A Hybrid Onsite-Online Conference 4 th LeCosPA International Symposium Unity of Physics- From Plasma Wakefields to Black Holes NTU, Taiwan. Nov. 29- Dec. 3, 2021
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AHybridOnsite-OnlineConference
4th LeCosPA InternationalSymposium
UnityofPhysics-FromPlasmaWakefieldstoBlackHoles
NTU,Taiwan.Nov.29- Dec.3,2021
1
A Hybrid Onsite-Online Conference
4th LeCosPA International Symposium
Unity of physics-From Plasma Wakefields to Black Holes
Chee-Chun Leung Cosmology Hall, National Taiwan University Taipei, Taiwan
19:00-23:00 (GMT+8), Nov. 29- Dec. 3, 2021
Sponsoring Organization and Institutions
2
4th LeCosPA Symposium Program
Time/Date
(Taipei Time) 11/29/2021 (Mon.) 11/30/2021 (Tue.) 12/01/2021 (Wed.) 12/02/2021(Thu.) 12/03/2021(Fri.)
18:00-19:00
Registration
At B1 Auditorium
Welcome Reception
At 7F Lobby
Symposium Help Center
Symposium
Banquet
At JM Cafe&Bistro
(Start at 17:00)
Session Chair
Pisin Chen
Session Chair
Kin-Wang Ng
Session Chair
Hideaki Takabe
Session Chair
Yuan-Hann Chang
Session Chair
Stathes Paganis
19:00-19:25 Joseph Silk Misao Sasaki Gerard Mourou Ue-Li Pen John Ellis
19:25-19:50 Alexei Starobinsky Sang-Pyo Kim Bernhard Hidding Remo Ruffini Antonino Marciano
19:50-20:15 Feng-Li Lin Rong-Gen Cai Tae Moon Jeong Bin Wang Jun’ichi Yokoyama
20:15-20:35 Hsu-Wen Chiang Chiang-Mei Chen Fabio Scardigli Mariam
Bouhmadi-Lopez Keisuke Izumi
20:35-20:55 Enea Romano Andrea Addazi Yen Chin Ong Taotao Qiu Yu- Hsien Kung
20:55-21:05 Coffee Break
Session Chair
Pisin Chen
Session Chair
Chiang-Mei Chen
Session Chair
Jyhpyng Wang
Session Chair
Ue-Li Pen
Session Chair
Feng-Li Lin
21:05-21:25 Che-Yu Chen Reggie Bernardo Kuan-Nan Lin Yifu Cai Michael Good
21:25-21:45 Frank Zimmermann Cong Zhang Lance Labun Debaprasad Maity Shih-Yuin Lin
21:45-22:10 Anzhong Wang Kin-Wang Ng Masahiro Hotta Jiwoo Nam Jeff Steinhauer
22:10-22:35 Chan Joshi Don Page Patric Muggli Albrecht Karle Pisin Chen
22:35-23:00 Barry Barish Dong-han Yeom Johann Rafelski Chao-Lin Kuo Bill Unruh
3
Monday, Nov. 29, 2021
Time (Taipei Time) Program
18:00-19:00 Registration at B1 Auditorium/ Welcome Reception at 7F Lobby
B1 Auditorium Plenary Session Chair: Pisin Chen
19:00-19:25 Joseph Silk (IAP, JHU, Oxford): “Knowing when to Stop”
19:25-19:50 Alexei Starobinsky (Landau Institute for Theoretical Physics, Moscow, Russia ): “Generating peaks and throughs in primordial perturbation power spectra”
19:50-20:15 Feng-Li Lin (Natl. Taiwan Norm U.): “Applications of Machine Learning to Gravitational Wave Data Analysis”
20:15-20:35 Hsu-Wen Chiang (LeCosPA, National Taiwan University): “How do we pluck the hair after it has grown?”
20:35-20:55 Enea Romano (University of Antioquia): “Deep learning merger masses estimation from gravitational waves signals in the frequency domain”
20:55-21:05 Coffee Break
B1 Auditorium Plenary Session Chair: Pisin Chen
21:05-21:25 Che-Yu Chen (Institute of Physics, Academia Sinica): “Black Hole Quasinormal Modes in GR and Beyond”
21:25-21:45 Frank Zimmermann (European Council for Nuclear Research): “Storage rings as detectors or sources of gravitational waves?”
21:45-22:10 Anzhong Wang (Baylor University): “Testing Gravitational Theories with Broken Lorentz Symmetry by Gravitational Wave and Black Hole Observations”
22:10-22:35 Chandrashekhar Joshi (University of California, Los Angeles) “Perspectives on Beam-Driven Plasma-Based Acceleration
22:35-23:00 Barry Barish (Caltech and UC Riverside) “Probing the Universe with Gravitational Waves”
4
Tuesday, Nov. 30, 2021
Time (Taipei Time) Program
B1 Auditorium Plenary Session Chair: Kin-Wang Ng
19:00-19:25 Misao Sasaki (Kavli IPMU, U Tokyo/LeCosPA, NTU): “Cosmology of Primordial Black Holes and Gravitational Waves”
19:25-19:50 Sang Pyo Kim (Kunsan National University): “Magnetic Monopoles and Black Holes”
19:50-20:15
Rong-Gen Cai (Institute of Theoretical Physics, Chinese Academy of Sciences): “No Cauchy horizon theorem of hairy black holes”
20:15-20:35 Chiang-Mei Chen (National Central University): “Schwinger Effect in Near Extremal KN-(A)dS Black Holes”
20:35-20:55 Andrea Addazi (Fudan University): “Primordial black holes from modified supergravity”
20:55-21:05 Coffee Break
B1 Auditorium Plenary Session Chair: Chiang-Mei Chen
21:05-21:25 Reggie Bernardo (Institute of Physics, Academia Sinica): “Progress on well-tempered cosmology: new teleparallel extensions and observational status”
21:25-21:45 Cong Zhang (University of Warsaw): “Loop quantum Schwarzschild interior and black hole remnant”
21:45-22:10 Kin-Wang Ng (Academia Sinica): “Latest observational results on the stochastic gravitational-wave background”
22:10-22:35 Don Page (The University of Alberta) “Black hole information”
22:35-23:00 Dong-han Yeom (Pusan National University): “Solving information loss paradox via Euclidean path integral”
5
Wednesday, Dec. 1, 2021
Time (Taipei Time) Program
B1 Auditorium Plenary Session Chair: Hideaki Takabe
19:00-19:25 Gerard Mourou (DAER-IZEST, Ecole Polytechnique): “Femto-attosecond Plasma Physics for Clean Abundant, Safe Nuclear Energy Production”
19:25-19:50 Bernhard Hidding (University of Strathclyde & Cockcroft Institute): “Trapped in plasma wakefields -- ultradense beams in 6D phase space”
19:50-20:15
Tae Moon Jeong (ELI-Beamlines, Institute of Physcis): “Formation of ultra-strong electromagnetic field through 4𝝅-spherical focusing scheme and Its application to nonlinear quantum electrodynamics”
20:15-20:35 Fabio Scardigli (Politecnico di Milano & Institute Lorentz, Leiden): “Bekenstein bound and uncertainty relations”
20:35-20:55 Yen Chin Ong (Center for Gravitation and Cosmology, Yangzhou University): “Primordial Black Hole Remnant Dark Matter and Hawking Radiation Recoil”
20:55-21:05 Coffee Break
B1 Auditorium Plenary Session Chair: Jyhpyng Wang
21:05-21:25 Kuan-Nan Lin (LeCosPA, National Taiwan University): “Analog Hawking radiation via relativistically flying mirrors”
21:25-21:45 Lance Labun (University of Taxes, Austin): “Kinematically enhancing the signal of strong-field pair production”
21:45-22:10 Masahiro Hotta (Tohoku University) “General partner formula in 1+1 dimensional moving mirror models”
22:10-22:35 Patric Muggli (Max Planck Institute for Physics): “AWAKE: physics and plans towards applications to high-energy physics”
22:35-23:00 Johann Rafelski (The University of Arizona): “Strong Field Report”
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Thursday, Dec. 2, 2021
Time (Taipei Time) Program
B1 Auditorium Plenary Session Chair: Yuan-Hann Chang
19:00-19:25 Ue-Li Pen (Institute of Astronomy and Astrophysics, Academia Sinica): “A brief history of FRBs and the future through BURSTT”
19:25-19:50 Remo Ruffini (ICRANet, ICRA, INAF): “What is the role of the rotational energy extraction from Black Holes”
19:50-20:15 Bin Wang (Center for Gravitation and Cosmology, Yangzhou University): “21cm intensity mapping: A new window to probe the DE.”
20:15-20:35 Mariam Bouhmadi- Lopez (University of the Basque Country): “On our way to describe the unseen: dark energy, black holes and wormholes
20:35-20:55 Taotao Qiu (Huazhong University of Science and Technology): “Confronting Inflation Models with the Observations on Primordial Gravitational Waves”
20:55-21:05 Coffee Break
B1 Auditorium Plenary Session Chair: Ue- Li Pen
21:05-21:25 Yifu Cai (University of Science and Technology): “Beating the Lyth bound during inflation in a resonant universe”
21:25-21:45 Debaprasad Maity (Indian Institute of Technology Guwahati): “Dynamics of reheating and it observable effects”
21:45-22:10 Jiwoo Nam (LeCosPA, National Taiwan University): “The TAROGE-M Project, A Rapid Probing of ANITA’s Anomalous Upward-moving Air-showers.”
22:10-22:35 Albrecht Karle (University of Wisconsin-Madison): “Exploring the cosmic neutrino sky at the highest energies.”
22:35-23:00 Chao-Lin Kuo (Stanford University): “Narrowing in on Inflation and Dark Matter – a microwave perspective”
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Friday, Dec. 3, 2021
Time (Taipei Time) Program
18:00-19:00 Symposium Banquet at JM Cafe&Bistro (Start at 17:00)
B1 Auditorium Plenary Session Chair: Stathes Paganis
19:00-19:25 John Ellis (King's College London): “Tracking Cosmic Strings: from NANOGrav to Atom Interferometers”
19:25-19:50 Antonino Marciano (Fudan University): “Renormalization Group a la Ricci flow: towards a Stochastic Quantization of Gravity”
19:50-20:15 Jun'ichi Yokoyama (The University of Tokyo): “Quantum correction to the inflationary power spectrum”
20:15-20:35 Keisuke Izumi (Nagoya University): “Area bound for surfaces in weak gravity region”
20:35-20:55 Yu-Hsien Kung (National Center for Theoretical Science, Physics Division): “Modified Teleparallel Gravity induced by quantum fluctuations”
20:55-21:05 Coffee Break
B1 Auditorium Plenary Session Chair: Feng-Li Lin
21:05-21:25 Michael Good (Nazarbayev University): “Energy radiated by jumping to hyperspace”
21:25-21:45 Shih-Yuin Lin (National Changhua University of Education): “A nearly black star may look like a 2D object”
21:45-22:10 Jeff Steinhauer (Physics Department, Technion): “Observation of stationary spontaneous thermal Hawking radiation, and the time evolution of an analogue black hole”
22:10-22:35 Pisin Chen (LeCosPA, National Taiwan University): “AnaBHEL (Analog Black Hole Evaporation via Lasers)”
22:35-23:00 Bill Unruh (University of British Columbia and CIFAR): “Measurement of acceleration radiation in BEC”
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Presentation Titles and Abstracts
Plenary
9
Knowing when to stop
Joseph Silk IAP, JHU, Oxford
When do we stop an ongoing science project to make room for something new? Decision-making is a complex process, ranging from budgetary considerations and tension between ongoing projects, to progress assessments and allowance for novel science developments. I will give examples of novel future projects in astronomy that could explore new frontiers yet potentially be feasible by going beyond traditional budgetary limitations.
10
Generating peaks and throughs in primordial perturbation
power spectra Alexei Starobinsky
Landau Institute for Theoretical Physics, Moscow, Russia
At the present state-of-the-art, the simplest inflationary models, based either on scalar fields in General Relativity or on modified f(R) gravity, which produce the best fit to all existing observational data, require only one dimensionless parameters taken from observations. These models include the pioneer R+R^2 one [1], the Higgs model, and the mixed R^2 - Higgs model that has been shown to be effectively one-parameter, too. They predict scale-free and close to scale-invariant power spectra of primordial scalar perturbations and gravitational waves generated during inflation. Their target prediction for the tensor-to-scalar ratio is r=3(1-n_s)^2 = 0.004, that is still about one order of magnitude less than the present upper bound. Still future observations, in particular the discovery of primordial black holes, may prove that the primordial scalar power spectrum has additional local peaks and troughs what requires at least two new parameters. I discuss mechanisms to produce such features including the recently proposed one which arise in many-field inflation with a large non-minimal kinetic term of an inflaton field leaving inflation before its end [2]. In this case, in addition to PBHs, large peaks in the primordial tensor perturbation spectrum at small scales are generated, too, in the second order of scalar perturbations. As for local non-scale-free features at cosmological scales suggested by features in the CMB temperature anisotropy for l = 2 and in the range l = 20-40, the total present CMB data including polarization do not favor them, but are not able to exclude them completely, too [3]. 1. A. A. Starobinsky, Phys. Lett. B 91, 99 (1980). 2. M. Braglia, D. K. Hazra, F. Finelli, G. F. Smoot, L. Sriramkumar, A. A. Starobinsky. JCAP 2008, 001 (2020); arXiv:2005.02895. 3. D. K. Hazra, D. Paoletti, I. Debono, A. Shafieloo, G. F. Smoot, A. A. Starobinsky, arXiv:2107.09460.
11
Applications of Machine Learning to Gravitational Wave Data Analysis Feng-Li Lin
Natl. Taiwan Norm U.
In this talk I will talk about two recent works of my group by applying the machine learning method to gravitational wave data analysis. We adopt a framework of machine learning called conditional (variational) autoencoder to help boost the data analysis in detecting the compact binary coalescences from LIGO/Virgo/KAGRA observational data. The first work is about generating the gravitational waveforms by unsupervised learning, and the second work is about performing Bayesian data analysis against the noise drifting. We find that the conditional autoencoder machine can accelerate both processes significantly with high accuracy comparable to the conventional methods.
12
Storage rings as detectors or sources of gravitational waves? Frank Zimmermann
European Council for Nuclear Research
Based on the 2021 ARIES workshop “Storage Rings and Gravitational Waves” (SRGW2021), I review history and prospects for using accelerators as tools to detect or generate gravitational waves.
13
Deep learning merger masses estimation from gravitational waves signals
in the frequency domain Enea Romano
University of Antioquia
Detection of gravitational waves (GW) from compact binary mergers provides a new window into multi-messenger astrophysics. The standard technique to determine the merger parameters is matched filtering, consisting in comparing the signal to a template bank. This approach can be time consuming and computationally expensive due to the large amount of experimental data which needs to be analyzed. In the attempt to find more efficient data analysis methods we develop a new frequency domain convolutional neural network (FCNN) to predict the merger masses from the spectrogram of the detector signal, and compare it to time domain neural networks (TCNN). Since FCNNs are trained using spectrograms, the dimension of the input is reduced as compared to TCNNs, implying a substantially lower number of model parameters, and consequently less over-fitting. The additional time required to compute the spectrogram is approximately compensated by the lower execution time of the FCNNs, due to the lower number of parameters. In our analysis FCNNs show a slightly better performance on validation data and a substantially lower over-fit, as expected due to the lower number of parameters, providing a new promising approach to the analysis of GW detectors data, which could be further improved in the future by using more efficient and faster computations of the spectrogram.
14
Black Hole Quasinormal Modes in GR and Beyond Che-Yu Chen
Institute of Physics, Academia Sinica
Quasinormal modes (QNMs) of perturbed black holes are tightly related to the gravitational wave signals emitted during the post-merger phase of a binary black hole coalescence. One of the intriguing features of these modes is that their spectra respect the no-hair theorem, and hence, can be used to test black hole spacetimes and the underlying gravitational theory. In this talk, I will exhibit three different aspects of how black hole QNMs could be altered in theories beyond Einstein’s general relativity (GR). They are (i) the shift of QNM spectra with respect to GR counterparts, (ii) the violation of the geometric correspondence between the high-frequency QNMs and the photon geodesics around the black hole, and (iii) the violation of the isospectrality between the axial and polar gravitational perturbations. Some examples will be provided in each individual case.
15
How do we pluck the hair after it has grown? Hsu-Wen Chiang
LeCosPA, National Taiwan University
We now know how soft hairs, or more precisely, not-so-soft hairs, are implanted on the horizon, how they affect the Hawking radiation and quasi-normal modes, how they are part of the long-lasting degrees of freedom on the horizon, all within the framework of general relativity plus quantum field theory in curved spacetime. The next question that needs answering is precisely the opposite of what was done before. Is there a process that allow us to pluck all hairs before the black hole evaporates into nothing?
16
Testing Gravitational Theories with Broken Lorentz Symmetry by
Gravitational Wave and Black Hole Observations Anzhong Wang
Baylor University
Observations of gravitational waves (GWs) will soon become routine, and their applications to understanding fundamental physics just start. One of such applications is to test gravitational theories. In this talk, I shall present our recent studies on testing Einstein-aether theory by GW and black hole observations. In particular, I shall show that the GW and black hole observations already reduce the four free coupling constants of the theory to two, and future observations of GWs and black holes shall further reduce the parameter space of the theory. Einstein-aether theory is a particular type of the general vector-tensor theory, in which the vector field is timelike and unity, so it defines a preferred direction. As a result, it locally breaks the Lorentz symmetry. Yet, it is self-consistent (free of ghosts, instabilities, and so on), and is consistent with all the observations and experiments. Its Cauchy problem is also well imposed. In addition, due to the presence of the aether, three different species of gravitons, the spin-0, spin-1, and spin-2, exist. This will bring dramatical differences especially in the strong-field regime.
17
Perspectives on Beam-Driven Plasma-Based Acceleration Chandrashekhar Joshi
University of California, Los Angeles Particle accelerators have been engines of discovery in our understanding of the Universe and have applications in many areas of modern life from medicine to security. The most powerful ones are 10’s of kilometers in length, determined by the strength of the accelerating electric field. It has been four decades since the concept of using a relativistic plasma wake for charged particle acceleration was first proposed. In relativistic plasma wakes the accelerating electric field can be orders of magnitude greater than in a conventional accelerator with the potential to reduce the size of the accelerating structure. The driver for producing such wakes can be in intense laser pulse or a high current charged-particle beam. In this talk I will give a personal perspective on the progress of the field of plasma-based acceleration driven by ultrashort electron bunches and where it is headed.
18
Probing the Universe with Gravitational Waves Barry Barish
Caltech and UC Riverside
The discovery of gravitational waves, predicted by Einstein in 1916, is enabling both important tests of the theory of general relativity, and the birth of a new astronomy. Modern astronomy, using all types of electromagnetic radiation, is giving us an amazing understanding of the complexities of the universe, and how it has evolved. Now, gravitational waves and neutrinos are beginning to give us the opportunity to pursue some of the same astrophysical phenomena in very different ways, as well as to observe phenomena that cannot be studied with electromagnetic radiation. The detection of gravitational waves and the emergence and prospects for this exciting new science will be explored.
19
Cosmology of Primordial Black Holes and Gravitational Waves Misao Sasaki
Kavli IPMU, U Tokyo/LeCosPA, NTU
After briefly reviewing what primordial black hokes are and how they may have formed, some recent topics will be discussed in particular in the context of gravitational wave cosmology.
20
Magnetic Monopoles and Black Holes Sang Pyo Kim
Department of Physics, Kunsan National University, 54150, Kunsan, South Korea
Dirac monopoles symmetrize the Maxwell theory and explain the quantization of electric charges. The non-Abelian theories predict monopoles such as ‘t Hooft-Polyakov monopoles. The Einstein-Maxwell theory has black hole solutions with electric and/or magnetic charges, known as Reissener-Nordstrom black holes and Kerr-Newman black holes both in the asymptotic flat space and the (anti-) de Sitter space. The Einstein-Yang-Mills theory also has black solution with monopoles in non-Abelian gauge theories. In this talk, we study the ultra-compact object and black holes with magnetic monopoles or charges in the early universe. Binaries of monopoles and antimonopoles or black holes with magnetic charges would have been formed in the early universe. The dynamics of binary systems with magnetic charges differs from that without any magnetic charges. Black holes with magnetic charges emit Hawking radiation from nonextremal ones and produce monopole pairs from near-extremal ones beyond the Breitenlohner-Freedman bound. We discuss possibility of black holes or ultracompact objects with magnetic charges as dark matter and then explore the characteristic properies of electromagnetic and gravitational radiations from those binaries and discuss possible observations.
21
No Cauchy horizon theorem of hairy black holes Rong-Gen Cai
Institute of Theoretical Physics, Chinese Academy of Sciences
We present a no inner-horizon theorem for black holes with charged scalar hairs. We prove that there exists no inner Cauchy horizon for both spherical and planar black holes with non-trivial scalar hair. The hairy black holes approach to a spacelike singularity at late interior time. This result is independent of the form of scalar potentials as well as the asymptotic boundary of spacetimes. We prove that the geometry near the singularity takes a universal Kasner form when the kinetic term of the scalar hair dominates, while novel behaviors different from the Kasner form are uncovered when the scalar potential become important to the background. For the hyperbolic horizon case, we show that hairy black hole can only has at most one inner horizon, and a concrete example with an inner horizon is presented. All these features are also valid for the Einstein gravity coupled with neutral scalars. We also consider the case of charged black holes with vector hairs.
22
Schwinger Effect in Near Extremal KN-(A)dS Black Holes Chiang-Mei Chen
National Central University
We study the Schwinger effect in the (near-)extremal Kerr-Newman-(A)dS black hole. The near-horizon region of the (near-)extremal black hole has a warped AdS geometry, which leads to the exact solutions of charges in terms of the known function. We find the mean number for the emission of electric and/or magnetic charges from the (near-)extremal KN black hole in the (A)dS space. The emission formula has a universal factorization of the Schwinger formula in the AdS2 and another Schwinger formula in the two-dimensional Rindler space determined by the effective temperature and the Hawking temperature with the chemical potentials of electric and magnetic charges and rotation. The emission of the same species of charges from the KN black hole is enhanced in the dS boundary while it is suppressed in the AdS boundary.
23
Primordial black holes from modified supergravity Andrea Addazi
Fudan University
We explore the Gravitational Waves (GW) phenomenology of a simple class of supergravity models that can explain and unify inflation and Primordial Black Holes (PBH) as Dark Matter (DM). Our (modified) supergravity models naturally lead to a two-field attractor-type double inflation, whose first stage is driven by Starobinsky scalaron and the second stage is driven by another scalar belonging to a supergravity multiplet. The PBHs formation in our supergravity models is efficient, compatible with all observational constraints, and predicts a stochastic GW background. We compute the PBH-induced GW power spectrum and show that GW signals can be detected within the sensitivity curves of the future space-based GW interferometers such as LISA, DECIGO, TAIJI and TianQin projects, thus showing predictive power of supergravity in GW physics and their compatibility.
24
Progress on well-tempered cosmology: new teleparallel extensions and
observational status Reggie Bernardo
Institute of Physics, Academia Sinica
Well-tempering is a promising mechanism for dark energy to screen an arbitrarily large cosmological constant and deliver a late-time, low energy vacuum state. We briefly review well-tempered cosmology and discuss recent progress on its teleparallel gravity extensions. We look at the theoretical features that dark energy may hold in order to be well-tempered and report on the observational status of well-tempered cosmology.
25
Loop quantum Schwarzschild interior and black hole remnant Cong Zhang
University of Warsaw
The interior of Schwarzschild black hole is quantized by the method of loop quantum gravity. The Hamiltonian constraint is solved and the physical Hilbert space is obtained in the model. The properties of a Dirac observable corresponding to the ADM mass of the Schwarzschild black hole are studied by both analytical and numerical techniques. It turns out that zero is not in the spectrum of this Dirac observable. This supports the existence of a stable remnant after the evaporation of a black hole. Our conclusion is valid for a general class of schemes adopted for loop quantization of the model.
26
Latest observational results on the stochastic gravitational-wave
background Kin-Wang Ng
Institute of Physics, Academia Sinica
Recently pulsar-timing observations have found strong evidence of a stochastic common-spectrum process across millisecond pulsars, alluding to a stochastic gravitational-wave background at nanohertz frequencies. We discuss the implications of the pulsar-timing-array results and other current constraints by CMB, astrometric, and interferometric measurements.
27
Black hole information Don Page
University of Alberta
Black hole information is one of the greatest puzzles of theoretical physics from the 20th century that has persisted into the 21st century. After Stephen Hawking discovered black hole evaporation in 1974, in 1976 he predicted that black hole formation and evaporation would cause a pure quantum state to change into a mixed state, effectively losing information from the universe. In 1979 I questioned this conclusion, as many years later did many others, and in 2004 Hawking conceded that black hole evaporation does not lose information. However, a minority of gravitational theorists have not accepted Hawking's concession. There do remain many puzzles about black hole information, such as how it gets out (if it indeed does), but there has been much recent progress on this puzzle.
28
Solving information loss paradox via Euclidean path integral Dong-han Yeom
Pusan National University
The information loss paradox associated with black hole Hawking evaporation is an unresolved problem in modern theoretical physics. In this paper, we revisit the entanglement entropy via the Euclidean path integral (EPI) of the quantum state and allow for the branching of semi-classical histories along the Lorentzian evolution. We posit that there exist at least two histories that contribute to EPI, where one is an information-losing history while the other is information-preserving. At early times, the former dominates EPI, while at late times the latter becomes dominant. By so doing we recover the essence of the Page curve and thus the unitarity, albeit with the turning point, i.e., the Page time, much shifted toward the late time. One implication of this modified Page curve is that the entropy bound may thus be violated. We comment on the similarity and difference between our approach and that of the replica wormholes and the island conjecture.
29
Femto-attosecond Plasma Physics for Clean Abundant, Safe Nuclear
Energy Production Gérard Mourou and Jonathan Wheeler DAER-IZEST, Ecole Polytechnique
Common forms of renewable energy will not be enough to sustain our way of life. Nuclear energy is our only realistic option. In this presentation, I will describe a new kind of nuclear energy based on the thorium cycle that will produce less toxic waste and last several thousand years. In many ways, thorium is a superior alternative to uranium for energy production. It is three times more abundant, with much less and much shorter-lived waste. Also being widely spread and difficult to be used for plutonium production, makes thorium unattractive to military applications. Our scheme is based on extreme light technologies. Single cycle high energy pulses are capable to generate efficiently high energy protons and after spallation large neutron fluxes. The neutron will produce energy via fission of the chemical element thorium. To guaranty safety, the configuration ADS (Advanced Driven Accelerator) to eliminate possible chain reaction runaway is adopted. The unique combination of extreme light with a promising nuclear material like thorium offers a new path to clean, abundant and safe energy that our society needs for its survival.
30
Trapped in plasma wakefields -- ultradense beams in 6D phase space Bernhard Hidding
University of Strathclyde & Cockcroft Institute
Plasma wakefields can accelerate electrons at Teravolt-per-meter gradients, many orders of magnitude larger than conventional accelerators. This vision [1] has become a reality and has been pioneered at the SLAC linac [2]. A further chief innovation is the plasma photocathode [3], where a laser pulse creates an ultracold electron population directly in the plasma wave via tunneling ionization. Rapid acceleration traps these electrons in the plasma wakefield and compresses them in real and phase space, and thus may enable generation of electron beams many orders of magnitude brighter than possible today. Following the first proof-of-concept realization of a plasma photocathode at SLAC [4], we now aim to produce such ultradense 6D phase space beams and to exploit them. First key applications of these ultrabright beams are already on the horizon in the form of utilizing them as drivers for ultrahard, ultrabright x-ray free-electron-lasers, or for high energy physics collider R&D. The interaction of ultrabright electron, laser and x-ray beams, in turn opens new vistas on future high energy density and QED experiments. This talk will report on the concepts, progress and prospects of these efforts, including a pathway to democratize big physics via hybrid laser-plasma wakefield accelerators [5,6]. [1] P. Chen et al., Phys. Rev. Lett. 54, 693 (1985) [2] I. Blumenfeld et al., Nature 445, 741–744 (2007) [3] B. Hidding et al., Phys. Rev. Lett. 108, 035001 (2012) [4] A. Deng et al., Nature Phys. 15, 1156–1160 (2019) [5] B. Hidding et al., Phys. Rev. Lett. 104, 195002 (2010) [6] T. Kurz et al., Nature Comm. 12, 2895 (2021)
31
Formation of ultra-strong electromagnetic field through 4𝝅-spherical
focusing scheme and Its application to nonlinear quantum
electrodynamics Tae Moon Jeong
Institute of Physics ASCR, v.v.i. (FZU), ELI-Beamlines Project, 182 21 Prague, Czech Republic
Femtosecond high-power lasers based on Chirped Pulse Amplification technique, which recently reached a peak intensity 1023 W/cm2 [1], have a wide range of applications in light-matter interactions [2, 3]. With the advance of such a high-power laser, much attention has been paid to light-vacuum interactions (known as the strong-field quantum electrodynamics), such as vacuum birefringence, light-light scattering, electron-positron pair creation in vacuum, and so on. These phenomena require ultra-high laser intensities (or laser field strength known as the Schwinger field) corresponding to ~1029 W/cm2. Tight-focusing of a laser pulse by a low f-number (1/3) focusing optics is employed to obtain a laser intensity of > 1025 W/cm2 through the l 3 scheme with ~80 PW laser [4-6]. The 4 p
-spherical focusing scheme [7,8], as a limiting case of the tight focusing scheme or the multiple laser pulse focusing scheme [9], can be also employed to obtain the theoretical limit of the focused intensity. The field configurations under the 4 p-spherical focusing scheme were analytically formulated with the radially- and azimuthally- polarized laser pulse [8], and it has been applied to the study of electron-positron pair creation [8], light-light scattering [10], and the intensification of electromagnetic radiation through the relativistic-flying parabolic mirror [11]. In this talk, we present the formation of ultra-strong electromagnetic field through the 4 p-spherical focusing scheme and its application to the nonlinear quantum electrodynamics. References:
[1] J. W. Yoon, et al., Optica 8, 630 (2021).
[2] G. A. Mourou, T. Tajima, and S. V. Bulanov, Rev. Mod. Phys. 78, 309 (2006); E. Esarey, C. B. Schroeder, and W. P.
Leemans, Rev. Mod. Phys. 81, 1229 (2009); H. Daido, M. Nishiuchi, and A. S. Pirozhkov, Rep. Prog. Phys. 75, 056401 (2012).
[3] A. Di Piazza, C. Müller, K. Z. Hatsagortsyan, and C. H. Keitel, Rev. Mod. Phys. 84, 1177 (2012).
[4] T. M. Jeong, S. Weber, B. Le Garrec, D. Margarone, T. Mocek, and G. Korn, Opt. Express 23, 11641 (2015).
[5] T. M. Jeong, S. V. Bulanov, S. Weber, and G. Korn, Opt. Express 26, 33091 (2018).
[6] P. Hadjisolomou, T. M. Jeong, P. Valenta, G. Korn, and S. V. Bulanov, Phys. Rev. E 104, 015203 (2021).
[7] I. Gonoskov, A. Aiello, S. Heugel, and G. Leuchs, Phys. Rev. A 86, 053836 (2012).
[8] T. M. Jeong, S. V. Bulanov, P. V. Sasorov, S. S. Bulanov, J. K. Koga, and G. Korn, Opt. Express 28, 13991 (2020).
[9] S. S. Bulanov, V. D. Mur, N. B. Narozhny, J. Nees, and V. S. Popov, Phys. Rev. Lett. 104, 220404 (2010).
[10] T. M. Jeong, S. V. Bulanov, P. V. Sasorov, G. Korn, J. K. Koga, and S. S. Bulanov, Phys. Rev. A 102, 023504 (2020).
[11] T. M. Jeong, S. V. Bulanov, P. Valenta, G. Korn, T. Zh. Esirkepov, J. K. Koga, A. S. Pirozhkov, M. Kando, and S. S.
Bulanov, arXiv:2111.04493v1 (2021) and Phys. Rev. A to appear.
Bekenstein bound and uncertainty relations
32
Fabio Scardigli Politecnico di Milano & Institute Lorentz, Leiden
The Bekenstein bound provides a universal limit on the entropy that can be contained in a localized quantum system of a given size and total energy. In this talk, we explore unsuspected links between the Bekenstein bound and the Heisenberg Uncertainty Principle. We also show how the Bekenstein bound is affected when the Heisenberg uncertainty relation is deformed so as to accommodate gravitational effects at Planck scale (Generalized Uncertainty Principle). Physical implications are discussed for both cases of positive and negative values of the deformation parameter. Ref.:arXiv:2009.12530 (to appear on PLB).
33
Primordial Black Hole Remnant Dark Matter and
Hawking Radiation Recoil Yen Chin Ong
Center for Gravitation and Cosmology, Yangzhou University
Primordial Black Hole Remnant Dark Matter and Hawking Radiation RecoilIt has recently been suggested that black hole remnants of primordial origin are not a viable dark matter candidate since they would have far too large a velocity due to the recoil of Hawking radiation. We re-examined this interesting claim in more detail and found that it does not rule out such a possibility. On the contrary, for models based on non-commutativity of spacetime near the Planck scale, essentially the same argument can be used to estimate the scale at which non-commutativity effect becomes important. If dark matter "particles" are non-commutative black holes that have passed the maximum temperature, this implies that the non-commutative scale is about 100 times the Planck length. The same analysis applies to other black hole remnants whose temperature reaches a maximum before cooling off, for example, black holes in asymptotically safe gravity.
34
Analog Hawking radiation via relativistically flying mirrors
Kuan-Nan Lin LeCosPA, National Taiwan University
It is of great challenges these days to directly detect Hawking radiation emitted by astrophysical black holes. Analog black hole systems that can be realised in laboratories have thus been developed to make the experimental studies of black holes possible. In this talk, I will introduce one of these analog models, i.e., the moving mirror radiation, and its generalisations to cope with near-future analog-black-hole-evaporation-via-lasers (AnaBHEL) experiment proposed by Chen and Mourou in 2017.
35
Kinematically enhancing the signal of strong-field pair production
Lance Labun University of Taxes, Austin
Spontaneous electron-positron pair production is a signature prediction of quantum electrodynamics in strong classical fields. Analogously to atomic ioniziation, pair production can be greatly enhanced by perturbing the high intensity field with a high frequency field. The perturbation can be provided by a coherent field, such as an XUV or x-ray laser, or by incoherent photons. A photon beam is easier to colocate and collide with a high intensity pulse but can also create pairs by scattering off e.g. nuclei in other components of the experiment. Experimentally proving the origin of produced positrons as the strong-field production mechanism calls for ways to distinguish them from background production mechanisms. Kinematics can help: Produced pairs can be boosted by the fact that a general electromagnetic field configuration has a rest frame moving relative to the lab frame.
36
General partner formula in 1+1 dimensional moving mirror models Masahiro Hotta
Tohoku University
AdS/CFT correspondence suggests unitary evolution of blackhole evaporation, but no quantum gravity theory succeeds in finding purification partners of Hawking particles yet. Moving mirror models as condensed matter analogs mimic the emission of Hawking radiation and blackhole evaporation. Since unitarity of quantum mechanics is preserved in the systems, the Hawking particles have its purification partners. In this talk, a general formula of partner modes for Hawking modes will be reviewed. This provides essential ideas about how quantum information is stored and maintained after the last burst of the blackholes.
37
AWAKE: physics and plans towards applications to high-energy physics
Patric Muggli Max Planck Institute for Physics
AWAKE [1] has demonstrated that, with self-modulation (SM), long, high-energy proton bunches can drive large amplitude wakefields in plasma [2, 3]. This includes many physics aspects of the SM process, as well as the acceleration of externally-injected MeV electrons up to 2GeV energy [3]. In addition, AWAKE has a clear science roadmap for producing by the end of the decade and in a single accelerator plasma, high-energy electron bunches suitable for particle physics applications. I will introduce AWAKE, summarize previous experimental results [3,4] and outline the roadmap.
38
Strong Field Report
Johann Rafelski Department of Physics, The University of Arizona
We describe recent advances in our understanding of classical and quantum particle dy- namics in the presence of strong electromagnetic fields. Strong fields imply strong forces and accelerations in regimes where electrodynamics becomes nonlinear and radiation ef- fects become dominant. The present understanding of the laws of physics was arrived at by observing applied forces in nano-scale regimes as measured in natural units. Therefore, we seek extensions of these laws to fully describe the strong fields physics regime. We explore unit strength acceleration in the experimentally accessible context of ultra-short pulsed lasers, and nonrelativistic and relativistic heavy-ion collisions. We connect indi- vidual classical and quantum particle dynamics with high density plasma behavior, and illustrate applications involving atomic, nuclear, and elementary particle physics in the laboratory, in astrophysics and in cosmology. The ‘acceleration frontier’ is then emerging as a novel research opportunity at the forefront of modern fundamental physics.
39
A brief history of FRBs and the future through BURSTT
Ue-Li Pen Institute of Astronomy and Astrophysics, Academia Sinica
The young field of FRBs has raised new questions on their nature. FRBs are the only extragalactic coherent extragalactic radiation source, opening their use as cosmic pulses maser. I will give a brief review of observations and theory, and an ambitious new initiative to open a new window on FRBs through BURSTT (bustling universe radio survey telescope in Taiwan).
40
What is the role of the rotational energy extraction from
Black Holes
Remo Ruffini ICRANet, ICRA, INAF
We have demonstrated that the inner engine of GRBs and AGN produces high-energy emission by synchrotron radiation of electrons/protons that are accelerated in the rotating BH vicinity. The angular momentum of the Kerr BH and the surrounding magnetic field determine the energetics and characteristic radiation frequency, and their relative direction determines whether the motion of the electrons around the magnetic field lines follows a right-handed or a left-handed helix, and likewise the angular momentum inherited by the radiation.
41
21cm intensity mapping: A new window to probe the DE. Bin Wang
Center for Gravitation and Cosmology, Yangzhou University In this talk I will go over the concept of 21cm cosmology and explain that it is a useful new window to study cosmology and understand DE.
42
On our way to describe the unseen: dark energy, black holes
and wormholes
Mariam Bouhmadi- Lopez University of the Basque Country
In the current talk, I will present some phantom dark energy modelsthat fully fit the available observational data. Those models are harmless from a quantum point of view, in the sense that the singularities or abrupt events they might induce are cured at the quantum level. In addition, some of those models can support regular blackholes as well as wormholes that do not require matter with a wrong kinetic term.
43
Confronting Inflation Models with the Observations on Primordial
Gravitational Waves
Taotao Qiu Huazhong University of Science and Technology,
The recent observations from CMB have imposed a very stringent upper-limit on the tensor/scalar ratio $r$ of inflation models, which indicates that the primordial gravitational waves (PGW) should be very tiny. However, current experiments on PGW is ambitious to detect such a tiny signal by improving the accuracy to an even higher level, and their results will provide us much information to the theoretical side such as model building. In this talk, I will discuss what kind of inflation models can be favored by future observations. Starting with a kind of general action offered by the effective field theory (EFT) approach, I give a general form of $r$ that can be reduced to various models, and I show how the accuracy of future observations can put constraints on model parameters by plotting the contours in their parameter spaces.
44
Beating the Lyth bound during inflation in a resonant universe
Yifu Cai University of Science and Technology of China
Recently, a novel mechanism for enhancing the primordial gravitational waves was proposed, which does not significantly affect the curvature perturbations produced during inflation. This is achieved due to non-linear sourcing of resonantly amplified scalar field fluctuations, and thus gives a scale-dependent counter-example of the famous Lyth bound. This hypothetical scenario opens up a promising perspective of producing detectable inflationary tensor modes with low-scale inflation and a sub-Planckian field excursion. We explicitly demonstrate the testability of our mechanism with upcoming Cosmic Microwave Background B-mode observations such as LiteBIRD.
45
Dynamics of reheating and it observable effects
Debaprasad Maity Indian Institute of Technology Guwahati
Reheating is an important phase of the early universe. This is the phase which connects inflation and standard radiation dominated phase of the universe though the decay of inflation. In this talk we will first discuss in detail about the reheating dynamics in the well-known perturbative framework. We further discuss about its observable effects on the primordial gravitational wave and large-scale magnetic field.
46
The TAROGE-M Project, A Rapid Probing of ANITA’s Anomalous
Upward-moving Air-showers Jiwoo Nam
LeCosPA, National Taiwan University
We propose a new experiment to unveil ANITA’s mysterious events. ANITA reported anomalous two upward-moving air-shower events with energies of ~0.6×10^18 eV. These events cannot be explained by the standard model and a lot of attention with various new theoretical proposals. While reproduction of these results with significant statistics is highly demanded, we propose a new rapid experiment, Taiwan astroparticle radiowave observatory for geo-synchrotron emissions in Mt. Melbourne (TAROGE-M), which is a synoptic radio array experiment on the top of high mountains in Antarctica. TAROGE-M is utilized to detect the upward moving air-showers with great advantages over ANITA, such as a lower the energy threshold, a long livetime, and extendibility. The first station consisting of 6 LPDA antennas has been installed atop Mt. Melbourne, Antarctica at an elevation of 2730 m, in Austral summer season 2019-2020, and successfully demonstrated the feasibility of the project by detecting 7 ultra-high energies cosmic ray events. We propose to install 10 stations over the next 5 years to obtain sufficient sensitivity to test ANITA’s `mystery events'. We present the scientific potential, detector design and construction, performance of the station, as well as future prospect.
47
Exploring the cosmic neutrino sky at the highest energies. Albrecht Karle
University of Wisconsin-Madison
IceCube has established the existence of a cosmic neutrino flux up to energies of 10^16 eV. At higher energies the radio detection method has emerged as the most promising technique. The Askaryan Radio Array in operation at the South Pole is currently the most sensitive detector. I will review what we have learned to date and discuss the plans for a very large radio detector array as part of the next generation neutrino detector facility: IceCube-Gen2.
48
Narrowing in on Inflation and Dark Matter – a microwave perspective Chao-Lin Kuo
Stanford University
The frontiers of fundamental physics have reached the very beginning of time, the very edge of space, and new particles/fields that fill the universe. I will review a deep connection between inflation and axion dark matter, and the efforts to shed light on the nature of both using microwave techniques. In this talk, I will focus on (1) how measurements of CMB (cosmic microwave background) E mode and B mode polarization can tell us about inflation and the axion dark matter, and (2) a novel axion dark matter detector that uses many microwave techniques from the CMB.
49
Tracking Cosmic Strings: from NANOGrav to Atom Interferometers
John Ellis King's College London
The NANOGrav pulsar timing array has reported detection of a possible stochastic common background process. If it is due to gravitational waves, they may be due to emissions from collapsing loops of cosmic strings. If so, there should be a near-constant spectrum extending to higher frequencies, which would be observed by LISA and future atom interferometer experiments and could cast light on the early expansion history of the Universe.
50
Renormalization Group a la Ricci flow: towards a Stochastic
Quantization of Gravity
Antonino Marciano Department of Physics, Fudan University
I will present results obtained in collaboration with Matteo Lulli, on a new road for the definition of the Stochastic Quantization (SQ) of the action functionals yielding Einstein’s equations. Hinging on the functional similarities between the Ricci-Flow equation and the SQ Langevin equations, we push forward a novel approach in which we the stochastic time tends to the proper time of a space-like foliation in the equilibrium limit. This procedure in turn requires adding to the usual symmetric connection a projective Weyl term that does not modify the classic equations of motion. Furthermore, we express the starting system of equations using the Arnowitt-Deser-Misner (ADM) variables and their conjugated Hamiltonian momenta. Such a choice is instrumental for understanding the newly derived equations in terms of breaking the diffeomorphism invariance of the classical theory, which will hold on average at the steady state. We finally argue that the Ricci flow equations naturally provide, in a geometrical way, the renormalization group equation for gravity theories, and comment on possible applications of this novel scenario.
51
Quantum correction to the inflationary power spectrum Jun'ichi Yokoyama
The University of Tokyo
"Four decades after its original proposal, inflationary expansion in the early Universe is now regarded as an indispensable ingredient of modern standard cosmology which not only explains fundamental properties of the global spacetime of our universe, namely, why our universe is so large, so homogeneous, and so old with full of matters, but also account for the origin of tiny density and curvature perturbations that eventually grow to all the cosmic structures we observe today. To single out the right theory in high energy physics responsible for inflation from these observation is one of the ultimate goal of the studies on inflationary cosmology. We have calculated one-loop correction to the power spectrum of curvature perturbations generated during inflation and found a nontrivial constraint on the propagation speed of these fluctuations, which may be helpful to further constrain model building."
52
Area bound for surfaces in weak gravity region Keisuke Izumi
Nagoya University
I will show a generalization of Riemannian Penrose inequality. Riemannian Penrose inequality gives an upper bound of the area of black hole, while our inequality is applicable even to a surface in a weak gravity region. On asymptotically-flat maximal spacelike 3-surfaces in general relativity, the area of minimal 2-surfaces is suppressed by that of Schwarzschild spacetime. Since, on a time-symmetric 3-surface, an apparent horizon becomes a minimal 2-surface, this upper bound must show the maximum entropy of black hole. The inequality expressing the upper bound is called Riemannian Penrose inequality. In this talk, the inequality is generalized for surfaces in generic gravitational fields where the gravity is moderately strong or even weak. It must be helpful to understand the thermodynamic properties of gravitational theory not relied on black holes. This talk is based on our paper PTEP 2021 Issue 8, 083E02 (arXiv: 2101.03860). Because of time constraints, in this talk I will show only the results and interpretation in physics, not show the proof.
53
Modified Teleparallel Gravity induced by quantum fluctuations Yu-Hsien Kung
National Center for Theoretical Science, Physics Division
In the semi-classical regime, quantum fluctuations embedded in a Riemannian spacetime can be effectively recast as classical back reactions and manifest themselves in the form of non-minimal couplings between matter and curvature. In this work, we exhibit that this semi-classical description can also be applied within the teleparallel formulation. In the teleparallel formulation, quantum fluctuations generically lead to non-minimal matter-torsion couplings. Due to the equivalence between the (classical) Einstein gravity in the Riemannian description and that in teleparallel description, some effective models which were constructed using Riemannian description can be reproduced completely using the teleparallel description. Besides, when the effective quantum correction term is proportional to the torsion scalar $T$, we obtain a subclass of novel $f(T,B,\mathcal{T})$ gravity, where $B$ is a boundary term, and $\mathcal{T}$ is the trace of the energy-momentum tensor. Next, we investigate the cosmological properties in this $f(T,B,\mathcal{T})$ theory by assuming that the matter Lagrangian is solely constructed by a dynamical scalar field. We exhibit some interesting cosmological solutions, such as those with decelerating expansion followed by a late-time accelerating phase. In addition, the non-minimal matter-torsion couplings induced by quantum corrections naturally lead to energy transfers between gravity and cosmological fluids in the universe.
54
Energy radiated by jumping to hyperspace Michael Good
Nazarbayev University
Connecting (1+1)D flying mirror radiation to (1+3)D flying mirror radiation, we account for the energy radiated by a discontinuous jump in velocity. The acceleration is a plateau line shape and a common description of radiative decay, characterizing a unitary, thermal, energy-conserved analog model for complete black hole evaporation. Information loss is avoided and negative energy flux in (1+1) D is a dimensional artifact which does not show up in (1+3)D.
55
A nearly black star may look like a 2D object Shih-Yuin Lin
National Changhua University of Education A nearly black, gravitationally intense star of semi-transparent, spherical, massive shell containing a few pointlike light sources inside would be perceived not like a three-dimensional ball for a localized observer outside the shell in terms of the affine or binocular distance. As the radius of the spherical shell approaches the Schwarzschild radius, the perceived distance between the front and rear surfaces of the shell would go to zero, while the images of most of the interior emitters would squeeze around the shell surfaces in terms of the affine or binocular distance. So, the Schwarzschild black hole formed from the star would be thought of as a two-dimensional membrane for the observers who can only measure the binocular distance and/or affine distance. However, the depth information of a point source inside the nearly black star can still be resolved in terms of the radar or luminosity distance, which needs the knowledge about the radar signals or standard candles sent in earlier by the observer outside the star. This suggests that at late times of gravitational collapse the area law of the entropy would dominate over the volume law for outside observers due to the loss of the knowledge about the ingoing probes earlier.
56
Observation of stationary spontaneous thermal Hawking radiation, and
the time evolution of an analogue black hole Jeff Steinhauer
Physics Department, Technion
We confirm that Hawking radiation from an analogue black hole is spontaneous, thermal, and stationary. Furthermore, we follow the time evolution of the Hawking radiation, and compare and contrast it with the predictions for real black holes. We observe the ramp up of the Hawking radiation, similar to a real black hole. The end of the spontaneous Hawking radiation is marked by the formation of an inner horizon. The Maryland group predicted that particles emanating from the inner horizon can cause stimulated Hawking radiation. We find that these stimulated Hawking pairs are directly observable.
57
AnaBHEL (Analog Black Hole Evaporation via Lasers) Pisin Chen
LeCosPA, National Taiwan University
Accelerating relativistic mirror has long been recognized as a viable model for BH. In 2017, Chen and Mourou proposed a novel way to realize such as system by traversing an ultra-intense laser through a plasma target with a decreasing density gradient. An international AnaBHEL (Analog Black Hole Evaporation via Lasers) collaboration has been formed with the objective to observe the analog Hawking radiation and to shed some lights on the information loss paradox. To reach this goal, it is found prudent to pursue it in three stages, where Stage-1 would be to verify the underlying physical mechanism of the flying plasma mirror, and based on that, Stage-2 would be to characterize the relationship between the density gradient of the plasma target and the trajectory of the accelerating plasma mirror. Only after we successfully performed these two stages can we be ready to finally tackle the ultimate goal at Stage-3. In this paper, we describe our vision and strategy of AnaBHEL using the Apollon laser as an example.
58
Measurement of acceleration radiation in BEC
Bill Unruh University of British Columbia and CIFAR
Relativistic quantum effects, like Hawking radiation, and acceleration temperature, are very difficult to measure directly. However, using analogs opens the possibility of measureing the effects in such systems. I will discuss the possibility of measuring the acceleration temperature in a BEC using a new type of detector, a energy laser interferometer on a circular orbit in a BEC which present the possibility that the effect could be measured.
59
Appendix
60
Participants （Onsite attendee）
Last Name First Name Institution E-mail
1 Bernardo Reginald Christian
Institute of Physics, Academia Sinica
2 Chang Un-Pang National Taiwan University [email protected]
3 Chang Che-Jui Graduate Institute of Communication Engineering, National Taiwan University
4 Chang Yuan-Hann Academia Sinica [email protected] 5 Chang Yu-Yen NCKU department of physics [email protected]
6 Chen Yaocheng LeCosPA, National Taiwan University
7 Chen Che-Yu Institute of Physics, Academia Sinica
8 Chen Wun-Yi ASIAA/NTU [email protected] 9 Chen augustine National central university [email protected]
10 Chen Yu-Jui National Taiwan University [email protected] 11 Chen Chiang-Mei National Central University [email protected] 12 Chen Ying-Chih [email protected]
13 Chiang Hsu-Wen LeCosPA, National Taiwan University
14 Chiang Cheng-Wei NTU & NCTS [email protected] 15 Chien Chen-Hsu National Taiwan University [email protected] 16 Chiu Ting-Wai National Taiwan University [email protected]
17 CHOU TZU-MIAO Institute of Applied Physics, National Taiwan University
18 Freynet Anna [email protected] 19 Huang Cheng-Tse National Taiwan University [email protected]
20 Lambaga Reyhan Dani
LeCosPA, National Taiwan University
21 Lin Chia-Min National Chin-Yi University of Technology
22 Lin Shih-Yuin National Changhua University of Education
23 Lin Kuan-Nan LeCosPA, National Taiwan University
24 Lin Yuan-Ru National Taiwan University [email protected]
25 Lin Jing-En Physics Department, National Taiwan University
61
Last Name First Name Institution E-mail 26 Lin Feng-Li Natl. Taiwan Norm U. [email protected] 27 Liu Yung-Kun National Taiwan University [email protected]
28 Liu TsungChe National Yang Ming Chiao Tung univ.
29 Liu ShuXiao LeCosPA, National Taiwan University
30 Luo Yu-Tang National Taiwan university [email protected]
31 Nam Jiwoo LeCosPA, National Taiwan University
32 Ng Kin-Wang Institute of Physics, Academia Sinica
33 Paganis Stathes National Taiwan University [email protected] 34 Patel Avani Academia Sinica [email protected]
35 Ue-Li Pen Institute of Astronomy and Astrophysics, Academia Sinica
36 Su Shih-Chieh LeCosPA, National Taiwan University
37 Sudevan Vipin LeCosPA, National Taiwan University
38 Takabe Hideaki LeCosPA, National Taiwan University
39 TSAI Anton [email protected] 40 Tseng Yen-Chu National Taiwan University [email protected] 41 Tseng Hui Yin [email protected]
42 Wang Shih-Hao LeCosPA, National Taiwan University
43 Wang Yu-Hsin LeCosPA, National Taiwan University
44 Wang Yen-Chieh Deparment of physics and LeCosPA, National Taiwan University
45 Wang Jyhpyng Academia Sinica [email protected]
46 Watamura Naoki LeCosPA, National Taiwan University
47 Wen Wen-Yu Academia Sinica [email protected] 48 Wu Siye NTHU [email protected] 49 黃 群翔 National Taiwan University [email protected]
62
Participants （Online attendee）
Last Name First Name Institution E-mail 1 Addazi Andrea Fudan University [email protected] 2 Appleby Stephen APCTP [email protected]
3 Barish Barry Caltech and UC Riverside
4 Bernardo Reggie Institute of Physics, Academia Sinica
5 Cai Yi-Fu University of Science and Technology
6 Cai Rong-Gen Institute of Theoretical Physics, Chinese Academy of Sciences
7 Chang We-Fu NTHU [email protected]
8 Chang Yu-Yen NCKU department of physics
9 Chang Yuan-Hann ACADEMIA SINICA [email protected]
10 Chen Kuan Yu National Taiwan University
11 Chen Wei-Huai NTU PHYS [email protected] 12 Cho Hing-Tong Tamkang University [email protected] 13 Domenech Guillem [email protected] 14 Das Mayusree IISc [email protected] 15 Ellis John King's College London [email protected]
16 Evans Stefan The University of Arizona, Tucson, USA
17 Felix Caroline CYCU [email protected]
18 Formánek Martin Max Plank Institute, Heidelberg, Germany
[email protected] [email protected]
19 Feng Wei-Xiang [email protected] 20 Good Michael Nazarbayev University [email protected]
21 Grayson Christopher Miller
The University of Arizona, Tucson, USA
22 Gregoris Daniele Jiangsu University of Science and Technology
23 Gwak Bogeun Dongguk University [email protected]
24 Hidding Bernhard University of Strathclyde & Cockcroft Institute
25 Ho Meng Yuan [email protected]
63
Last Name First Name Institution E-mail
26 Ho Amigo [email protected] 27 Hotta Masahiro Tohoku University [email protected] 28 Izumi Keisuke Nagoya University [email protected] 29 Jayawiguna Byo Universitas Indonesia [email protected]
30 Jeong Tae Moon ELI-Beamlines, Institute of Physcis
31 Jo Yongseok Seoul National University
32 Joshi Chandrashekhar
UCLA [email protected]
33 Karle Albrecht University of Wisconsin-Madison
34 Kim Sang Pyo Kunsan National University
35 Kim Hang Bae Hanyang University [email protected]
36 Kim Jin Young Kunsan National University
37 King Sun-Kun [email protected]
38 Kung Yu-Hsien National Center for Theoretical Science, Physics Division
39 Kuo Chao-Lin Stanford University [email protected] 40 Lenart Arpad University of Strathclyde [email protected]
41 Labun Lance University of Taxes, Austin
42 Lee Chang-Hwan Pusan National University
43 Lee Ray-Kuang National Tsing Hua University
44 Levi Said Jackson University of Malta [email protected] 45 Lin Chunshan Jagiellonian University [email protected]
46 Liu Lang Kunsan national university
47 Lopez Mariam University of the Basque Country
48 Lulli Matteo Southern University of Science and Technology
49 Maity Debaprasad Indian Institute of [email protected]
64
Technology Guwahati Last Name First Name Institution E-mail
50 Marciano Antonino Fudan University [email protected]
51 Ming Yin Sam
Wong National Taiwan University
52 Mondal Sayid Chung Yuan Christian University
53 Moreira Delgado
Paola Carolina
Jagiellonian University [email protected]
54 Mourou Gerard DAER-IZEST, Ecole Polytechnique
55 Muggli Patric Max Planck Institute for Physics
56 Nester James National Central University
57 OH John J. NIMS [email protected]
58 Ong Yen Chin Center for Gravitation and Cosmology, Yangzhou University
59 Page Don University of Alberta [email protected]
60 Parisi Alessandro Scuola Normale Superiore di Pisa
61 Prasetyo Ilham University of Indonesia [email protected]
62 Price Will The University of Arizona, Tucson, USA
63 Qiu Taotao 华中科技大学 [email protected]
64 RAFELSKI JOHANN The University of Arizona
65 Romano Enea University of Antioquia [email protected] 66 Ruffini Remo ICRANet, ICRA, INAF [email protected]
67 Steinmetz Andrew James
The University of Arizona, Tucson, USA
68 Sasaki Misao Kavli IPMU, U Tokyo/LeCosPA, NTU
69 Scardigli Fabio Politecnico di Milano & Institute Lorentz, Leiden
70 Shing Jukfai SYSU [email protected] 71 Silk Joseph IAP, JHU, Oxford [email protected] 72 Starobinsky Alexei Landau Institute for [email protected]
65
Theoretical Physics, Moscow, Russia
Last Name First Name Institution E-mail
73 Steinhauer Jeff Technion-Israel Institute of Technology
74 THAKRAN ANJALI [email protected]
75 Unruh William The University of British Columbia
76 Wang Bin Center for Gravitation and Cosmology, Yangzhou University
77 Wang Anzhong Baylor University [email protected] 78 Wen Wen-Yu CYCU [email protected] 79 WONG Henry Academia Sinica [email protected]
80 Wu Meng-Ru Institute of Physics, Academia Sinica
81 Yang Cheng Tao The University of Arizona, Tucson, USA
[email protected] [email protected]
82 Yeom Dong-han Pusan National University
83 Yokoyama Jun'ichi The University of Tokyo [email protected] 84 Zhang Cong University of Warsaw [email protected] 85 Zhang Yun-Long NAOC [email protected] 86 Zhao Suping [email protected]
87 Zimmermann Frank European Council for Nuclear Research
88 陳 泊錞 彰化師大物理系 [email protected] 89 陳 柏全 [email protected]
66
Note
67
68
69
70
71
LeungCenterforCosmologyandParticleAstrophysics
NATIONALTAIWANUNIVERSITY
https://lecospa.ntu.edu.tw
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