ASTROPARTICLES IN THE LHC Time.


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LHC does not see any sign of NP: still a NP identified with the adjustment of the elw. ... Be that as it may, for one arrangement obliging a non-insignificant vaulting ...
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Slide 1

NO - VE 2008, Venice, April 15-18, 2008 ASTROPARTICLES IN THE LHC ERA Antonio Masiero Univ. of Padova and INFN, Padova

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LHC and "LOW-ENERGY" NEW PHYSICS LHC finds NP : troublesome, if not unimaginable, to "remake" the essential hypothesis lying behind those signs of NP; LHC does not see any sign of NP : still a NP identified with the adjustment of the elw. scale might be available, however with particles whose masses are in the multi-TeV range .

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TEVATRON LHC I L C DM - FLAVOR for DISCOVERY and/or FUND. TH. Recreation A MAJOR LEAP AHEAD IS NEEDED NEW PHYSICS AT THE ELW SCALE DARK MATTER "LOW ENERGY" PRECISION PHYSICS m  n    … LINKED TO COSMOLOGICAL EVOLUTION FCNC, CP ≠, (g-2), ( ) 0  LFV Possible interchange with dynamical DE LEPTOGENESIS NEUTRINO PHYSICS

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WHY TO GO BEYOND THE SM "OBSERVATIONAL" REASONS THEORETICAL REASONS INTRINSIC INCONSISTENCY OF SM AS QFT (spont. broken gage hypothesis without irregularities) NO ANSWER TO QUESTIONS THAT "WE" CONSIDER "Principal" QUESTIONS TO BE ANSWERED BY "Major" THEORY ( progressive system, unification, flavor ) HIGH ENERGY PHYSICS (yet A FB … ) FCNC, CP  NO (however confirm >3 σ for NP in b - s transitions,,,) HIGH PRECISION LOW-EN. NO (yet (g-2)  … ) NEUTRINO PHYSICS YE m   0,    0 COSMO - PARTICLE PHYSICS YE (DM, ∆ B cos m , INFLAT., DE) Z bb NO YES Strong CP infringement? YES

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ON THE COMPLEMENTARITY OF DM and LFV SEARCHES to DIRECT LHC SEARCHES FOR NP Twofold significance of such complementarity: collaboration in "remaking" the "principal hypothesis" staying behind the marks of NP; ii) scope of correlative regions of the NP parameter space ( ex.: multi-TeV SUSY material science)

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MICRO MACRO PARTICLE PHYSICS COSMOLOGY HOT BIG BANG STANDARD MODEL GWS STANDARD MODEL HAPPY MARRIAGE Ex: NUCLEOSYNTHESIS POINTS OF FRICTION BUT ALSO COSMIC MATTER-ANTIMATTER ASYMMETRY INFLATION - DARK MATTER + DARK ENERGY "OBSERVATIONAL" EVIDENCE FOR NEW PHYSICS BEYOND THE (PARTICLE PHYSICS) STANDARD MODEL

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Present "Observational" Evidence for New Physics NEUTRINO MASSES DARK MATTER-ANTIMATTER ASYMMETRY INFLATION

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SM FAILS TO GIVE RISE TO A SUITABLE COSMIC MATTER-ANTIMATTER ASYMMETRY SM DOES NOT SATISFY AT LEAST TWO OF THE THREE SACHAROV\'S NECESSARY CONDITIONS FOR A DYNAMICAL BARYOGENESIS : NOT ENOUGH CP VIOLATION IN THE SM NEED FOR NEW SOURCES OF CPV IN ADDITION TO THE PHASE PRESENT IN THE CKM MIXING MATRIX FOR M HIGGS > 80 GeV THE ELW. Stage TRANSITION OF THE SM IS A SMOOTH CROSSOVER NEED NEW PHYSICS BEYOND SM. IN PARTICULAR, FASCINATING POSSIBILITY: THE ENTIRE MATTER IN THE UNIVERSE ORIGINATES FROM THE SAME MECHANISM RESPONSIBLE FOR THE EXTREME SMALLNESS OF NEUTRINO MASSES

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MATTER-ANTIMATTER ASYMMETRY NEUTRINO MASSES CONNECTION: BARYOGENESIS THROUGH LEPTOGENESIS Key-element of the SEE-SAW instrument for neutrino masses: substantial Majorana mass for the RIGHT-HANDED neutrino In the early Universe the overwhelming RH neutrino rots with Lepton Number violatiion; if these rots are joined by another wellspring of CP infringement in the leptonic division, then it is conceivable to make a lepton-antilepton asymmetry right now RH neutrinos rot . Since SM communications safeguard Baryon and Lepton numbers at all requests in irritation hypothesis, however abuse them at the quantum level, such LEPTON ASYMMETRY can be changed over by these simply quantum impacts into a BARYON-ANTIBARYON ASYMMETRY ( Fukugita-Yanagida system for leptogenesis )

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SUSY SEESAW : Flavor all inclusive SUSY breaking but then vast lepton flavor infringement Borzumati, A. M. 1986 (after examinations with W. Marciano and A. Sanda) ~ Non-diagonality of the slepton mass framework in the premise of corner to corner lepton mass grid relies on upon the unitary lattice U which diagonalizes (f  + f  ) see Isidori\'s discussion at this meeting

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µ e+  in SUSYGUT : past and future Calibbi, Faccia, A. M., Vempati

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INFLATION CAUSALITY (isotropy of CMBR) FLATNESS (  near 1 today) AGE OF THE UNIV. PRIMORDIAL MONOPOLES SEVERE COSMOGICAL PROBLEMS COMMON SOLUTION FOR THESE PROBLEMS VERY FAST (EXPONENTIAL) EXPANSION IN THE UNIV.  V(  ) VACUUM ENERGY  commanded by vacuum en. Genuine VACUUM NO WAY TO GET AN "INFLATIONARY SCALAR POTENTIAL" IN THE STANDARD MODEL

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NO ROOM IN THE PARTICLE PHYSICS STANDARD MODEL FOR INFLATION V=  2  2 +  4 no swelling But for one arrangement requiring a non-paltry vaulting Need to augment the SM scalar potential Ex: GUT\'s, SUSY GUT\'s,… See Giudice\'s discussion at this meeting ENERGY SCALE OF "INFLATIONARY PHYSICS": LIKELY TO BE » Mw DIFFICULT BUT NOT IMPOSSIBLE TO OBTAIN ELECTROWEAK INFLATION IN SM EXTENSIONS

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The Energy Scale from the "Observational" New Physics neutrino masses dim matter baryogenesis expansion NO NEED FOR THE NP SCALE TO BE CLOSE TO THE ELW. SCALE The Energy Scale from the "Hypothetical" New Physics Stabilization of the electroweak symmetry breaking at M W requires a ULTRAVIOLET COMPLETION of the SM as of now at the TeV scale + CORRECT GRAND UNIFICATION "CALLS" FOR NEW PARTICLES AT THE ELW. SCALE

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Mandatory to search for P - DECAY

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On the Energetic Budget of the Universe Courtesy of H. Murayama

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WMAP3 + little scale CMB exps (BOOMERang, ACBAR, CBI ans VSA) + Large-Scale Structures (SDSS,2dFCRS) + SuperNova ( HST/GOODS, SNLS) CONSISTENT WITH BARYON DENSITY DETERMINATION FROM BIG BANG NUCLEOSYNTHESIS

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DM: the most great proof at the "quantitative" and "subjective" levels of New Physics past SM QUANTITATIVE : Taking into record the most recent WMAP information which in mix with LSS information give stringent limits on  DM and  B EVIDENCE FOR NON-BARYONIC DM AT MORE THAN 10 STANDARD DEVIATIONS!! THE SM DOES NOT PROVIDE ANY CANDIDATE FOR SUCH NON-BARYONIC DM QUALITATIVE : it is insufficient to give a mass to neutrinos to acquire a legitimate DM hopeful; LSS arrangement obliges DM to be COLD NEW PARTICLES NOT INCLUDED IN THE SPECTRUM OF THE FUNDAMENTAL BUILDING BLOCKS OF THE SM !

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THE RISE AND FALL OF NEUTRINOS AS DARK MATTER Massive neutrinos: just applicants in the SM to represent DM. From here the "partiality" of neutrinos of a couple eV to accurately represent DM Neutrinos decouple at ~1 MeV ; being their mass<<decoupling temperature, neutrinos stay relativistic for quite a while. Being quick, they smooth out any conceivable development of thickness change disallowing the arrangement of proto-structures. The "weight" of neutrinos in the DM spending plan is seriously constrained by the perceptions disfavoring situations where first superlarge structures emerge and after that cosmic systems start from their discontinuity

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WIMPS ( Weakly Interacting Massive Particles )  #  exp(- m/T) #  does not change any more # ~# m  T decoup l. regularly ~ m /20    relies on upon molecule material science ( annih. ) and "cosmological" amounts (H, T 0 , … 10 - 3   h 2 _ ~ <( annih . ) V  > TeV 2 From T 0 M Planck ~  2/M 2   h 2 in the reach 10 - 2 - 10 - 1 to be cosmologically intriguing (for DM) m  ~ 10 2 - 10 3 GeV (powerless cooperation) h 2 ~ 10 - 2 - 10 - 1 !!! Warm RELICS ( WIMP in thermodyn.equilibrium with the plasma until T decoupl )

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STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS SUSY EXTRA DIM. LITTLE HIGGS. 1) ENLARGEMENT OF THE SM (x  , ) (x , j i) SM part + new part Anticomm. New bosonic to wipe out  2 Coord. Coord. at 1-Loop 2) SELECTION RULE DISCRETE SYMM. STABLE NEW PART. R-PARITY LSP KK-PARITY LKP T-PARITY LTP Neutralino turn 1/2 spin1 spin0 m LSP ~100 - 200 GeV * m LKP ~600 - 800 GeV 3) FIND REGION (S) PARAM. SPACE WHERE THE "L" NEW PART. IS NEUTRAL + Ω L h 2 OK m LTP ~400 - 800 GeV * But surrendering gaugino-masss unif. Conceivable to have m LSP down to 7 GeV Bottino, Donato, Fornengo, Scopel

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D. kAZAKOV

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FROM THE MSSM TO THE C MSSM ( obliged MSSM) PROLIFERATION OF PARAMETRS IN THE SOFT BREAKING SECTOR OF THE MSSM : OVERALL NUMBER OF PARAM. IN THE MSSM IS 1 2 4 C MSSM

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WHICH SUSY HIDDEN SECTOR SUSY BREAKING AT SCALE F F = (10 5 - 10 6 ) GeV F = M W M Pl GRAVITY Gage INTERACTIONS MESSENGERS M gravitino ~ F/M Pl ~ (10 2 - 10 3 ) eV M gravitino ~ F/M Pl ~ (10 2 - 10 3 ) GeV OBSERVABLE SECTOR SM + superpartners MSSM : negligible substance of superfields

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GRAVITINO LSP? Gage MEDIATED SUSY BREAKING (GMSB) : LSP prone to be the GRAVITINO ( it can be light to the point that it is more a warm DM than a chilly DM competitor ) Although we can\'t specifically recognize the gravitino, there could intrigue marks from the by the LSP ( NLSP) : for occurrence the s-tau could rot into tau and gravitino, Possibly with a long life time, even of the request of days or months

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DIFFERENT FROM THE THERMAL HISTORY OF WIMPS SWIMPS (Super Weakly Interacting Massive Particles) - LSP Gravitino in SUSY - First excitation of the graviton in UED … They acquire the fitting relic thickness through the rot of a more enormous warm animal varieties that has prior decoupled from the warm shower

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ELLIS, OLIVE,SANTOSO,SPANOS .:tslidesep

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