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TeraLeptons in Sinister Universe by D.Fargion and M.Khlopov in hep-ph/0507087

TeraLeptons in Sinister Universe by D.Fargion and M.Khlopov in hep-ph/0507087. The paper was inspired by last : Sheldon L. Glashow and Andy Cohen A Sinister Extension of the Standard Model to SU(3)XSU(2)XSU(2)XU(1) in hep-ph/0504287. Sinister model solving Sea saw and Dark Matter Problems.

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TeraLeptons in Sinister Universe by D.Fargion and M.Khlopov in hep-ph/0507087

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  1. TeraLeptons in Sinister Universeby D.Fargion and M.Khlopovin hep-ph/0507087 The paper was inspired by last: Sheldon L. Glashow and Andy Cohen A Sinister Extension of the Standard Model to SU(3)XSU(2)XSU(2)XU(1) in hep-ph/0504287 Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  2. Sinister model solving Sea saw and Dark Matter Problems Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  3. Abstract • The role of Sinister Heavy Fermions in recent Glashow's SU(3)*SU(2)*SU(2)'*U(1) model is to offer in a unique frame relic Helium-like products (an ingenious candidate to the dark matter puzzle), a solution to the See-Saw mechanism for light neutrino masses as well as to strong CP violation problem in QCD. Their mass are million times larger than common ones • The Sinister model requires a three additional families of leptons and quarks, but only the lightest of them Heavy U-quark and E-"electron" are stable. U E Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  4. Final neutral Helium-like UUUEE state is an ideal evanescent dark-matter candidate. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  5. Why Tera-helium is a good Dark Matter gas? • Teraparticles do not have normal W and Z interactions and do not contribute into SM parameters, so they can not be excluded by precision measurements of SM parameters • CP' symmetry of Glashow’s model helps to solve strong CP violation problem in QCD. • Tera-neutrino is unstable, because it gives Dirac see-saw mass to normal neutrino. • UUU as the new form of hadron - bound by ChromoCoulomb forces. It's size is about 1/alpha_QCD m_U about 10^-16 cm and it weakly interacts with hadrons. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  6. However UUUEE it is reached by multi-body interactions along a tail of more manifest secondary frozen blocks in analogy to He,Li,D. They should be now here polluting the matter. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  7. Tera Leptons in Glashow’s Sinister Universe • Moreover, in opposition to almost effective pair Tera-Quark U annihilations (like common proton-anti-proton), there is no such an early or late Tera-Lepton pairs suppressions, because: • a) electromagnetic interactions are "weaker" than nuclear ones because their coupling is smaller and mainly because the cross sections is proportional to inverse square Tera-Lepton Mass • b) helium ion 4He++ is able to attract and capture, E-, fixing it into a hybrid tera helium "ion" trap. This takes place during the first few minutes of the Universe Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  8. Why Grave Shadows over theSinister universe? • The helium ion 4He++ capture of E- leads to a pile up of relic (4HeE)+ traces, a lethal compound for any Sinister Universe. • This capture leaves no Tera-Lepton frozen in Ep relic (otherwise an ideal catalyzer to achieve effective late E+E- annihilations possibly saving the model). • The (4HeE)+ Coulomb screening is also avoiding the synthesis of the desired UUUEE hidden dark matter gas. The e(4HeE)+ behave chemically like an anomalous hydrogen isotope. • Also tera-positronium (eE+) relics are over-abundant and they behave like an anomalous hydrogen atom: Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  9. Consequences and Shadows • these hydrogen-like gases do not fit by many orders of magnitude known severe bounds on hydrogen anomalous isotope, making grave shadows over a Sinister Universe. • However a surprising and resolver role for Tera-Pions in UHECR astrophysics has been revealed. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  10. Masses of Tera Quark-Leptons Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  11. Brief History of Sinister Universe Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  12. Later Tera-Particle evolution Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  13. Why U- Anti U Annihilate Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  14. Why Tera Lepton do not annihilate Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  15. First Second Relics Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  16. Real Trap Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  17. The anomalous hydrogen relic Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  18. A surprising Role of Tera Pions in UHECR Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  19. Novel Candidate To UHECR • A different and more exciting role may come from the Tera-Hadron UHE secondary of the top-down UHECR source: the birth of neutral Tera-Mesons U-anti-u and u-anti-U. • Contrary to early Universe, where there is enough time and hard dense matter to proceed in the very complex cooking of Tera-Hadrons relics summarized in present article, tera quarks born by UHECR source escape mostly as neutral U-Anti-u and u-Anti-U. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  20. pair production energy loss -resonance pion production energy loss multi-pion production pion production rate The Greisen-Zatsepin-Kuzmin (GZK) cut-off Ultra High Energy Nucleons may produce pions on the 2.75 K BBR  nucleon • sources must be nearby (Local SuperCluster) • Or Neutrino Mediated (Z- Shower Model) Or Lorentz symmetry breaking. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  21. THE UHECR puzzle: Isotropy –Homogeneity- BL Lac correlation Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  22. New Particles and New Interactions Motivated by possible correlations of UHECR with high redshift objects: Gorbunov et al 2002 HIRES 2005 If this is confirmed, one can only think of 3 possibilities: 1.) Neutrino primaries but Standard Model interaction probability in atmosphere is ~10-5. • resonant (Z0) secondary production on massive relic neutrinos: needs extreme parameters and huge neutrino fluxes. • strong interactions above ~1TeV: only moderate neutrino fluxes required. 2.) New heavy neural (SUSY) hadron X0: m(X0) > mNincreases GZK cut-off threshold. but basically ruled out by constraints from accelerator experiments. 3.) New weakly interacting light (keV-MeV) neutral particle electromagnetic coupling small enough to avoid GZK effect; hadronic coupling large enough to allow normal air showers: very tough to do. BUT now Neutral Tera Pion maybe the source Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  23. Tera Pions escaping GZK: • These hybrid pions are very exceptional candidates to UHECR because two surprising abilities. • The first is that they interact hadronically with matter. This may imply a high altitude atmosphere interaction on Earth in agreement with the observed UHECR fluorescence light curve. • The second ability is a very smart interaction with radiation: indeed while the photo-pion production with matter takes place as for all the common nucleons (either proton or neutrons), the threshold in the "center of mass frame" for tera-pions is much higher. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  24. Are UHECR meta-stable Tera Neutral Pions? • The photo-pion production for neutrons onto the 2.75 K^o BBR begins at Lorentz factor 4 10^{10} and energy E = 4 10^{19} eV while for a corresponding Lorentz factor the Hybrid Tera-Pion threshold energy • E is 1.4 10^{23} eV, is above three order of magnitude higher simply because of the huge Tera-pion mass respect nucleon one. • This imply that for Tera-Pion there is a GZK cut off much above common {Greisen}{Zatsepin, Kuzmin} energies E= 4 10^{19} eV making this rare UHE tera-pion an ideal candidate able to travel along the whole Universe without deflection of Galactic or Extra-galactic magnetic fields or much energy losses, overcoming the otherwise controversial absence of a GZK cut-off. These Tera-pions are among the best candidate to solve recent UHECR correlated events with far BL-Lac sources {Gorbunov et al 2005}{HiRes,ICRC 2005}. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

  25. Conclusions: • No Sinister Dark Matter Cosmology because the Tera-Lepton Shadows hanging over the model. But possible role for meta-stable Tera-pions Uu and uU originated in Jets by BL Lac or in TD evaporation, able to travel undeflected and with no energy loss behaving as nuclear matter. Explaning Hires data with no Z-Burst need. Thank You for your attention. Gran Sasso-12-Sept-2005-Particle phys. and Astroph. beyond TeV-Tera Leptons..by D.Fargion

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