We consider the possibility to gain information on the lepton mixing matrix element
<mml:math id="E2" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mrow><mml:mo>|</mml:mo><mml:mrow><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mi>e</mml:mi><mml:mn>3</mml:mn></mml:mrow></mml:msub></mml:mrow><mml:mo>|</mml:mo></mml:mrow></mml:mrow></mml:math> from an improved experimental limit on the effective neutrino mass governing
neutrinoless double beta decay. We show that typically a lower limit on <mml:math id="E3" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mrow><mml:mo>|</mml:mo><mml:mrow><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mi>e</mml:mi><mml:mn>3</mml:mn></mml:mrow></mml:msub></mml:mrow><mml:mo>|</mml:mo></mml:mrow></mml:mrow></mml:math> as a function of the smallest neutrino mass can be set. Furthermore, we give the values of the sum of neutrino masses and <mml:math id="E4" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mrow><mml:mo>|</mml:mo><mml:mrow><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mi>e</mml:mi><mml:mn>3</mml:mn></mml:mrow></mml:msub></mml:mrow><mml:mo>|</mml:mo></mml:mrow></mml:mrow></mml:math> which are allowed and forbidden by an experimental upper limit on the effective mass. Alternative explanations for neutrinoless double beta decay, Dirac neutrinos or unexplained cosmological features would be required if future measurements showed that the values lie in the respective regions. Moreover, we show that a measurement of <mml:math id="E5" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mrow><mml:mo>|</mml:mo><mml:mrow><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mi>e</mml:mi><mml:mn>3</mml:mn></mml:mrow></mml:msub></mml:mrow><mml:mo>|</mml:mo></mml:mrow></mml:mrow></mml:math> from neutrinoless double beta decay is very difficult due to the expected errors on the effective mass and the oscillation parameters.

Alexander Merle

Werner Rodejohann

Getting Information on <svg style="vertical-align:-3.3907pt" height="20.0625" version="1.1" viewBox="0 0 39.625 20.0625" width="39.625" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg"><g transform="matrix(.017,-0,0,-.017,.062,15.775)"><path id="x7C" d="M162 -163h-61v866h61v-866z" /></g><g transform="matrix(.017,-0,0,-.017,4.533,15.775)"><path id="x1D448" d="M751 650l-6 -28q-53 -1 -69 -12.5t-24 -38.5q-23 -85 -43 -192l-13 -69q-34 -181 -130 -262q-79 -65 -185 -65t-171 57q-87 77 -54 258l42 232q12 58 0.5 73t-75.5 19l8 28h263l-6 -28q-63 -5 -78 -18t-26 -74l-41 -226q-25 -135 22 -201t139 -66q99 0 161.5 68t91.5 217&#xA;l11 57q28 149 28 193q0 28 -19 38t-79 12l6 28h247z" /></g><g transform="matrix(.012,-0,0,-.012,17.5,19.863)"><path id="x1D452" d="M391 364q0 -28 -20.5 -53.5t-50 -43.5t-70 -34t-73.5 -25t-68 -17v-29q0 -48 20 -81t65 -33q73 0 157 76l16 -23q-107 -113 -221 -113q-21 0 -40.5 6.5t-39 22t-31.5 47t-12 75.5q0 69 33.5 139.5t95.5 114.5q77 55 143 55q42 0 69 -24.5t27 -59.5zM313 350&#xA;q0 26 -14.5 40.5t-37.5 14.5q-32 0 -44 -7q-82 -46 -104 -175q200 49 200 127z" /></g><g transform="matrix(.012,-0,0,-.012,22.426,19.863)"><path id="x33" d="M285 378v-2q65 -13 102 -54.5t37 -97.5q0 -57 -30.5 -104.5t-74 -75t-85.5 -42t-72 -14.5q-31 0 -59.5 11t-40.5 23q-19 18 -16 36q1 16 23 33q13 10 24 0q58 -51 124 -51q55 0 88 40t33 112q0 64 -39 96.5t-88 32.5q-29 0 -64 -11l-6 29q77 25 118 57.5t41 84.5&#xA;q0 45 -26.5 69.5t-68.5 24.5q-67 0 -120 -79l-20 20l43 63q51 56 127 56h1q66 0 107 -37t41 -95q0 -42 -31 -71q-22 -23 -68 -54z" /></g><g transform="matrix(.017,-0,0,-.017,28.762,15.775)"><use xlink:href="#x7C"/></g><g transform="matrix(.012,-0,0,-.012,33.238,7.613)"><path id="x32" d="M412 140l28 -9q0 -2 -35 -131h-373v23q112 112 161 170q59 70 92 127t33 115q0 63 -31 98t-86 35q-75 0 -137 -93l-22 20l57 81q55 59 135 59q69 0 118.5 -46.5t49.5 -122.5q0 -62 -29.5 -114t-102.5 -130l-141 -149h186q42 0 58.5 10.5t38.5 56.5z" /></g></svg> from Neutrinoless Double Beta Decay

Three (or four) straightforward experiments would contribute greatly to completing the
spectroscopy of baryons and light mesons. In the baryon sector, data are needed on inelastic
reactions from a polarised target with <mml:math id="E1" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mi>π</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:mrow></mml:math> and <mml:math id="E2" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mi>K</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:mrow></mml:math> beams up to <mml:math id="E3" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mo>∼</mml:mo></mml:math> 3 GeV/c. Similar data are
needed in the light meson sector for <mml:math id="E4" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mover accent="true"><mml:mi>p</mml:mi><mml:mo>¯</mml:mo></mml:mover><mml:mi>p</mml:mi></mml:mrow></mml:math> interactions in the momentum range 0.3–2 GeV/c.
In both cases, valuable information is to be obtained from longitudinal (L) and sideways
(S) target polarisations as well as the conventional normal (N) polarisation. Thirdly, <mml:math id="E5" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mn>3</mml:mn><mml:msub><mml:mi>S</mml:mi><mml:mn>1</mml:mn></mml:msub></mml:mrow></mml:math> and <mml:math id="E6" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mn>3</mml:mn><mml:msub><mml:mi>D</mml:mi><mml:mn>1</mml:mn></mml:msub></mml:mrow></mml:math> mesons in the mass range 1–2.4 GeV could probably be separated either
by diffractive dissociation of transversely polarised photons or by <mml:math id="E7" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msup><mml:mi>e</mml:mi><mml:mo>+</mml:mo></mml:msup><mml:msup><mml:mi>e</mml:mi><mml:mo>−</mml:mo></mml:msup></mml:mrow></mml:math> radiative return experiments using transversely and longitudinally polarised electrons.

D. V. Bugg

Experiments Needed in Meson and Baryon Spectroscopy

Following our recent work on the cosmological constant problem, in this letter we make
a specific proposal regarding the fine structure (i.e., the spectrum) of dark energy. The
proposal is motivated by a deep analogy between the blackbody radiation problem, which
led to the development of quantum theory, and the cosmological constant problem, for 
which we have recently argued calls for a conceptual extension of the quantum theory. We
argue that the fine structure of dark energy is governed by a Wien distribution, indicating
its dual quantum and classical nature. We discuss observational consequences of such a
picture of dark energy and constrain the distribution function.

Vishnu Jejjala

Michael Kavic

Djordje Minic

Fine Structure of Dark Energy and New Physics

It is well known that one cannot construct a self-consistent quantum field
theory describing the nonrelativistic electromagnetic interaction mediated
by massive photons between a point-like electric charge and a magnetic
monopole. We show that, indeed, this inconsistency arises in the classical
theory itself. No semiclassic approximation or limiting procedure for <mml:math id="E1" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>&#x210f;</mml:mi><mml:mo>&#x2192;</mml:mo><mml:mtext>0</mml:mtext></mml:mrow></mml:math>
 is used. As a result, the string attached to the monopole emerges as visible also if finite-range electromagnetic
interactions are considered in classical framework.

C. Cafaro

S. Capozziello

Ch. Corda

S. A. Ali

Can Magnetic Monopoles and Massive Photons Coexist in the Framework of the Same  Classical Theory?

We compute the effect of nondiagonal neutrino mass in 
<mml:math id="E2" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>l</mml:mi><mml:mrow><mml:mi>i</mml:mi></mml:mrow></mml:msub><mml:mo>&#x2192;</mml:mo><mml:msub><mml:mi>l</mml:mi><mml:mi>j</mml:mi></mml:msub><mml:mi>&#x3b3;</mml:mi></mml:math> in Supersymmetry (SUSY) theories with nontrivial quark-lepton
complementarity and a flavor symmetry.
The correlation matrix <mml:math id="E3" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>V</mml:mi><mml:mi>M</mml:mi></mml:msub></mml:math> 
= <mml:math id="E4" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mtext>CKM</mml:mtext></mml:mrow></mml:msub><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mtext>PMNS</mml:mtext></mml:mrow></mml:msub></mml:math> is such that its
(1,3) entry, as preferred by the present experimental data, is zero.
We do not assume that <mml:math id="E5" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>V</mml:mi><mml:mi>M</mml:mi></mml:msub></mml:math> is bimaximal. Quark-lepton complementarity and the flavor symmetry strongly constrain
the theory and we obtain a clear prediction for the contribution to <mml:math id="E6" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>&#x3bc;</mml:mi><mml:mo>&#x2192;</mml:mo><mml:mi>e</mml:mi><mml:mi>&#x3b3;</mml:mi></mml:mrow></mml:math> and the <mml:math id="E7" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>&#x3c4;</mml:mi></mml:math> decays
<mml:math id="E8" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>&#x3c4;</mml:mi><mml:mo>&#x2192;</mml:mo><mml:mi>e</mml:mi><mml:mi>&#x3b3;</mml:mi></mml:math>
 and <mml:math id="E9" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>&#x3c4;</mml:mi><mml:mo>&#x2192;</mml:mo><mml:mi>&#x3bc;</mml:mi><mml:mi>&#x3b3;</mml:mi></mml:math>. If the Dirac neutrino Yukawa couplings are degenerate but the
low-energy neutrino masses are not degenerate, then the
lepton decays are related among them by the <mml:math id="E10" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>V</mml:mi><mml:mi>M</mml:mi></mml:msub></mml:math> entries. On the other hand, if the Dirac neutrino Yukawa couplings are
hierarchical or the low-energy neutrino masses are degenerate,
then the prediction for the lepton decays comes from the <mml:math id="E11" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>U</mml:mi><mml:mrow><mml:mtext>CKM</mml:mtext></mml:mrow></mml:msub></mml:math> hierarchy.

Marco Picariello

Predictions for <svg style="vertical-align:-3.56265pt" height="12.175" version="1.1" viewBox="0 0 56.4375 12.175" width="56.4375" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg"><g transform="matrix(.017,-0,0,-.017,.062,7.675)"><path id="x1D707" d="M538 96q-38 -45 -84 -76.5t-71 -31.5q-44 0 -15 117q12 49 18 89h-2q-99 -128 -163 -178q-36 -28 -70 -28q-26 0 -44 38h-2q-16 -69 -16 -129q0 -43 11 -75.5t24 -42.5l1 -6q-7 -12 -24.5 -23t-37.5 -11q-40 0 -40 76q0 52 35 202l94 407l78 24l5 -5q-32 -122 -72 -310&#xA;q-7 -33 0 -55t25 -22q36 0 105.5 75t107.5 145l32 146l75 26h10q-50 -197 -78 -347q-7 -38 6 -38q7 0 31 17t47 39z" /></g><g transform="matrix(.017,-0,0,-.017,17.044,7.675)"><path id="x2192" d="M901 255q-71 -62 -185 -187l-22 15l102 147h-727v50h727l-102 147l22 15q114 -125 185 -187z" /></g><g transform="matrix(.017,-0,0,-.017,40.809,7.675)"><path id="x1D452" d="M391 364q0 -28 -20.5 -53.5t-50 -43.5t-70 -34t-73.5 -25t-68 -17v-29q0 -48 20 -81t65 -33q73 0 157 76l16 -23q-107 -113 -221 -113q-21 0 -40.5 6.5t-39 22t-31.5 47t-12 75.5q0 69 33.5 139.5t95.5 114.5q77 55 143 55q42 0 69 -24.5t27 -59.5zM313 350&#xA;q0 26 -14.5 40.5t-37.5 14.5q-32 0 -44 -7q-82 -46 -104 -175q200 49 200 127z" /></g><g transform="matrix(.017,-0,0,-.017,47.846,7.675)"><path id="x1D6FE" d="M478 372q0 -39 -31 -97t-61 -98t-78 -98q-45 -55 -73 -102q-13 -79 -13 -197q-11 -11 -43.5 -25.5t-53.5 -15.5l-15 17q5 35 26 101.5t47 123.5q8 72 -1.5 174.5t-37.5 178.5q-14 37 -29 37q-20 0 -67 -65l-25 21q37 60 73 90.5t63 30.5q47 0 72 -112q13 -56 17.5 -141.5&#xA;t0.5 -143.5h2q155 193 155 297q0 26 -12 47q-5 8 -5 15q0 16 12.5 27t29.5 11q21 0 34 -21t13 -55z" /></g></svg> in Supersymmetry from Nontrivial Quark-Lepton Complementarity and Flavor Symmetry

We use the corrections to the Newton-Einstein secular precessions 
of the longitudes of the perihelia of the inner planets, 
phenomenologically estimated  E.V. Pitjeva by fitting almost one 
century of data with the EPM2004 ephemerides, to constrain some 
long-range models of modified gravity recently put forth to 
address the dark energy and dark matter problems. They are the 
four-dimensional ones obtained with the addition of inverse powers 
and logarithm of some curvature invariants, and the DGP 
multidimensional braneworld model. After working out the 
analytical expressions of the secular perihelion precessions 
induced by the corrections to the Newtonian potential of such 
models, we compare them to the estimated extra-rates 
of perihelia by taking their ratio for different pairs of planets 
instead of using one perihelion at a time for each planet 
separately, as done so far in literature. The curvature 
invariants-based models are ruled out, even by rescaling by a 
factor 10 the errors in the estimated planetary orbital 
parameters. Less neat is the situation for the DGP model. Only the 
general relativistic Lense-Thirring effect, not included, as the 
other exotic models considered here, by Pitjeva in the EPM force 
models, passes such a test.

Lorenzo Iorio

Astronomical Constraints on Some Long-Range Models of Modified Gravity

With a view towards applications for de Sitter, we construct the multiparametric <mml:math id="E1" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>q</mml:mi></mml:math>-deformation of the so<mml:math id="E2" xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mo>(</mml:mo><mml:mrow><mml:mn>5</mml:mn><mml:mo>,</mml:mo><mml:mi>ℂ</mml:mi></mml:mrow><mml:mo>)</mml:mo></mml:mrow></mml:math> algebra using the Faddeev-Reshetikhin-Takhtadzhyan (FRT)
formalism.

Chethan Krishnan

Edoardo Di Napoli

Multiparametric Quantum Algebras and the Cosmological Constant

Toy models of a nonassociative quantum mechanics are presented. The Heisenberg equation of
motion is modified using a nonassociative commutator. Possible physical applications of a nonassociative
quantum mechanics are considered. The idea is discussed that a nonassociative algebra
could be the operator language for the nonperturbative quantum theory. In such approach the
nonperturbative quantum theory has observables and unobservables quantities.

Vladimir Dzhunushaliev

Toy Models of a Nonassociative Quantum Mechanics

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<p><em>Advances in High Energy Physics</em> publishes the results of theoretical and experimental research on the nature of, and interaction between, energy and matter.</p>


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<p>Chief Editor, Professor Seidel, is a professor in the Department of Physics and Astronomy at the University of New Mexico. She is a collaborator on the ATLAS experiment at the Large Hadron Collider, researching high-energy collider physics.</p>


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Advances in High Energy Physics publishes the results of theoretical and experimental research on the nature of, and interaction between, energy and matter.

Advances in High Energy Physics