XXIX-th International Workshop on High Energy Physics: NEW RESULTS and ACTUAL PROBLEMS in PARTICLE & ASTROPARTICLE PHYSICS and COSMOLOGY

26 Jun 2013, 09:00 → 28 Jun 2013, 21:50 Europe/Moscow

Conference hall (IHEP, Theoretical Division)

Nikolai Tyurin (Institute for High Energy Physics (RU))

Institute for High Energy Physics  (in the framework of the National Research Centre "Kurchatov Institute") is organizing the XXIX-th International Workshop on High Energy Physics “NEW RESULTS and ACTUAL PROBLEMS in PARTICLE & ASTROPARTICLE PHYSICS and COSMOLOGY”, June 26-28, 2013, in Protvino, Moscow region, Russia.

 The purpose of this Workshop is to exhibit a more complete and coherent picture of our understanding of the structure and dynamics of the microcosm, the megacosm and its evolution and the relationship between these two extremes of modern physics.

 The Workshop covers both theory and experiment/observations in most actual and critical points.

 We would like to promote, at the meeting, much more critical discussions than is usually the case. An example is the series of historic debates at famous Solvay Congresses.

 To this end the meeting will be organized so that reports will be accompanied by discussion panels and talks. In addition, the poster event for brief actual notes will be organized.

 Topics to discuss contain presumably Higgs boson observed at LHC and Tevatron (including alternative interpretations), exploratory searches for dark matter and dark energy, neutrino oscillations and the problem of neutrino mass, progress in the study of confinement in YM theory and beyond, quark-gluon plasma and other exotic states of matter, problems in QCD as the strong interaction theory, black holes (pro et contra), progress in Grand Unification theories, early Universe, cosmic microwave background radiation, progress in experimental and accelerator techniques.

 We believe that such a relatively wide scope of subjects for presentation and discussion will be also a good opportunity for participants to learn first hands about the state of art in the fields of common interest where they are not experts.

CONFERENCE FEE

- 5000 Rub. (~ 125 Euro)  for applications before 15/05/2013
- 8000 Rub. (~ 200 Euro) for applications after 15/05/2013
Includes visa payments, transportation from/to the airport, coffee breaks,

conference dinner, welcome and farewell parties, complete set for the participant.

IMPORTANT DATES:

January 15, 2013 - start of the registration procedure and abstract submission
May 15, 2013 – 1st registration deadline for those who needs Russian visa, change of the registration fee (5000 rub. to 8000 rub.)
May 1, 2013 - start of the presentation upload
June 1, 2013 –  2nd registration deadline for those who needs Russian visa
June 15, 2013 - registration deadline for domestic participants
June 15, 2013 - end of the registration procedure and abstract submission  
                              

Since visa formalities may take a long time, please, try to send us the information as early as possible (it is better before May 1, 2013).

Please, send us the title of your talk (even if preliminary) before June 15, 2013 and try to upload your presentation by the web interface (will be open after January 15, 2013) or send it by e-mail to Roman.Rioutine@cern.ch  before June 15, 2013.
Please, inform organizers about any changes.

Participation

About 50 scientists from Russia and other countries are expected to participate. The sessions will be held in the Conference Hall of the Theory Division Building.

The Proceedings of the Workshop will be published in “Proceedings of Science”.

Accommodation

The Workshop will be held in Protvino, a small town 100 km to the south of Moscow. The town is situated nearby the State Research Center of Russia—IHEP (Serpukhov 76 Gev accelerator) inside a pine forest and near the Protva river.

The participants will be accommodated in the “Protva” hotel in single or double rooms. Prices for one night are from $40 to $80. The total living expenses (including breakfast, lunch, and dinner) will be about $10 a day. The participants can have their meal in the restaurant and snack-bar of the Hotel, in the restaurant of the Club of Scientists or in other restaurants of Protvino indicated in the map.

Transportation

All the participants will be transported from/to the Sheremetievo or Domodedovo airports by the IHEP transport or taxi. The information on flights or trains and the date of arrival should be communicated to the Scientific Secretary of the Organizing Committee a few days in advance.

Information bulletin

• bulletin_1.doc
• bulletin_1.pdf
• bulletin_2.doc
• bulletin_2.pdf
• bulletin_3_v3.docx
• bulletin_3_v3.pdf

photo

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Preliminary agenda Preliminary_agenda_17.06.2013.doc Preliminary_agenda_17.06.2013.pdf

proceedings

• bookblock_gray.pdf
• corrs.zip
• editors.zip

Program Program_printable.doc Program_printable.pdf

Russian visa information Procedure to obtain russian visa VISA_INFO.pdf

Style for Proceedings ws-procs975x65_2e.zip

Wednesday, 26 June

09:30 → 13:15 Morning session

Mostly devoted to Higgs boson physics

09:30 Opening address

Speaker: Nikolai Tyurin (Institute for High Energy Physics (RU))

09:40 Overview of the Higgs boson searches at the LHC

Speaker: Rosy Nikolaidou (CEA/IRFU,Centre d'etude de Saclay Gif-sur-Yvette (FR))

Slides RN_IHEP2013.pdf

10:10 Higgs studies at the Tevatron

Speaker: Gregorio bernardi (LPNHE University of Paris 6 & 7)

Slides bernardi-ihep.pdf

10:40 Coffee break

11:00 Higgs at Least

Speaker: Francesco Riva (Ecole Polytechnique Federale de Lausanne (CH))

Slides

• Higgs_Protvino_FR_3_part_10.pdf
• Higgs_Protvino_FR_3_part_11.pdf
• Higgs_Protvino_FR_3_part_12.pdf
• Higgs_Protvino_FR_3_part_13.pdf
• Higgs_Protvino_FR_3_part_1.pdf
• Higgs_Protvino_FR_3_part_2.pdf
• Higgs_Protvino_FR_3_part_3.pdf
• Higgs_Protvino_FR_3_part_4.pdf
• Higgs_Protvino_FR_3_part_5.pdf
• Higgs_Protvino_FR_3_part_6.pdf
• Higgs_Protvino_FR_3_part_7.pdf
• Higgs_Protvino_FR_3_part_8.pdf
• Higgs_Protvino_FR_3_part_9.pdf

11:30 On possible interpretation of the LHC Higgs-like state in the framework of the non-perturbative effective interaction of W bosons

Speaker: Boris ARBUZOV (SINP MSU, Moscow)

Slides ARBUZOV.pdf

12:00 The Higgs, a Higgs or Higgs-like alternatives?

Speaker: Alexander KNOCHEL (ITTK RWTH, Aachen, Germany)

Slides ihephiggs_knochel.pdf

12:30 Panel Discussion on Higgs Boson

Moderator: V. Kiselev Panelists: B. Arbuzov A. Knochel R. Nikolaidou G. Bernardi F. Riva Questions: • If the SM with elementary Higgs field is completely confirmed with the discovery of a heavy scalar boson at LHC and Tevatron? • Does the Higgs mass value of 126 GeV point to the need of new physics below the Planck scale? • Do we need the next Higgs factory to solve problems with its identification? • How can we distinguish extended Higgs sector from the standard one as well as from the composite Higgs?

Speaker: Valery Kiselev (IHEP, Protvino, Russia)

Video higgs_www.mp4

13:25 → 14:05 Lunch

14:15 → 19:05 Evening session

Mostly devoted to QGP, Heavy quarks and Exotics

14:15 Review of the physics of Quark Gluon Plasma

Speaker: Sonja Kabana (Laboratoire de Physique Subatomique et des Technologies Associe)

Slides SoniaKabana_protvino_26-28june2013_final_online.pdf

14:45 Recent Results on Heavy Ions at RHIC

Speaker: Olga Evdokimov (Physics Department-University of Illinois at Chicago)

Slides 2013_HEPFT_Olga_final.pdf 2013_HEPFT_Olga_final.pptx

15:15 Quark-gluon plasma multiplicity from AdS spaces modifications

In holographic approach the Quark Gluon Plasma (QGP) formation in 4D space is related with Black Hole (BH) creation in 5D Anti de Sitter space (AdS) and multiplicity in heavy-ion collisions is determined by entropy of 5D BH. Using the general relativity technique the entropy of formed BH can be estimate by the trapped surface area. We simulate energy dependence of entropy considering modifications to AdS by different wrapping factors. We compare the results with experimental data.

Speaker: Ekaterina POZDEEVA (SINP MSU, Moscow)

Slides Pozdeeva.pdf

15:30 Quark-gluon plasma, challenges to theory

Speaker: Valentin ZAKHAROV (ITEP, Moscow)

Slides zakharov_25.06.13.pdf

16:00 Coffee-break

16:20 Recent results from the LHCb experiment

Speaker: Bernardo Adeva (Universidade de Santiago de Compostela (ES))

Slides LHCb_results_Protvino.pdf

16:50 Top quark physics results from CMS

Speaker: Cristina Ferro (National Central University (TW))

Slides Ferro.pdf Particle_Astro_cferro.pdf

17:20 Searches for Supersymmetry at CMS

Speaker: Fedor Ratnikov (KIT - Karlsruhe Institute of Technology (DE))

Slides 130626_SUSY_IHEP_v2.pdf

17:50 Exotica, Beyond Two Generations

Speaker: Khristian Kotov (Ohio State University (US))

Slides kk_2013.06.26_2.pdf

18:20 Panel Discussion on QGP, Heavy Quarks and Exotics

Moderator: V. Zakharov Panelists: S. Kabana O. Evdokimov K. Kotov S. Troshin S. Sadovsky Questions: • In which case experiment could unambiguously (dis)prove the existence of Quark-Gluon Plasma? • If the investigations of HI collisions can clarify the confinement problem? • Is there time enough for establishing the local thermodynamic equilibrium in the course of the HI collision? • Can HI collisions imitate the early instants of the Universe evolution?

Speaker: Valentin Zakharov (ITEP, Moscow, Russia)

Minutes Minutes_of_the_Quark.docx Minutes_of_the_Quark.pdf

Video QGP_www.mp4

19:10 → 20:40 Welcome party

Thursday, 27 June

09:30 → 13:20 Morning session

Mostly devoted to neutrinos

09:30 OPERA experiment

This talk is focused on a general description of the OPERA experiment, which is designed to observe directly the appearance of nu-tau produced by neutrino oscillations in an almost pure nu_mu beam. The neutrino beam is produced at CERN and detected 730 km away in an underground hall of the National Laboratory of Gran Sasso. OPERA detector is a hybrid structure, containing nuclear emulsion detector modules with lead plates, acting as a target for the neutrino beam, complemented by electronic target trackers and muon spectrometers. The signature of a tau neutrino interaction is the observation of the tau lepton decay and the absence of muon at the primary vertex. To obtain information about the charged particles trajectories around the interaction vertex, the emulsion is scanned with automatic scanning systems. The current status of data taking is reported. The main background sources having the nu_tau event topology include the reinteraction of hadrons, the decay of charmed mesons produced in nu_mu Charged Current interaction, and the scattering of muons from nu_mu Charged Current interactions. In this talk the estimated level of background events is reported and the results of the nu_mu->nu_tau analysis are presented.

Speaker: Mr Andrey Sheshukov (JINR)

Slides Sheshukov.pdf

09:55 Search for neutrino oscillations in appearance mode with the OPERA experiment

The present talk highlights the data analysis status of the OPERA experiment. The experiment exploited the CNGS beam from CERN to Gran Sasso, at the average L/E ratio of 43 km/GeV, optimized to search for ν_μ→ν_τ oscillation in appearance mode, and also allowing to perform a ν_e appearance search. Profiting of the sub-micrometer spatial resolution of nuclear emulsions, employed in the OPERA experiment, it is possible to identify and analyze the neutrino interactions on event-by-event basis. The hardware of the experiment as well as the status of emulsion scanning are described in the other OPERA presentation by Andrey Sheshukov. In this talk we review the data simulation and the analysis chains, with an emphasis on what was done during the last year. The main kinematical parameters of the neutrino event are introduced; we specially discuss the parameters sensitive to the neutrino flavor. The uncertainties on the event parameter estimation are reviewed, and the main sources of background for the ν_μ→ν_τ oscillation search are examined. The topologies of the three observed ν_τ candidate events are discussed. The status of the ν_e appearance search is also reviewed, the ν_e identification technique and the main sources of relevant background are briefly discussed. Finally, we present the constraints set by the OPERA experiment on the mixing angle θ_13 and on the LSND/MiniBooNE anomaly.

Speaker: Timur Dzhatdoev (PNPI MSU, Moscow, Russia)

Slides dzhatdoev.pdf

10:15 Super-Kamiokande Results

Speaker: Michael Smy (UCI)

Slides smy_skneutrino_iwhep.pdf

10:50 Coffee-break

11:10 KATRIN Experiment: status and perspectives 2013

KATRIN project has a goal to set electron antineutrino mass upper limit at 0.2 eV level. Installation construction at Karlsruhe Institute of Technology (KIT) proceeds to it final stage. Inner electrodes are installed inside the main spectrometer and first background tests are launched. Windowless gaseous tritium source (WGTS) temperature stabilization was proven to provide 20 mK temperature uniformity. WGTS superconducting coils are under construction. INR RAS participates in the Rear Wall subproject. RW should control gaseous tritium electric potential uniformity inside WGTS via plasma generated by tritium beta-electrons. Set of experimental test is planned at INR “Troitsk nu-mass” spectrometer.

Speaker: Nikita Titov (INR RAS, Moscow)

Slides Titov_KATRIN_project.pdf

11:30 Status and results of the GERDA experiment

The study of neutrinoless double beta decay ($0\nu\beta\beta$) is a powerful approach to investigate fundamental properties of neutrinos. The observation of $0\nu\beta\beta$ would demonstrate lepton number violation in nature and prove that neutrinos have a Majorana component. It will also give an access to the neutrino mass hierarchy and to the information on the absolute values of the neutrino masses. The {\sc Gerda} experiment [1] is an low background experiment aimed to search for the $0\nu\beta\beta$ of $^{76}$Ge. The aim of {\sc Gerda} is to test the claim of discovery by part of Heidelberg-Moscow Collaboration [2], and, in a second phase, to achieve much better sensitivity than recent experiments. The main concept of {\sc Gerda} is the operation of naked HPGe detectors made from enriched $^{76}$Ge, which are immersed in liquid argon (LAr). A cryostat with 64~m$^3$ liquid argon is located inside a steel tank containing 590~m$^3$ pure water. Presently in Phase~I, eight detectors of coaxial type made from material enriched in $^{76}$Ge are deployed. Detectors are mounted on low mass holders and read out by custom made, low radioactive amplifiers located close to the diodes. A background index of about 2$\times$10$^{-2}$ cts/(keV$\cdot$kg$\cdot$yr) is reached near the region of $0\nu\beta\beta$ search. Obtained half-life of two-neutrino double beta decay of $^{76}$Ge is ($1.84\substack{+0.14 \\ -0.10}$)$\times$10$^{21}$ yr [3]. Currently an exposure more than 20 kg$\cdot$yr has been accumulated in {\sc Gerda} experiment since November 2011. In June 2013 it is planning to stop data taking and open narrow blinded region of the expected 0$\nu\beta\beta$ peak location. \\ At the same time preparations towards the second phase of {\sc Gerda} are ongoing. New enriched BEGe detectors with total mass of about 20 kg were successfully produced and tested. They show good resolution and pulse shape discrimination capability. Operations for the deployment of these detectors together with LAr light scintillation veto in {\sc Gerda} is planned to start just after the finishing of the Phase I data taking. We are expecting that such improvements allow us to suppress backgrounds in {\sc Gerda} to the level of 1$\times$10$^{-3}$ cts/(keV$\cdot$kg$\cdot$yr) in the region of interest. [1] H.-K.Ackermann et al., Eur. Phys. J. C 73 (2013) 2330. [2] H.V. Klapdor-Kleingrothaus et al., Phys. Lett. B586, 198 (2004). [3] M.Agostini et al., J. Phys. G: Nucl. Part. Phys. 40 (2013) 035110.

Speaker: Alexey Lubashevskiy (MPIK)

Slides lubashev_Protvino.pdf

11:55 Neutrino oscillations: recent results and perspectives

Speakers: Dr Marat Khabibullin (INR RAS, Troitsk), Prof. Yury Kudenko (Russian Academy of Sciences (RU))

Slides kudenko_protvino_1306.pdf kudenko_protvino_1306.pptx

12:35 Panel discussion on Neutrino Problems

Moderator: V. Obraztsov Panelists: M. Smy M. Khabibullin N. Titov S. Gershtein Questions: • How well do we need to know the standard neutrino sector parameters? • Neutrino and the lepton/baryon asymmetry in the Universe. • Are there new species of neutrino (e.g. the "sterile"one)? • What are the most important problems of neutrino physics? • Perspectives of neutrino experiments.

Speaker: Vladimir Obraztsov (Institute for High Energy Physics (RU))

Video neutrino_www.mp4

13:30 → 14:30 Lunch

14:40 → 18:45 Evening session

Devoted to SM, diffrative, spin physics

14:40 SM and QCD Results at the LHC

Speaker: Oleg Zenin (Institute for High Energy Physics (RU))

Slides ATL-COM-PHYS-2013-747.pdf

15:10 Charge Particle Production at HERA

Speaker: Alexander Bylinkin (ITEP)

Slides HEPFT_Bylinkin9.pdf

15:30 Search for the U boson in WASA@COSY experiment

Speaker: Damian PSZCZEL (NCNR, Warsaw, Poland; Uppsala University)

Slides Protvino2013.pdf

15:50 What can we learn from nuclei-nuclei interactions at LHC

The discovery of Higgs boson completed the first (and main) stage of experiments on p-p-interactions at LHC. Attempts to search new physics effects in these experiments did not give positive results. At that time, many interesting and not described by modern theories and models phenomena were observed in cosmic ray experiments in the energy region 1015 – 1017 eV, which corresponds to the LHC energy interval 1 – 14 TeV. It is important that all unusual phenomena were observed in interactions of cosmic ray particles (most part, nuclei) with nuclei of atoms of the atmosphere. In this talk, on the basis of the analysis of cosmic ray experimental results, some propositions for nuclei-nuclei experiments at LHC are considered.

Speaker: Prof. Anatoly Petrukhin (MEPhI, Moscow)

Slides Petrukhin_PAPC_2013.pdf Petrukhin_PAPC_2013.ppt

16:10 Coffee-break

16:30 What Do We Learn about Strong Interactions from Experiments at High Energies?

Speaker: Vladimir Petrov (Institute for High Energy Physics (RU))

Slides

• High-Energy_Collisions_in_Space-Time_Perspective_[Автосохраненный].pdf
• High-Energy_Collisions_in_Space-Time_Perspective_[Автосохраненный].pptx
• moz_mapi-1.pdf

17:00 Spin Results at RHIC

Speaker: Alexander Bazilevsky (B)

Slides Bazilevsky_RHIC_Spin_(1).pdf Bazilevsky_RHIC_Spin_(1).pptx

17:30 Inward Horizons of the Spinning Nucleons

Speaker: Alexey PROKUDIN (JLAB, Newport News, USA)

Slides AlexeiProkudin.pdf

18:00 Panel discussion on SM&QCD at High Energies and Nucleon Structure

Moderator: A. Prokudin Panelists: O. Zenin B. Adeva C. Ferro A. Likhoded Questions: Panel Discussion IV. • Does QCD help us to understand strong interactions? • Does the SM theory with Kobayashi-Maskawa (CKM) quark-mixing matrix describe all CP-violation and rare decays phenomena observed in the heavy quark sector? • Can quantum loop corrections reveal new physics mass scales well above the TeV scale, by means of indirect searches? • Is the low-energy supersymmetry of TeV scale in trouble after the LHC results on its direct search?

Speaker: Alexey Prokudin (JLAB, Newport News)

Video SM_www.mp4

19:00 → 21:30 Culture Programm

Concert and Conference Dinner

19:00 CONCERT

Speaker: TRIO ELEGIA

20:00 Conference Dinner

Friday, 28 June

09:30 → 13:15 Morning session

Devoted to Black Holes

09:30 Black Holes in Binary Systems ang Galaxy Nuclei

Speaker: Prof. Anatoly CHEREPASHCHUK (SAI MSU, Moscow)

Slides Cherepaschuk.pdf Cherepaschuk.ppt

10:00 Supermassive Black Hole at the Galactic Center

Speaker: Alexander ZAKHAROV (ITEP, Moscow)

Slides

• zakharov_101-120.pdf
• zakharov_101-120.pptx
• zakharov_1-20.pdf
• zakharov_1-20.pptx
• zakharov_121-140.pdf
• zakharov_121-140.pptx
• zakharov_141-160.pdf
• zakharov_141-160.pptx
• zakharov_161-177.pdf
• zakharov_161-177.pptx
• zakharov_21-40.pdf
• zakharov_21-40.pptx
• zakharov_41-50.pdf
• zakharov_41-50.pptx
• zakharov_51-56.pdf
• zakharov_51-56.pptx
• zakharov_57-60.pdf
• zakharov_57-60.pptx
• zakharov_61-80.pdf
• zakharov_61-80.pptx
• zakharov_81-100.pdf
• zakharov_81-100.pptx

10:30 Point massive particle in General Relativity

It is well known that the Schwarzschild solution describes the gravitational field outside compact spherically symmetric mass distribution in General Relativity. In particular, it describes the gravitational field outside a point particle. Nevertheless, what is the exact solution of Einstein's equations with \delta-type source corresponding to a point particle is not known. In the present paper, we prove that the Schwarzschild solution in isotropic coordinates is the asymptotically flat static spherically symmetric solution of Einstein's equations with \delta-type energy-momentum tensor corresponding to a point particle. Solution of Einstein's equations is understood in the generalized sense after integration with a test function. Metric components are locally summable functions for which nonlinear Einstein's equations are mathematically defined. The Schwarzschild solution in isotropic coordinates is locally isometric to the Schwarzschild solution in Schwarzschild coordinates but differs essentially globally. It is topologically trivial neglecting the world line of a point particle. Gravity attraction at large distances is replaced by repulsion at the particle neighborhood.

Speaker: Mikhail Katanaev (Steklov Mathematical Institute, Moscow)

Slides Katanaev.pdf

10:55 Coffee-break

11:15 Einsteinian revolution's misinterpretation: no true black holes, no information paradox, but just quasi-static balls of quark gluon plasma'

Even if one would assume existence of Black Holes (BHs), High Energy Astrophysics observations cannot be explained because no free charge, no current can emerge from central singularities. In other words, even supposed charged BHs cannot have any electromagnetic property. In fact gravitational effects too should not propagate out of Event Horizons! Several authors try to resolve the BH conundrum by invoking the original Schwarzschild solution for a ``Point Mass’’ by assuming the integration constant ᬬ¬¬ to be finite. But this approach is inconsistent because it endows a ``Point Mass’’ with a surface area of 4πᬬ¬ 2. This problem was finally resolved by Mitra (J. Math. Phys. 2009) by showing that, for a ``Point Mass’’, α=0. Mathematically this implies that BHs have unique gravitational mass M=0. Physically, for continued gravitational collapse the entire mass energy must be radiated out. Since the comoving proper time for formation of a M=0 BH is infinite, such a singular state is never formed and the so-called BH Candidates must be ``Eternally Collapsing Objects’’ (ECO). As the collapsing object heats up by contraction and start trapping its own radiation, at a certain stage, it attains ``Eddington Luminosity’’ when the inward pull of gravity gets balanced by outward radiation force. Astrophysical ECOs are expected to be strongly magnetized (MECOs), and there are many evidences that whether in X-ray binaries or in Quasars, the BH Candidates are MECOs. The magneto radiative instabilities of MECO plasma cause unpredictable Solar Flare and Coronal Mass Ejection like phenomena. The long duration Gamma Ray Bursts are associated with formation of nascent MECOs and rejuvenation of their central engines can be understood as further collapse of unstable nascent MECOs.

Speaker: Abhas MITRA (BARC, Mumbai, India)

Slides ProtvinoMitra1.pdf ProtvinoMitra1.ppt

Video Solar_Flare_Upclose_-_Video.avi

11:45 Theoretical Flaws in Black Hole Theory and General Relativity

All alleged black hole solutions pertain to a universe that is spatially infinite, is eternal, contains only one mass, is not expanding, and is asymptotically flat. But the alleged big bang cosmology pertains to a universe that is spatially finite, is of finite age, contains radiation and many masses including multiple black holes (some of which are primordial), is expanding, and is not asymptotically flat. Thus the black hole and the big bang contradict one another – they are mutually exclusive. The black hole is almost universally claimed to be predicted by General Relativity. It is surprisingly easy to prove that this is not true. Similarly it is very often claimed that Newton’s theory of gravitation also predicts the black hole, but this too is very easily proven to be erroneous. Despite numerous claims for discovery of black holes in their millions, nobody has ever actually found one. In addition it is not very difficult to prove that General Relativity violates the usual conservation of energy and momentum, with only a little use of mathematics. The simple proofs also demonstrate that all ‘singularity theorems’ related to General Relativity are invalid. Fundamentally there are contradictions contained in the very physical principles of General Relativity, combined with invalid mathematics, which render the theory untenable. It is the object of this paper to provide the proofs without the complicated mathematics usually associated with the subject.

Speaker: Stephen CROTHERS (AIAS, USA)

Slides Crothers-Protvino-2013.pdf

12:15 Panel discussion on Black Holes

Moderator: S. Sokolov Panelists: A. Cherepashchuk A. Mitra S. Crothers A. Zakharov Questions: • Is there a definitive observational/experimental proof of the existence of black holes? • Are there theoretical problems with black holes? • Are any understanding of mass gap between the supermassive black holes in centers of spiral galaxies and star-range black holes ascribed to probable candidates? • Do we need to get primordial black holes from the first times?

Speaker: Skiff Sokolov (IHEP, Protvino, Russia)

Video BlackHoles_www.mp4

13:25 → 14:20 Lunch

14:30 → 18:45 Evening session

Devoted to Dark Matter and Cosmology

14:30 On Semiclassical Quantum Cosmology becoming a numerical subject

Speaker: Edward ANDERSON (APC, Paris/Cambridge Univ., DAMTP, UK)

Slides Anderson.pdf

15:00 Einsteinian revolution's wrong turn: lumpy interacting cosmos assumed as smooth perfect fluid: no dark energy

Newtonian Cosmology was apparently plagued with the problem of infinite gravitational force, and Einstein’s General Relativity apparently ushered in the revolutionary concept of a closed finite non-singular static universe. Later, Big Bang model (BBM) essentially incorporated non-static versions of similar relativistic model. Simultaneously the concept of a Cosmological Constant or a repulsive vacuum energy density got incorporated by either for Inflation or for Dark Energy. We dismantle this nearly century old edifice by presenting several exact proofs showing that Cosmological Constant or Dark Energy is non-existent, and Einstein’s Static universe is just the Minkowski vacuum. By using the just found Schwarzschild form of the FRW metric (Mitra, Grav. Cosmo. 2013), we show that FRW metric too is actually the Minkowski vacuum! It is suggested that physical universe is quasi-Newtonian where for any given galaxy, finite gravitational potential is due to interaction of nearest neighbors while the infinite background forces cancel one another due to symmetry. Such an universe is likely to have a fractal structure as suggested by observations. The cosmic redshift might arise due to asymmetric spread of wave packets associated with line emissions from distant galaxies. The cosmic background radiation might be due to thermalization of star lights in an eternal universe as suggested by Hoyle, or it might be superposition of gravitationally redshifted quiescent Eternally Collapsing Objects’’, the supposed ``Black Hole Candidates’’. The atmosphere of hot ECOs may synthesize not only light elements but infuse fresh hydrogen from flares of ECO plasma.

Speaker: Abhas Mitra (BARC, Mumbai, India)

animation Thermally_Agitated_Molecule.gif Translational_motion.gif

Slides ProtvinoMitra2.pdf ProtvinoMitra2.ppt

15:30 The gamma-ray bursts, core-collapse supernovae and global star forming rate at large redshifts

The brief review and discussion of statement of some observational problems of gamma-ray bursts (GRB), GRB host galaxies and star forming at small and large redshifts: Are there similarities and differences between GRB hosts and the typical galaxy population - this is currently the main question for the study of GRB host galaxies. The direct connection between long-duration GRBs and massive stars explosions, GRBs and some puzzles of core-collapse supernovae are discussed. On model-independent observational cosmological tests - GRB rate and star forming rate at high redshifts.

Speaker: Vladimir Sokolov (SAO RAS, Nizhnij Arkhyz, Russia)

Slides WSokolov-PROTVINO.pdf WSokolov-PROTVINO.ppt

16:00 Coffee-break

16:20 High Energy Gravitational Waves from the Early Universe

Speaker: Alexander Dolgov

Slides hi-gw-early-univ.pdf

16:50 Cosmological perturbations: what do they tell?

Speaker: Prof. Valery RUBAKOV (INR RAS, Moscow)

Slides protvino-jun2013.pdf

17:20 Panel discussion on Cosmology

Moderator: E. Anderson Panelists: A. Mitra V. Rubakov A. Dolgov S. Crothers A. Zakharov Questions: Discussion VI. • To what extent Dark Matter and Dark Energy are necessary to explain the observed properties of the Universe? • Why the Dark matter profiles so universal at the galactic scales? • Are there viable candidates of modified gravitational dynamics to exclude the dark components of Universe? • Have we any perspectives to distinguish the Dark Energy from the cosmological constant? • Are there any certain indications for the sterile neutrinos in the cosmos? • How does the Planck data change the view to the inflation of early Universe? What is an origin of inflaton plateau? So far, what else is interesting about the Planck data? • What are nearest crucial points in cosmological observations? • Can we be more decisive discriminating between anthropic principle, super-stringy landscape, fine tuning or dynamics as concerns for the cosmological coincidences?

Speaker: Edward Anderson (Cambridge Univ., DAMTP, UK)

Video Cosmology_www.mp4

18:20 Closing address

Speaker: Vladimir Petrov (Institute for High Energy Physics (RU))

18:50 → 20:30 Farewell party