Academic

Name	Primary Category	Discipline/Position	Phone	Office
Zalic Ayelet	Graduate Students	Condensed Matter Physics	02 6594 031	Kaplun Bldg.
Zevin Vilen	Emeriti	Condensed Matter Physics	02 6584 592	Danciger B 219
Zhang MingMing	Post-Docs	Nonlinear	02 6586 104	Levin 22
Zigler Arie	Emeriti	Atomic, Molecular and Optical Physics	02 6585 157	Marks 103
Ziskin Shlomi	Post-Docs	Astrophysics and Relativity

Upcoming Events

Yesterday

Nonlinear Physics Seminar: "How Much Memory is in the Stock Markets?"
- Start time: 12:00pm
- End date: Wednesday, March 29th
- End time: 01:30pm
- Lecturer: Thomas Guhr, Faculty of Physics, University of Duisburg-EssenAbstract:The basic models of stock markets assume purely Markoviandynamics in the stock markets, i.e. lack of memory. Thiscannot be completely true, one of the reasons being thatsome traders use strategies. We study a fully correlatedstock market and quantitatively extract the deviationsfrom purely Markovian behavior in intraday trading.Non-stationarity is one of the most important featuresof stock markets or complex systems in general. We showhow to identify and determine, on long time scales,quasistationary states of the correlated stock markets.The time evolution of the system is along trajectoriesin the space spanned by these quasistationary states.This is, on long time scales, another non-Markovianeffect.
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Today

HE astro seminar: Taeho Ryu
- Start time: 01:00pm
- End date: Thursday, March 30th
- End time: 02:00pm
- Title: Varieties of Tidal Disruption EventsAbstract: Tidal disruption events (TDEs) are one of the most dramatictransients in which a star is tidally disrupted by a supermassive blackhole, generating a flare luminous enough to outshine the entire hostgalaxy. Approximately 100 tidal disruption event candidates have beenobserved so far. In the near future, the number will grow dramaticallywith detections by the ongoing and upcoming surveys (e.g., eROSITA andLSST). The conventional picture has been that a star is fully disrupted atthe first pericenter passage and the debris circularizes rapidly, forminga compact accretion disk. However, TDEs are more diverse and they can becategorized into several groups depending on stellar pericenter distance,from partial disruptions (i.e., partial mass loss and surviving remnant)to full disruptions which is further sub-categorized depending onrelativistic effects. TDEs of each class have qualitatively differentoutcomes and reveal very distinctive debris evolution, indicatingdifferent observational features. In this talk, I will briefly explainthe physics behind TDEs and discuss the properties of the outcomesproduced in TDEs of different types and their observational implications,based on fully relativistic hydrodynamics simulations for TDEs.──────────Emanuele Sobacchi is inviting you to a scheduled Zoom meeting.Join Zoom Meetinghttps://huji.zoom.us/j/86998137272?pwd=QjB3bmxKLzA2TWM1Uk1POWlpZlpNQT09Meeting ID: 869 9813 7272Passcode: 172088One tap mobile+97223764510,,86998137272#,,,,*172088# Israel+97239786688,,86998137272#,,,,*172088# IsraelDial by your location +972 2 376 4510 Israel +972 3 978 6688 Israel +972 2 376 4509 IsraelMeeting ID: 869 9813 7272Passcode: 172088Find your local number: https://huji.zoom.us/u/kcr6DQ699kJoin by Skype for Businesshttps://huji.zoom.us/skype/86998137272──────────
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Tuesday, April 4th

Astrolunch: Salvatore Orlando
- Start time: 12:30pm
- End date: Tuesday, April 4th
- End time: 01:30pm
- Title: Connecting Supernova Remnants to their parent Supernovae and progenitor stellar systemsAbstract: The remnants of core-collapse supernovae (SNe) are diffuse extended sources with a rather complex morphology and a highly non-uniform spatial distribution of stellar debris. In young (< 5000 years) remnants, part of their features reflect the inner mechanisms of the SN engine, in particular, those determining the nucleosynthetic yields and the large-scale asymmetries left from the earliest phases of the SN explosion. Other features originate from the internal structure of the progenitor star at collapse and from the effects of remnant interaction with the circum-stellar medium (CSM) resulted from the mass-loss history of the progenitors. Hence, investigating the link between young supernova remnants (SNRs), parent SNe and progenitor massive stars can be essential: 1) to probe the physics of SN engines by providing insight into the asymmetries that occurred during the SN explosion, and 2) to investigate the endpoint in massive stars evolution and the still uncertain physical mechanisms that drive their mass-loss. Nowadays, our ability to study the progenitor-SN-SNR connection has been greatly improved thanks to three-dimensional magnetohydrodynamic models that describe the longterm evolution from the progenitor star, to the SN and to the SNR as well as to observational data of growing quality across the electromagnetic spectrum that allow to constrain the models. In this talk, I will review recent advances in modelling young to middle-aged SNRs, focusing on investigations aimed at linking the observed physical and chemical properties of SNRs to their progenitor stars and SN explosions, thus telling us about life and death of massive stars.──────────Matteo Pais is inviting you to a scheduled Zoom meeting.Join Zoom Meetinghttps://huji.zoom.us/j/88944424167?pwd=QXMrcmJNcHJaVnlYR3dtSkZCU2E1dz09Meeting ID: 889 4442 4167Passcode: 277806One tap mobile+97223764509,,88944424167#,,,,*277806# Israel+97223764510,,88944424167#,,,,*277806# IsraelDial by your location +972 2 376 4509 Israel +972 2 376 4510 Israel +972 3 978 6688 IsraelMeeting ID: 889 4442 4167Passcode: 277806Find your local number: https://huji.zoom.us/u/kdtDfNRyazJoin by Skype for Businesshttps://huji.zoom.us/skype/88944424167──────────
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