AMS-02, Antimatter, Strangelets , Cosmic Rays Nicolò Masi May 2012

1. AMS-02, Antimatter, Strangelets, Cosmic Rays NicolòMasi May 2012 Bologna University and INFN

2. AMS-02 and the Antiworld

3. Island of Antimatter? The CPT theorem assures that any particle species there exists the antiparticle with exactly the same mass and decay width and eventually opposite charges. This striking symmetry would naturally lead us to conclude that the Universe contains particles and antiparticles in equal number densities. The observed Universe is drastically different. We do not observe any bodies of antimatter within the solar system and only antiprotons in the cosmic rays, which are believed to be of extra solar origin. Antiprotons are likely to be produced as secondaries in collisions:

4. Search for Antimatter • 100 MeV g flux excludes wide antimatter regions up 50÷100 Mpc • Sakharov’s 3 Principles of Baryogenesis ….. • … but alternative models predict distant antimatter local domains • A single anti-He CR nucleus represents a strong evidence for Antimatter Domains in our Universe: antistars, antigalaxies and cosmological remnants • We need : • - very large statistics of primary CRs • - very good particle identification, including charge sign reconstruction

5. Expected Goal for Antinuclei Search Antihelium/HeliumFlux Ifwereachthisvaluewe can affirm antiworlddoesn’texist 10 years

6. ANTIMATTER in this Universe: And if it really not existed?

7. When?: Big Bang Timeline • Planck Epoch:10-44÷10–43 seconds after the Big Bang • Grand Unification epoch • 10–43÷10–36 seconds after the Big Bang, T ∼ 1015 GeV • Gravitation begins to separate from the fundamental gauge interactions. Physics may be described by GUT in which the gauge group of the Standard Model is embedded in a much larger group, which is broken to produce the observed forces of nature. • Electroweak epoch • 10–36÷10–12 seconds after the Big Bang, T ∼ 1014 ÷103 GeV • The temperature of the universe is low enough (1028 K) to separate the strong force from the electroweak force. This phase transition triggers a period of exponential expansion known as cosmic inflation. After inflation ends, particle interactions are still energetic enough to create large numbers of exotic particles, including W, Z and H.

8. Inflationary epoch • 10–36÷10–32 seconds after the Big Bang, T ≲ 1013 GeV • The universe is flattened (its spatial curvature reaches the so called critical value) and the universe enters a homogeneus and isotropic rapidly expanding. Some energy from photons becomes virtualquarks and hyperons, but these particles decay quickly. • According to the ΛCDM model, dark energy is present as a property of space itself, beginning immediately following the period of inflation. • ⇒Reheating • T ∼ 107 ÷104GeV • The exponential de Sitter-like expansion that occurred during inflation ceases and the potential energy of the inflaton, the inflation field, decays into a hot, relativistic plasma of particles. The universe is dominated by radiation; quarks, electrons and neutrinos form. • ⇒ Baryogenesis: Yes or No?

9. The magic words for a cosmologist of baryogenesis

10. Finite Temperature EffectivePotential (FTEP): the Evolution of the Mexican-hat for Finite temperature phasetransitions D E Coleman –Weinberg Potential Inflaton

11. CP Violation: 𝛈 problem BaryonAsymmetryParameter ABaryonicAsimmetry B tinyvaluefor the cosmologicalsynthesis We need a correct amount of CP Violation A link between B and CP Standard Model CP Violation: A Great Disagreement

12. CMB vs 𝛈 ratio Dependence of the CMB Doppler peaks on 𝛈

13. Primordial Abundances Nucleosynthesis versus η Etadetermines light nuleicosmicratios

14. Baryogenesis (Riotto, Trodden) • Via Electroweak Phase Transition - SM compatible • Via Leptogenesis - sterile neutrinos • GUT Processes - SU(5) • Via Scalar Field (CPT Violation)

15. Anomalous B-violating processes Sakharov Criteria • B violation • C & CP violation • Nonequilibrium dynamics Prevent washout by inverse processes Sakharov, 1967 Baryogenesis: Ingredients We start from nullbaryonicnumber and baryonasimmetry: B = 0 and 𝛈 = 0 How can we create a B violation?

16. Anomalies: Standard Model borders Itinducesadditionalterms in the EW action and notconservedcurrents Baryonic Leptonic Chiral The Anomalyisdescribed by the Chern-Simonscurrent

17. B+L Anomaly: the Sphaleron BaryonicNumber Chern-SimonsNumber 0 Non NoetherBaryonic and LeptonicCurrents B + L not conserved B - L conserved Not conserved Fermionic Numbers and CS Numbers

18. Electroweak Sphaleronic Baryogenesis This process trades three leptons, one from each generation, for nine quarks, three within each generation, and one of each color per generation. L and B are not conserved separately , though the quantum number B − L is. With a 1° orderPhaseTransition, a FTEP and a calibratedHiggsMechanism, we can trigger the B numberviolationprocess

19. Baryons via Leptogenesis: Sterile Neutrinos • A simple modification of the Standard Model that is able to realize the program of Sakharov is the one suggested by M. Fukugita and T. Yanagida. • The Standard Model is extended by adding right-handed neutrinos, permitting implementation of the see-saw mechanism and providing the neutrinos with mass. At the same time, the extended model is able to spontaneously generate leptons from the decays of right-handed neutrinos. • Finally, the sphalerons are able to convert the spontaneously generated lepton asymmetry into the observed baryonic asymmetry.

20. Sterile Neutrinos If an asymmetry in the lepton number is produced, sphaleron transition, which conserve B - L, will reprocess it and convert it into baryon number. GUT SO(10): Majorana Neutrinos decay out-of-equilibrium

21. GUT Baryogenesis SU(5): Leptoquark and X Bosons scalar Departure from Equilibrium: X decay – itsatisfiesallSakharovconditions

22. Scalar or Quintessential Baryogenesis (De Felice, Nasri & MT; Li, Wang, Feng & Zhang) Spontaneous Baryogenesis(Cohen & Kaplan) • If CPT simmetry is broken, 𝛈 asymmetry can be generated in equilibrium. • We can’t break CPT explicitly but, if broken spontaneously, we can generate a baryon asymmetry. • A single scalar field may be responsible for inflation, baryogenesis and dark energy.

23. Bounds and Tests: Some Problems • EW: Only a small window of parameter space in extensions of the EW theory in which baryogenesis is viable; severe upper bound on lightest Higgs boson mass, mh< 120GeV, stop mass close to experimental bound and < top quark mass (Light Higgs and Stop Scenario): truly disadvantagedby LHC measurements. • Lepto and GUT: Heavy Majorana neutrinos, more massive than the 10 TeVsphaleron, and superheavy bosons, with fine tuning. Or maybe we simply missed an antiuniverse… Testability???

24. New Physics: Strangelets

25. New Physics: Strangelets

27. From quark stars A lot of new unexpectedstuff 10 years

28. Last butnotleast:CosmicRaysPhysics

29. Cosmic Rays • AMS measures: • |Z| independently in the Tracker, TOF and RICH subdetectors • Momentum in the tracking system. • Velocity independently by the TOF, TRD and RICH subdetectors.

30. CR Propagation CR PropagationModels with DM: Steady-state Parker Equation with a primaryflux source term Number density Diffusioncoefficient ConvectiveGalactic Wind Annihilation Rate DM Flux Source PropagationParameters From B/C and Be IsotopesMeasures

31. CR Propagation Constraint Average residence time in the Galaxy Averagegrammage (traversedmatter) Light nuclei ratios to fix the propagationparameters and improve the accuracy of GALPROPand DRAGON software