The Lecture abstracts will be announced here soon. 

  Mon
17th July
Tue
18th July
Wed
19th July
Thu
20th July
Fri
21stJuly
Sat
22nd July
Sun
23rd July
800 830   Breakfast Breakfast Breakfast Breakfast Breakfast Breakfast
830 900
900 930
930 1000 Transport Transport Excursion Transport Transport Departure
1000 1030 Opening Poster session Lecture by Vladimir Chvykov from ELI-ALPS Lecture by András László from MTA Wigner FK RMI
1030 1100 Lecture by Peter Saulson from Syracuse University NC
1100 1130 Break Break Break
1130 1200 Break Lecture by Zsolt Frei from ELTE Lecture by Subhendu Kahaly from ELI-ALPS Lecture by Márton Tápai from SZTE
1200 1230 Arrival and Registration Lecture by Peter Saulson from Syracuse University NC
1230 1300 Lunch Lunch Lunch
1300 1330 Lunch
1330 1400 Lecture by Péter Raffai from ELTE Lecture by Mousumi Upadhyay Kahaly from ELI-ALPS Lecture by Márton Tápai from SZTE
1400 1430 Lecture by Franco Frasconi from Virgo
1430 1500 Break Break Break
1500 1530 Break Lecture by Tim Pennucci from ELTE Lecture by Attila Pál Kovács from ELI-ALPS Lectures by Emma Kun from SZTE
1530 1600 Lecture by Eric Genin from Virgo
1600 1630 Transport Transport Transport
1630 1700 Transport Beach Beach Beach
1700 1730 Beach
1730 1800
1800 1830
1830 1900 Dinner Dinner Hungarian Night Dinner Dinner Dinner
1900 1930
1930 2000  
2000 2030 Welcome Party Scavenger Hunt Beach Party Free Night Farewell Party
2030 2100
2100 2130
2130 2200
2200 2230
2230

 


Lectures:

 

Tuesday:

 

The Detection of Gravitational Waves: What We’ve Learned, and Where We Go from Here [pdf]
Peter Saulson
Syracuse University NC, Department of Physics
Gravitational wave detection has now entered the era in which signals are being found. I will explain the basics of how interferometric detectors work and what limits their sensitivity. Current interferometers have worked well enough to find several black hole binaries, whose properties are interesting. Finally, I’ll give an account of what improvements are expected soon, and what new science is likely to come when those improvements are achieved.

 

Title: How can we sense a gravitational wave? [pdf]
Peter Saulson
Syracuse University NC, Department of Physics
Even though gravitational wave detectors are now finding signals, it can still be puzzling to understand how they work. In this lecture, I’ll review the history of how people figured out that gravitational waves were real and were detectable, and then trace how that understanding led to today’s detectors. The explanations will help listeners to sort out what it means to say that a gravitational wave interacts with space, with test masses, or with light, so that nothing will seem paradoxical about how a gravitational wave interferometer works.

 

Seismic noise suppression in ground based interferometric detectors for Gravitational Waves: the Advanced VIRGO Superattenuator
Franco Frasconi
Virgo Interferometer, EGO
Seismic noise is one of the limiting factor of the modern ground based interferometers for Gravitational Waves detection and observations. This noise source represents a major obstacle to the continuous operation of these complex experiments where the optical components mimic a free falling mass. Since the very beginning the INFN Pisa Group conceived the so called Superattenuator, a sophisticated mechanical structure based on the working principle of a multistage pendulum and adopted to isolate the optical components from seismic noise. With this solution the detection bandwidth of the laser interferometers has been extended in the low frequency region where many astrophysical sources are expected to emit mainly low frequency gravitational waves. In this lecture a description of the main elements of the Superattenuator together with the technological solution developed to fulfil the requirements of the second generation interferometer, Advanced VIRGO, will be presented.

 Balatonschoolv3AA.pdf

Laser interferometers to detect gravitational waves on Earth: focus on laser and optics [pdf]
Eric Genin
Virgo Interferometer, EGO
In this talk, we will introduce some aspects related to the Laser and optics employed in the giant laser interferometers aiming to detect Gravitational waves.
We will start by a description of the interferometer optical configuration required to detect Gravitational waves emitted from astrophysical objects. Then, we will go more deeply into the description of the laser and input optics system and how we can stabilize it in order not to limit the detector’s sensitivity.
Some introduction to optical cavity properties and locking will be given. In particular, the Pound-Drever-Hall locking technique will be described.
We will also explain the particular design of the Faraday isolator, a magnetooptic component widely used in the experiment. Indeed, this configuration has been introduced to keep a good isolation ratio when this device is exposed to high intensity laserradiation in an Ultra high vacuum environment.

 

Wednesday:

 

Zsolt Frei
ELTE, Nuclear Physics Department

 

Extracting astrophysical information from gravitational-wave transient detections [pdf]
Péter Raffai
ELTE, Nuclear Physics Department
During their first observing run between September 2015 and January 2016, the two detectors of Laser Interferometer Gravitational-wave Observatory (LIGO) achieved the first detections of gravitational waves from coalescences of binary black holes. As LIGO detectors continue to monitor the gravitational-wave sky with improving sensitivities, and other terrestrial detectors, such as Virgo and KAGRA, are coming online, there is a growing chance for common detections of gravitational-wave transients from more compact binary coalescences, as well as from weakly modeled or as-yet-unknown types of sources. Utilizing gravitational-wave detections in testing and constraining astrophysical models requires precise reconstructions of signal waveforms and source parameters. In my talk, I will give an introduction to the basics of how parameters of signals and sources are extracted from detections of gravitational-wave transients.

 

The Next Window — Detecting Nanohertz Gravitational Waves with Pulsar Timing Arrays
Tim Pennucci
ELTE, Nuclear Physics Department
In this lecture, I will describe the history, principles, on-going efforts, and most recent results of the pulsar timing array (PTA) community, which is an international group of astrophysicists who will open the next window onto the gravitational wave (GW) universe, at nanohertz frequencies. Millisecond pulsars (MSPs) are rapidly rotating neutron stars that have such predictably stable radio emission that they function as laboratory clocks. By observing a network of dozens of MSPs across the galaxy over decades-long timing scales, a PTA detector is sensitive to nanohertz gravitational wave perturbations with strain amplitudes below ~1e-15. The unresolved ensemble background of coalescing supermassive black hole binaries across the universe, as well as individually nearby, strong binaries, are expected to produce the first detected signals, which can constrain astrophysical models of hierarchical galaxy and black hole formation. There are three large, mature PTA efforts across the globe (NANOGrav, the EPTA, and the PPTA), which expect to make these first detections in the next several years. Alongside the kilohertz GW band of ground-based laser interferometers, like LIGO and Virgo, and the expected millihertz GW band of space-based interferometers like eLISA, PTAs help fill out the spectrum of the burgeoning field of GW astrophysics.

 

Friday:

 

Ultra-High Power Lasers: Principles, Modern Conditions and Perspectives
Vladimir Chvykov
ELI-ALPS, High Field Laser Group
During the past three decades, the short laser pulse generation technology experienced a huge progress which allowed to reduce the pulse duration from tens of nanosecond (10-9 s) to femtoseconds (10-15 s), that means seven orders of the total reduction. At the same time, the development of amplification technique made possible to accumulate significant energy in these very short pulses and achieved the several PW (1015 Watt) peak power. On the other hand, the application of adaptive optics principles to these laser systems allowed to concentrate this energy into very small volume (about 1 μm) and reach such way the intensity of more than 1022 W/cm2 , highest in the known universe. A fascinating story of these investigations will be presented in the lecture.

 

Mirrors and Lenses Generated with Ultrafast Light: the Quest for the Shortest Pulse and the Shortest Accelerator
Subhendu Kahaly
ELI-ALPS, Surface Plasma Attosource Group
Mirrors and lenses are the most fundamental optical elements that are used to enhance our domain of visual observation to render phenomena within the limits of human sense perceptions. These were invented much before Albert Einstein discovered special theory of relativity in 1905. The microscopic understanding rests on the physics of how light interacts with charged particles that constitute the matter forming the reflecting (mirrors) or refracting (lenses) material. Light, sufficiently intense and brief, can turn these passive optics into ‘relativistic’ dynamic objects opening the doors to tremendous potentials of nonlinear science making possible the generation of the shortest pulses and implementations of the smallest accelerators with enormous scientific and societal applications. Currently the extreme intensities achievable with high-power, high-contrast, state of the art femtosecond lasers have enabled one to reach this domain where light drives charged particles into relativistic motion on ultrafast timescales allowing simultaneous control of the spatio-spectral properties of both the light beam itself and the particle bunches during the interaction. This has recently opened a novel route to compact particle accelerators and coherent X-ray sources from solid surfaces. I would introduce the topic motivating the students to the current state of the art in the field culminating in some very recent experimental results that permits measurements on the laboratory scale that allows for mimicking scenarios present under extreme astrophysical conditions.

 

Probing the Structure and Dynamics of Materials with Laser
Mousumi Upadhyay Kahaly
ELI-ALPS, Computational and Applied Materials Science Group
Modern technology entails the manipulation of matter on ultrashort scales, and measurement of the dynamic processes in ultrafast domain. Thus “ultrafast science” impacts multiple areas of modern physics, chemistry, biology, materials science, engineering etc. Formation and breaking of chemical bonds occur in femtosecond time scale, and thus, elementary molecular processes can be observed and utilised by freezing the transition states of chemical processes at ultrashort time scale, even shorter than the vibrational and rotational periods in matter. Along with the technological advances, ultrafast lasers, such as in ELI-ALPS, are employed to probe the molecular systems, to understand their time evolution and, to investigate intricate details of the time-resolved behavior of matter. However limitations in controlling the experimental parameters and data processing require theoretical tools to support and complement while probing the evolution of the electronic structures post controlled excitation in the time domain. In the presentation, we will discuss structure-function relationships in materials using first principles quantum mechanical calculations based on density functional theory and time dependent density functional theory, touching upon different aspects of novel material synthesis, energetics, lower dimensional systems, organometallic substances etc. In this presentation, we will discuss some applications of such controlled excitations (laser) on materials. From an electronic perspective, we will see, how theoretical modeling can be efficiently used to explain/predict materials functionalities and responses, with specific focus on their physical properties under interaction with electromagnetic fields.

 

Laser Interferometry
Attila Pál Kovács
ELI-ALPS, Optical Preparatory Workshop
Since the first demonstration of the interferometer made by A. A. Michelson in the 1880s, interferometry has become a widely used technique in science and industry. Interferometers can be illuminated by either coherent – laser light – or incoherent light. In this lecture first a short introduction will be given about the interferometers and how interferograms in the temporal or the frequency domains are generated. Then the measurement of small displacements of the interferometer mirrors using monochromatic laser beams will be presented. A new application of this method is the interferometric detection of gravitational waves. In the next part I am going to talk about the details of surface profilometry. In the last part of the lecture the results of another interesting application will be presented, when ultrashort laser pulses are directed into an interferometer instead of monochromatic laser beams and various optical elements are placed in the sample arm of the interferometer. In this case the effect of the dispersion of the optical elements on the temporal shape of the pulse can be determined from the interferograms. If the interferometer is empty and nonlinear light detection is used, the temporal shape of the laser pulses can be measured by the evolution of the interferograms.

 

Saturday:

 

András László
MTA Wigner Research Centre for Physics

 

Márton Tápai
SZTE, Department of Experimental Physics

 

Emma Kun
SZTE, Department of Experimental Physics