics, radiative transfer,](https://reader035.vdocuments.us/reader035/viewer/2022071003/5fc01055d7f5205dbd7b8dc0/html5/thumbnails/2.jpg)
• UV escape fraction → cosmic UV background Previous work: • Need good handle on neutral fraction Paardekooper et al. 2011,
• Coupling with radiative transfer code Razoumov & Sommer-Larsen 2010, Wise & Chen 2009
Oesch et al. 2010 Large population of z~7 dwarf galaxies
![Page 3: Sven De Rijcke, Bert Vandenbroucke , NN Ghent University · • WP5: radiation & dynamics Benefit from collaborations with groups working on (solar) plasma physics, radiative transfer,](https://reader035.vdocuments.us/reader035/viewer/2022071003/5fc01055d7f5205dbd7b8dc0/html5/thumbnails/3.jpg)
Conclusions
hydrodynamical props. ↑ Heating by SN, UV background → ionization balance → cooling/heating rate Chianti(Py) ↓ UV escape fraction High-fidelity simulations → observational domain
• WP1: code coupling • WP3: turbulence • WP5: radiation & dynamics
Benefit from collaborations with groups working on (solar) plasma physics, radiative transfer, … → CHARM