People by Discipline

Name	Discipline	Category	Phone	Office
Leviatan Amiram	Nuclear Hadronic and Few-Body Physics	Faculty	02 6585 136	Kaplun 206
Paul Michael	Nuclear Hadronic and Few-Body Physics	Emeriti	02 6584 795	Kaplun 16
Barnea Nir	Nuclear Hadronic and Few-Body Physics	Faculty	02 6585 138	Popick 114
Panagiotis Georgoudis	Nuclear Hadronic and Few-Body Physics	Post-Docs	02 6584 354	Kaplun 202
Gavrielov Noam	Nuclear Hadronic and Few-Body Physics	Graduate Students	02 6586 788	Kaplun 213
Cohen Dan	Nuclear Hadronic and Few-Body Physics	Graduate Students	02 6584 783	Kaplun Bldg.
Ohayon Ben	Nuclear Hadronic and Few-Body Physics	Graduate Students	02 6585 868	Kaplun Bldg.
Weiss Ronen	Nuclear Hadronic and Few-Body Physics	Graduate Students		Popick Bldg.
Krief Menahem	Nuclear Hadronic and Few-Body Physics	Graduate Students		Popick Bldg.
Gazit Doron	Nuclear Hadronic and Few-Body Physics	Faculty	02 6586 858	Popick 125

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Upcoming Events

Monday, November 11th

Physics Colloquium : "Forging the Future of CERN."
- Start time: 12:00pm
- End date: Monday, November 11th
- End time: 01:30pm
- Lecturer: Prof. Eliezer Rabinovici (HUJI)Abstract:The Council of CERN is responsible for formulating the scientific and financial policy of CERN.It does this with strong coordination with the CERN Director General and Management.I will describe how the Cern Council reaches its decisions in general and the process in the recent years that has led to initiating the Fourth European Strategy Group for Particle Physics. The expected timeline for that process will be outlined as well.
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Tuesday, November 12th

astrolunch: Thorsten Naab
- Start time: 12:30pm
- End date: Tuesday, November 12th
- End time: 01:30pm
- Title: 14 orders of magnitude - from the multi-phase ISM to IMBH formationSpeaker: Thorsten NaabAbstract: The rapid collision of stars and compact objects in young, dense and massive star clusters has been proposed in the late 70’s as a formation channel for the first massive black holes as the seeds for supermassive black holes. Confirming this process with numerical models has been a challenge since then. A self-consistent model following the formation of a galactic star cluster in a massive gas cloud down to the coalescence of black holes would have to cover more than 14 orders of magnitude in spatial resolution and complex physical processes. We present recent progress in high-resolution hydrodynamical simulations of the formation of compact massive star clusters in galactic starbursts with resolved multi-phase ISM and individually sampled stars. With accurate Nbody simulations of such compact star clusters we show that stellar and compact object collisions can result in the formation of massive black holes consistent with recent gravitational wave detections. We discuss successes and limitations of novel simulations techniques which will eventually bridge the gap between galaxy formation, interstellar medium, star formation and stellar evolution studies. Such approaches are required for a comprehensive understanding the formation of massive black holes – a fundamental science question in the era of JWST, ELT and gravitational wave detectors.Zoom: https://huji.zoom.us/j/86991266018?pwd=UWRmWDhGM3NudnhHVUJXdmQ4RnFTZz09Meeting ID: 869 9126 6018 Passcode: 537391Contact: Zhaozhou Li
- View this event in Google Calendar

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