Neutrino Mass Origin of Matter: Probing at LHC . R. N. Mohapatra MPI-Heidelberg Seminar,2009. Universe is full of matter and “no” anti-matter. How do we know ? (i) Solar probes have not exploded- (ii) Sun sends us billions of particles and no
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R. N. Mohapatra
(i) Solar probes have not exploded-
(ii) Sun sends us billions of particles and no
antiparticles since there are no natural fireworks
in the sky-
(iii) Anti-matter fraction in cosmic rays: 1 in 10,000
(completely understandable in terms of known
Not tenable since inflation empties the universe—
(Blanchet, Chacko, Granor, RNM: arXiv:0904.2974)
sym. of SM:
whereas even with TeV MR, (more reasonable)
B-L breaking crucial to seesaw:
Minkowski; Gell-Mann, Ramond Slansky,Yanagida, R.N.M.,Senjanovic,Glashow
of SM (‘t Hooft) (Kuzmin,Rubakov,Shaposnikov)
GUT - GeV- Small neutrino mass could be indication for SUSYGUT;
Many interesting SO(10) GUT models.
(corresponding Yukawa~ ) ;
(Liu and Segre’94; Covi et al’95 ; Flanz et al.’95 Pilaftsis’97)
they have gravitinos with TeV mass that are produced during inflation reheat along with all SM particles-
No such conflict for TeV scale leptogenesis !! Goes well with collider friendly TeV seesaw !
cross section observable
only if mixing is >
~100 GeV implies Not observable at LHC.
mixings as in generic neutrino models.
to break symmetry to implement seesaw, if no new physics upto Planck scale.
2.5 TeV Z’
(Del Aguila, Aguilar-Saavedra; Aguilar-Saavedra )
(i)RH neutrinos must be degenerate in mass;
since h >10^-5 degeneracy ok anywhere from ;technically natural and enough for baryogenesis!
(ii) Since there are fast processes at that temperature, the net lepton asymmetry and primordial lepton asym are related by
where <1 (efficiency factor); depends on rates for Z’ med. scatt. ;inverse decay
(Buchmuller,di Bari Plumacher)
Yes; MZ’ > 2.5 TeV for MZ’ > 2MN
very small so that ~0.1-1;
visible at LHC:
(i) RH nu’s are Majorana masses whereas q, l masses
(ii) RH masses arise at different scale and from a
different mechanism (B-L breaking) as against the
Q, L masses which arise from SM symmetry br.
(iii) Already large neutrino mixings are an indication
that in the seesaw formula RH neutrinos must
have some peculiarity.
with RH nu’s triplet under O(3)H – all other fermion fields singlet.
willerase lepton asymmetry.
(Frere, Hambye and Vertongen)
- Sym br. to U(1)I3RxU(1)B-L SM at TeV-
to do resonant leptogenesis.
the dominant process does not occur. We need
to avoid the WR bound.
Leptogenesis possible but visible only for ~1.
1. Rapid p-decay due to
2. Neutrino mass not easy
3. EW baryo in a corner
of parameter space.
4. Light Higgs and stop
5. DM gravitino/Neutra
+ h. c.
leading to B-violating decays
MS < 500-700 GeV to get right amount of baryons.
arises via the diagram:
(I) Single production:
xsection calculated in (RNM, Okada, Yu’07;) resonance peaks above
SM background- decay to tt or tj depending on RH nu
Majorana coupling; directly measures seesaw parameters.
(II) Drell-Yan pair production:
( Chen, Klem, Rentala, Wang, 08)
Diquark has a baryon number & LHC is ``pp’’ machine
Depends on Yukawa coupling
using like sign dilepton mode.
Constraints by rare processes
Similarly B-B-bar etc. Can generate neutrino masses - satisfying FCNC