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L’ UNIVERSO INVISIBILE:IL PROBLEMA DELLA
MATERIA ED ENERGIA OSCURE
Antonio MasieroUniv. di Padova
eINFN, Padova
INCONTRI DI FISICA, LNF, 9 OTT. 2009
UNIFICAZIONE delle
INTERAZIONI FONDAMENTALIINTERAZIONI FONDAMENTALI
IL MODELLO STANDARD PARTICELLAREIL MODELLO STANDARD PARTICELLARE
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
WHY TO GO BEYOND THE SM
““OBSERVATIONAL” REASONSOBSERVATIONAL” REASONS•HIGH ENERGY PHYSICS
(but AFB……)
•FCNC, CPNO (but b sqq penguin …)
•HIGH PRECISION LOW-EN.
NO (but (g-2) …)
•NEUTRINO PHYSICS YE m 0, 0
•COSMO - PARTICLE PHYSICS
YE (DM, ∆B cosm, INFLAT., DE)
Z bbNO
NO
NO
YES
YES
THEORETICAL REASONSTHEORETICAL REASONS•INTRINSIC INCONSISTENCY OF SM AS QFT
(spont. broken gauge theory without anomalies)
•NO ANSWER TO QUESTIONS THAT “WE” CONSIDER “FUNDAMENTAL” QUESTIONS TO BE ANSWERED BY “FUNDAMENTAL” THEORY
(hierarchy, unification, flavor)
NO
YES
INDICAZIONI DI NUOVA FISICA AL DI LA’ DEL MODELLO STANDARD PARTICELLARE
• MASSA DEI NEUTRINI• ESISTENZA DI MATERIA OSCURA NON COSTITUITA DALLA
“SOLITA” MATERIA (protoni, neutroni) • ASIMMETRIA COSMICA TRA MATERIA E ANTIMATERIA:
ESISTENZA DI UNA NUOVA SORGENTE DI VIOLAZIONE DI CP OLTRE A QUELLA PREVISTA DAL MODELLO STANDARD
• IMPOSSIBILITA’ NEL MS DI OTTENERE UNA FASE INFLAZIONARIA ( ESPANSIONE ACCELERATA ESPONENZIALMENTE ) NELL’UNIVERSO PRIMORDIALE
• DOMANDE “FONDAMENTALI” A CUI IL MODELLO STANDARD NON RISPONDE:
- UNIFICAZIONE DELLE FORZE FONDAMENTALI - MASSE E MESCOLAMENTI DEI FERMIONI- “STABILITA’” DELLA SCALA DI ENERGIA A CUI I BOSONI W e Z
PRENDONO MASSA ( circa 100 GeV)
THEORETICAL REASONS TO GO THEORETICAL REASONS TO GO BEYOND THE SM BEYOND THE SM
• FLAVOR PUZZLE RATIONALE FOR FERMION MASSES AND MIXINGS
• UNIFICATION PROBLEM NO REAL UNIF. OF ELW.+STRONG INTERACTIONS +GRAVITY LEFT OUT OF THE GAME
• HIERARCHY PROBLEM(S) ULTRAVIOLET COMPLETION OF THE SM TO (NATURALLY) STABILIZE THE ELW. BREAKING SCALE + TUNING OF THE COSMOLOGICAL CONSTANT
Present “Observational” Evidence for New Physics
• NEUTRINO MASSES
• DARK MATTER
• MATTER-ANTIMATTER ASYMMETRY
• INFLATION
MICRO MACROPARTICLE PHYSICS COSMOLOGY
GWS STANDARD MODEL HOT BIG BANG STANDARD MODEL
HAPPY MARRIAGE Ex: NUCLEOSYNTHESIS
BUT ALSO POINTS OF FRICTION
-COSMIC MATTER-ANTIMATTER ASYMMETRY
-INFLATION
- DARK MATTER + DARK ENERGY
“OBSERVATIONAL” EVIDENCE FOR NEW PHYSICS BEYOND
THE (PARTICLE PHYSICS) STANDARD MODEL
The Energy Scale from the“Observational” New Physics
neutrino masses
dark matter
baryogenesis
inflation
NO NEED FOR THE NP SCALE TO BE CLOSE TO THE ELW. SCALE
The Energy Scale from the “Theoretical” New Physics
Stabilization of the electroweak symmetry breaking at MW calls for an ULTRAVIOLET COMPLETION of the SM already ULTRAVIOLET COMPLETION of the SM already
at the TeV scaleat the TeV scale +
CORRECT GRAND UNIFICATION “CALLS” FOR NEW PARTICLES CORRECT GRAND UNIFICATION “CALLS” FOR NEW PARTICLES AT THE ELW. SCALEAT THE ELW. SCALE
LE “COSTANTI” DI ACCOPPIAMENTO FONDAMENTALI
NON SONO COSTANTI
DA G.U.T. A SUSY G.U.T.
Aggiunta di nuove particelle SUSY partner di quelle ordinarie del Modello Standard ad una scala di massa tra 100 e 1000 GeV
Di cosa è fatto l'Universo?
EVIDENCE FOR DMEVIDENCE FOR DM
MODIFICARE LA GRAVITA’ (MOND)
• DM e’ sempre derivata dalle osservazioni assumendo la validita’ della legge standard della gravita’ possibile evitare l’introduzione di DM se modifico la legge di gravita’ su varie scale astronomiche
• Possibili problemi per CDM • Fit di MOND a >100 curve di rotazione galattiche con
successo • Problemi a riprodurre i dati relativi alla dinamica di
clusters: necessita’ di introdurre materia invisibile (neutrini, barioni oscuri)
• Versione relativistica di MOND ( Tensor-Vector Scalar Th. - TeVeS) + covarianza ( Bekenstein ’04, Sanders ’05)
• TeVeS : OK per strong lensing, invece necessita di materia invisibile per riprodurre il weak lensing. Barioni oscuri necessari anche per fenomeni quali il Bullet Cluster ( Milgrom ’08)
The BULLET CLUSTER: two colliding clusters of galaxies
Stars, galaxies and putative DM behave differently during collision, allowing for them to be studied separately. In MOND the lensing is expected to follow the baryonic matter, i.e. the X-ray gas. However the lensing is strongest in two
separated regions near the visible galaxies most of the mass in the cluster pair is in the form of collisionless DM
La conoscenza che abbiamo riguarda solo il 4% dell’Universo il resto è ancora ignoto !!
1% Stelle
7% Gas nelle galassie
7% Gas
85% Materia Oscura
materia barionica
materia non barionica
Inventario della materia nell’ Universo
ik ij jk jk4
1 8πGR - g R+Λg = T
2 c
Equazione del Campo di Gravitazione
Costante Cosmologica
Albert Einstein (1879-1955)
LA COSTANTE COSMOLOGICA SORGENTE LA COSTANTE COSMOLOGICA SORGENTE DELL’ENERGIA OSCURA DELL’UNIVERSO E CAUSA DELL’ENERGIA OSCURA DELL’UNIVERSO E CAUSA DELLA SUA ESPANSIONE ACCELERATA?DELLA SUA ESPANSIONE ACCELERATA?
Bilancio energetico dell’Universo
PROBLEMA DELL’ENERGIA DEL VUOTO O DELLA COSTANTE COSMOLOGICA
??
IS THE FINE-TUNING A REAL PROBLEM?
• WARNING: THERE EXISTS AN EVEN “LARGER” HIERARCHY OR FINE -TUNING OR NATURALNESS PROBLEM: THE COSMOLOGICAL CONSTANT PROBLEM (“ THE MOTHER” OF ALL NATURALNESS PROBLEMS); SO FAR, WE SIMPLY “ACCEPT” SUCH FINE-TUNING!
• (OUTRAGEOUS) POSSIBILITY: THE “THEORY OF EVERYTHING” COULD BE UNIQUE, BUT WITH MANY (INFINITE?) VACUA EACH GIVING RISE TO A DIFFERENT UNI-VERSE ( MULTI-VERSE POSSIBILITY). WE CAN LIVE ONLY IN THE VERY RESTRICTED CLASS OF THE “MULTI-VERSE SPACE” WHERE THE “BOUDARY CONDITIONS” ( FOR INSTANCE, THE VALUE OF THE COSMOLOGICAL CONSTANT OR THE SCALE OF THE ELW.SYMMETRY BREAKING AND, HENCE, THE HIGGS MASS) EXHIBIT VALUES ALLOWING FOR THE CORRECT BBN, LSS,… OUR LIFE!
ANTHROPIC PRINCIPLE
UNIUNI -- VERSOO
MULTIMULTI -- VERSO• Tutta l’evoluzione dell’Universo (asimmetria tra
materia ed antimateria, nucleosintesi, formazione delle galassie, ammassi, etc., sistema solare, vita sulla Terra etc.) dipende in maniera molto stretta dal preciso valore assunto da alcuni parametri fondamentali ( tra questi quello della costante cosmologica): e’ possibile che quello in cui noi siamo sia solo uno dei moltissimi –versi ( MULTI – VERSO) ?
DM DM NEW PHYSICS BEYOND THE NEW PHYSICS BEYOND THE ( ( PARTICLE PHYSICSPARTICLE PHYSICS ) SM - ) SM - if Newton is right if Newton is right
at scales>size of the Solar Systemat scales>size of the Solar System
• ΩDM = 0.233 ± 0.013 *
• Ωbaryons = 0.0462 ± 0.0015 ***from CMB ( 5 yrs. of WMAP) + Type I Supernovae + Baryon Acoustic Oscillations (BAO)
**CMB + TypeI SN + BAO in agreement with Nucleosynthesis (BBN)
LA MATERIA OSCURAMATERIA OSCURA E’ QUANTITATIVAMENTEQUANTITATIVAMENTE E QUALITATIVAMENTEQUALITATIVAMENTE LA PIU’ IMPRESSIONANTE EVIDENZA
DI NUOVA FISICA OLTRE IL MS PARTICELLARENUOVA FISICA OLTRE IL MS PARTICELLARE
• QUANTITATIVE: Taking into account the latest WMAP data which in combination with LSS data provide stringent bounds 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 NOT enough to provide a mass to neutrinos to obtain a valid DM candidate; LSS formation requires DM to be COLD NEW PARTICLES NOT INCLUDED IN THE SPECTRUM OF THE FUNDAMENTAL BUILDING BLOCKS OF THE SM !
SONO I NEUTRINI LA MATERIA OSCURANEUTRINI LA MATERIA OSCURA?SIC TRANSIT GLORIA MUNDI
• Massive neutrinos: only candidates in the SM to account for DM. From here the “prejudice” of neutrinos of a few eV to correctly account for DM
• Neutrinos decouple at ~1 MeV ; being their mass<<decoupling temperature, neutrinos remain relativistic for a long time. Being very fast, they smooth out any possible growth of density fluctuation forbidding the formation of proto-structures.
• The “weight” of neutrinos in the DM budget is severely limited by the observations disfavoring scenarios where first superlarge structures arise and then galaxies originate from their fragmentation
LSS PATTERN AND NEUTRINO MASSES
(E..g., Ma 1996)
m = 0 eV m = 1 eV
m = 7 eV m = 4 eV
Cosmological Bounds on the sum of the masses of the 3 neutrinos from increasingly rich samples of data sets
LA MATERIA OSCURA QUALE CHIAVE DI ACCESSO ALLA
NUOVA FISICA OLTRE IL MS: PUO’ LA PARTICELLA DI LA PARTICELLA DI
MATERIA OSCURA ESSERE IL MATERIA OSCURA ESSERE IL PRIMO SEGNALE DELLA PRIMO SEGNALE DELLA
NUOVA FISICA ALLANUOVA FISICA ALLA
SCALA ELETTRODEBOLESCALA ELETTRODEBOLE ??
THE “WIMP MIRACLEWIMP MIRACLE”
Tante le possibilita’, ma gli WIMP sono speciali : singolare coincidenza tra param. dei MODELLI STANDARD PART. e COSM. per dare validi candidati di DM proprio alla scala eletttrodebole (TeV)
Bergstrom
WIMPS (Weakly Interacting Massive
Particles)
#~# m
# exp(-m/T)# does not change any more
Tdecoupl. typically ~ m /20
depends on particle physics (annih.) and “cosmological” quantities (H, T0, …
h2_ ~ 10-3
<(annih.) V > TeV2
~ 2 / M2 From T0 MPlanck
h2 in the range 10-2 -10-1 to be cosmologically interesting (for DM)
m ~ 102 - 103 GeV (weak interaction) h2 ~ 10-2 -10-1 !!!
THERMAL RELICS (WIMP in thermodyn.equilibrium with the
plasma until Tdecoupl)
COSMO – PARTICLE
CONSPIRACY
HOW TO COPE WITH THE HIERARCHY PROBLEM
• LOW-ENERGY SUSY
• LARGE EXTRA DIMENSIONS
• DYNAMICAL SYMMETRY BREAKING OF THE ELW. SYMMETRY
• LANDSCAPE APPROACH (ANTHROPIC PRINCIPLE)
STABLE ELW. SCALE WIMPs from STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS PARTICLE PHYSICS
1) ENLARGEMENT OF THE SM
SUSY EXTRA DIM. LITTLE HIGGS. (x, ) (x, ji) SM part + new part
Anticomm. New bosonic to cancel 2
Coord. Coord. at 1-Loop2) SELECTION RULE
DISCRETE SYMM.
STABLE NEW PART.
R-PARITY LSP KK-PARITY LKP T-PARITY LTP
Neutralino spin 1/2 spin1 spin0
3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + ΩL h2 OK
* But abandoning gaugino-masss unif. Possible to have mLSP down to 7 GeV
mLSP
~100 - 200
GeV *
mLKP
~600 - 800
GeV
mLTP
~400 - 800
GeV
Bottino, Donato, Fornengo, Scopel
SUSY & DM : a successful marriage
• Supersymmetrizing the SM does not lead necessarily to a stable SUSY particle to be a DM candidate.
• However, the mere SUSY version of the SM is known to lead to a too fast p-decay. Hence, necessarily, the SUSY version of the SM has to be supplemented with some additional ( ad hoc?) symmetry to prevent the p-decay catastrophe.
• Certainly the simplest and maybe also the most attractive solution is to impose the discrete R-parity symmetry
• MSSM + R PARITY LIGHTEST SUSY PARTICLE (LSP) IS STABLE .
• The LSP can constitute an interesting DM candidate in several interesting realizations of the MSSM ( i.e., with different SUSY breaking mechanisms including gravity, gaugino, gauge, anomaly mediations, and in various regions of the parameter space).
WHO IS THE LSP?
• SUPERGRAVITY ( transmission of the SUSY breaking from the hidden to the obsevable sector occurring via gravitational interactions): best candidate to play the role of LSP:
NEUTRALINO ( i.e., the lightest of the four eigenstates of the 4x4 neutralino mass matrix)
In CMSSM: the LSP neutralino is almost entirely a BINO
WHICH SUSY
HIDDEN SECTOR SUSY BREAKING AT
SCALE F
OBSERVABLE SECTOR
SM + superpartnersMSSM : minimal content
of superfields
ME
SS
EN
GE
RSF = MW MPl
GRAVITY
Mgravitino ~ F/MPl ~
(102 -103) GeV
GAUGE INTERACTIONS
F = (105 - 106) GeV
Mgravitino ~ F/MPl ~
(102 - 103) eV
NEUTRALINO LSP IN THE CONSTRAINED MSSSM:
A VERY SPECIAL SELECTION IN THE PARAMETER SPACE?
Ellis, Olive, Santoso, Spanos
Excluded: stau LSP
Excluded by bsγ
Favored by gµ -2
Favored by DM
After LEP: tuning of the SUSY param. at the % level to correctly reproduce
the DM abundance: NEED FOR A “WELL-TEMPERED” NEUTRALINO
MA SIAMO SICURI CHE LA MA SIAMO SICURI CHE LA MATERIA OSCURAMATERIA OSCURA SIA SIA LEGATA LEGATA SOLAMENTESOLAMENTE A NUOVA FISICA OLTRE IL A NUOVA FISICA OLTRE IL
MODELLO STANDARD PARTICELLAREMODELLO STANDARD PARTICELLARE??
• LA PIU’ LONTANA INFORMAZIONE ( AFFIDABILE) CHE ABBIAMO SULLE PRIME FASI DELL’UNIVERSO E’ LA NUCLEOSINTESI ( t > 1 sec. dopo il Big Bang)
• PRIMA DELLA NUCLEOSINTESI L’EVOLUZIONE ( ad es. la velocita’ di espansione) DELL’UNIVERSO POTEVA DIFFERIRE SIGNIFICATIVAMENTE DAL QUADRO DELLA COSMOLOGIA STANDARD DEL BIG BANG CALDO CON PROFONDE IMPLICAZIONI SULL’ABBONDANZA E NATURA DELLA MATERIA OSCURA
DM and NON-STANDARD COSMOLOGIES BEFORE NUCLEOSYNTHESIS
• NEUTRALINO RELIC DENSITY MAY DIFFER FROM ITS STANDARD VALUE, i.e. the value it gets when the expansion rate of the Universe is what is expected in Standard Cosmology (EX.: SCALAR-TENSOR THEORIES OF GRAVITY, KINATION, EXTRA-DIM. RANDALL-SUNDRUM TYPE II MODEL, ETC.)
• WIMPS MAY BE “COLDER”, i.e. they may have smaller typical velocities and, hence, they may lead to smaller masses for the first structures which form GELMINI, GONDOLO
LARGER WIMP ANNIHILATION CROSS-SECTION IN NON-STANDARD COSMOLOGIES
• Having a Universe expansion rate at the WIMP freeze-out larger than in Standard Cosmology possible to provide a DM adequate WIMP population even in the presence of a larger annihilation cross-section ( Catena, Fornengo, A.M., Pietroni)
• Possible application to increase the present DM annihilation rate to account for the PAMELA results in the DM interpretation (instead of other mechanisms like the Sommerfeld effect or a nearby resonance)
El Zant, Khalil, Okada
WIMPs: proviamo a “fabbricarli” anche noi !
L’IPOTESI “WIMPS”
MATERIA OSCURA COSTITUITA DA PARTICELLE “NUOVE” CON MASSA TRA 100 E 1000 GEV CHE INTERAGISCONO SOLO DEBOLMENTE
LHC, ILC (LINEAR COLLIDER )POSSONO PRODURRE WIMPS
WIMPS scappano dal rivelatore
“FIRMA” DELL’HIGGS:
ENERGIA MANCANTE
DALLA MISURA DI MATERIA OSCURA POSSO RISALIRE A QUANTO GLI WIMPS INTERAGISCANO CON LA MATERIA ORDINARIA E QUINDI PREDIRE LA QUANTITA’ DI WIMPS CHE PRODURRO’ A LHC O A ILC
PREDICTION OF Ω DM FROM LHC AND ILC FOR TWO DIFFERENT SUSY PARAMETER SETS
BALTZ, BATTAGLIA, PESKIN, WIZANSKY
HUNTING FOR DARK MATTER
DIRECT DM SEARCHES
INDIRECT DM SEARCHES
ELLIS, OLIVE, SAVAGE
Neutralino-nucleon scattering cross sections along the WMAP-allowed coannihilation strip for tanbeta=10 and coannihilation/funnel strip for tanbeta=50 using the hadronic parameters
Ellis, Olive, Sandick
LHC Sensitivity
PROSPECTS FOR DISCOVERING THE CMSSM AT THE LHC IN LIGHT OF WMAP
RED: FULL SAMPLE OF CMMS MODELS
BLUE: POINTS COMPATIBLE WITH WMAP
GREEN: POINTS ACCESSIBLE TO LHC
YELLOW: POINTS ACCESSIBLE TO PRESENT DIRECT DM SEARCHES
Ellis et al.
MODULAZIONE DEL SEGNALE DI MODULAZIONE DEL SEGNALE DI INTERAZIONE TRA MATERIA INTERAZIONE TRA MATERIA
OSCURA E NUCLEI-BERSAGLIOOSCURA E NUCLEI-BERSAGLIO
“VENTO DI MATERIA
OSCURA “ VARIA A
SECONDA DELLA
VELOCITA’ DELLA TERRA
DM INDIRECT DETECTIONDM INDIRECT DETECTION
RICERCA INDIRETTA DI MATERIA OSCURA• ANNICHILAZIONE WIMP-ANTIWIMPANNICHILAZIONE WIMP-ANTIWIMP
• RILEVANTI PRODOTTI DELL’ANNICHILAZIONE :RILEVANTI PRODOTTI DELL’ANNICHILAZIONE : I) I) FOTONI AD ALTA ENERGIAFOTONI AD ALTA ENERGIA II) II) NEUTRINI AD ALTA ENERGIANEUTRINI AD ALTA ENERGIA III) III) ANTIMATERIA ANTIMATERIA
I) I) ASTRONOMIA GAMMA: telescopi a terra ( es. MAGIC alle ASTRONOMIA GAMMA: telescopi a terra ( es. MAGIC alle Canarie o ARGO in Tibet ) o nello spazio ( es. AGILE e Canarie o ARGO in Tibet ) o nello spazio ( es. AGILE e FERMI)FERMI)
II) II) TELESCOPI DI NEUTRINI: sotto il ghiaccio del polo TELESCOPI DI NEUTRINI: sotto il ghiaccio del polo (AMANDA), o sotto il mare ( ANTARES, Marsiglia, in futuro (AMANDA), o sotto il mare ( ANTARES, Marsiglia, in futuro NEMO, Capo Passero, Sicilia)NEMO, Capo Passero, Sicilia)
III) III) ANTIMATERIA: ricerche di eccessi di antiprotoni o ANTIMATERIA: ricerche di eccessi di antiprotoni o positroni in esperimenti spaziali (PAMELA su razzo russo, positroni in esperimenti spaziali (PAMELA su razzo russo, AMS sulla ISS)AMS sulla ISS)
INDIRECT SEARCHES OF DM• WIMPs collected inside celestial bodies ( Earth, Sun):
their annihilations produce energetic neutrinos • WIMPs in the DM halo: WIMP annihilations can take place
( in particular, their rate can be enhanced with there exists a CLUMPY distribution of DM as computer simulations of the DM distribution in the galaxies seem to suggest. From the WIMP annihilation:
-- energetic neutrinos ( under-ice, under-water exps Amanda, Antares, Nemo, Nestor, …)
--photons in tens of GeV range ( gamma astronomy on ground Magic, Hess, … or in space Agile, Glast…)
--antimatter: look for an excess of antimatter w.r.t. what is expected in cosmic rays ( space exps. Pamela, AMS, …)
PAMELA excess: October 2008, stimulated enormous theoretical activity; note: statistical errors only! Fermi: feature observed by ATIC not confirmed
Strumia
EPS09
Pulsars: Fermi & PAMELA
pulsar parameters “randomly” varied!
Grasso et al
1) Necessario innalzare la sezione d’uro di annichilazione OGGI rispetto a quella presente quando gli WIMP si sono disaccoppiati nel primo Universo
2) SUSY WIMP piuttosto pesanti m> 1 TeV
Strumia
EPS09
THE “WHY NOW” PROBLEM
DM DEDO THEY “KNOW” EACH OTHER?
DIRECT INTERACTION (quintessence) WITH DARK MATTER DANGER:
Very LIGHTm ~ H0
-1 ~ 10-33 eVThreat of violation of the equivalence principle constancy of the fundamental “constants”,…
INFLUENCE OF ON THE NATURE AND THE ABUNDANCE OF CDM
Modifications of the standard picture of WIMPs FREEZE - OUTCDM CANDIDATES
CATENA, FORNENGO, A.M., PIETRONI, SCHELKE
COMPONENTE SCALARE DELLA GRAVITA’ IN COMPONENTE SCALARE DELLA GRAVITA’ IN AGGIUNTA ALLA SOLITA COMPONENTE TENSORIALE?AGGIUNTA ALLA SOLITA COMPONENTE TENSORIALE?
S. Katsanevas ASPERA
FCNC, CP ≠, (g-2), ()0 m n …
LINKED TO COSMOLOGICAL EVOLUTION
Possible interplay with dynamical DE
NEWNEWPHYSICS ATPHYSICS AT
THE ELW THE ELW SCALESCALE
DM - FLAVOR
for DISCOVERY
and/or FUND. TH.
RECONSTRUCTION
A MAJOR LEAP AHEAD IS NEEDED
LFV
NEUTRINO PHYSICSLEPTOGENESIS
TEVATRON I L C
MICRO MACROMODELLO STANDARDMODELLO STANDARD PARTICELLARE: COSTITUENTI E INTERAZIONI FONDAMENTALI
MODELLO STANDARDMODELLO STANDARDCOSMOLOGICO:
HOT BIG BANG
MATRIMONIO FELICEMATRIMONIO FELICEES: NUCLEOSINTESI
MA ANCHE PUNTI DI ATTRITO
MATERIA ED ENERGIA OSCURAMATERIA ED ENERGIA OSCURA
LHC LHC UNA ECCEZIONALE FINESTRA PER UNA ECCEZIONALE FINESTRA PER ESPLORARE L’UNIVERSO E LA SUA ORIGINEESPLORARE L’UNIVERSO E LA SUA ORIGINE