Review of Particle Physics

Amsler, C.; Doser, M.; Antonelli, M.; Asner, D. M.; Babu, K. S.; Baer, Howard; Band, H. R.; Barnett, R. M.; Bergren, E.; Beringer, J.; Bernardi, G.; Bertl, W.; Bichsel, H.; Biebel, O.; Bloch, P.; Blucher, E.; Blusk, S.; Cahn, R. N.; Carena, Marcela; Caso, C.; Ceccucci, A.; Chakraborty, D.; Chen, M.-C.; Chivukula, R. Sekhar; Cowan, G.; Dahl, O. I.; D’Ambrosio, Giancarlo; Damour, Thibault; Gouvêa, A. de; DeGrand, Thomas; Dobrescu, Bogdan A.; Drees, M.; Edwards, D. A.; Eidelman, S.; Elvira, V. D.; Erler, Jens; Ежела, В. В.; Feng, Jonathan L.; Fetscher, W.; Fields, Brian D.; Foster, B.; Gaisser, T. K.; Garren, L.; Gerber, H.J.; Gerbier, G.; Gherghetta, Tony; Giudice, Gian F.; Goodman, M. C.; Grab, C.; Gritsan, A. V.; Grivaz, J.-F.; Groom, D. E.; Grünewald, M.; Gurtu, A.; Gutsche, Thomas; Haber, Howard E.; Hagiwara, K.; Hagmann, C.; Hayes, K.; Hernández-Rey, J. J.; Hikasa, K.; Hinchliffe, I.; Höcker, A.; Huston, J.; Igo‐Kemenes, P.; Jackson, John D.; Johnson, K. F.; Junk, T. R.; Karlen, D.; Kayser, Boris; Kirkby, D.; Klein, Sebastian; Knowles, I.G.; Kolda, Christopher; Kowalewski, R.; Kreitz, P.; Krusche, B.; Kuyanov, Yu.V.; Kwon, Y. J.; Lahav, O.; Langacker, Paul; Liddle, Andrew R.; Ligeti, Zoltan; Lin, C.; Liss, T. M.; Littenberg, Laurence; Liu, J.C.; Lugovsky, K. S.; Lugovsky, S. B.; Mahlke, Hanna; Mangano, M.; Mannel, Thomas; Manohar, Aneesh V.; Marciano, William J.; Martin, A. D.; Masoni, A.; Milstead, D.; Miquel, R.; Mönig, K.; Murayama, Hitoshi; Nakamura, K.; Narain, M.; Nason, Paolo; Navas, S.; Nevski, P.; Nir, Yosef; Olive, Keith A.; Pape, L.; Patrignani, C.; Peacock, J.; Piepke, A.; Punzi, G.; Quadt, A.; Raby, Stuart; Raffelt, Georg G.; Ratcliff, B. N.; Renk, B.; Richardson, Peter; Roesler, S.; Rolli, S.; Romaniouk, A.; Rosenberg, L.; Rosner, Jonathan L.; Sachrajda, Christopher; Sakai, Y.; Sarkar, S.; Sauli, F.; Schneider, O.; Scott, D. M.; Seligman, W.; Shaevitz, M. H.; Sjöstrand, Torbjörn; Smith, J. G.; Smoot, George F.; Spanier, S. M.; Spieler, H.; Stahl, A.; Stanev, T.; Stone, S.; Sumiyoshi, T.; Tanabashi, Masaharu; Terning, John; Titov, M.; Ткаченко, Н. П.; Törnqvist, Nils A.; Tovey, D. R.; Trilling, G. H.; Trippe, T. G.; Valencia, G.; Bibber, K. van; Vincter, MG; Vogel, P.; Ward, D. R.; Watari, Taizan; Webber, B.R.; Weiglein, G.; Wells, James D.; Whalley, M. A.; Wheeler, Amanda; Wohl, C.G.; Wolfenstein, Lincoln; Womersley, J.; Woody, C.; Workman, R.L.; Yamamoto, A.; Yao, W-M.; Zenin, O.; Zhang, J.; Zhu, R. Y.; Żyla, P.; Harper, G.; Lugovsky, V. S.; Schaffner, Paul E.

doi:10.1016/j.physletb.2008.07.018

Cited by 4,761 publications

(5,534 citation statements)

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“…In fact, substituting the present experimental values of the charged lepton masses [2], the formula is valid within the present experimental accuracies. The relative experimental error of the left-hand side (l.h.s. )…”

Section: Jhep05(2009)075supporting

confidence: 68%

“…Comparing to the present experimental bound Br(K L → eµ) < 4.7 × 10 −12 [2], we obtain a limit v 2 5 × 10 2 TeV. Naively this limit may already be marginally in conflict with the estimated unification scale in the above scenario.…”

Section: Jhep05(2009)075supporting

confidence: 55%

“…2 Since the values of mτ and vew are known, once we choose the values of v3/M ′ ( 3) and y1, y2, y3(≈ 1), the value of v3/M ( 0.03) will be fixed. Then the mass eigenvalues corresponding to the SM charged leptons can be computed in series expansion in the small parameters vew/M ′ , vi/M and Figure 2.…”

Section: Jhep05(2009)075mentioning

confidence: 99%

“…(3.16), which constrains the form of the radiative correction by the U(3) gauge bosons. To achieve this, we need additional fields or dynamics, such as an SU(2) doublet scalar field whose VEV breaks SU (2). As yet, we have not succeeded to incorporate such a mechanism consistently into our model.…”

Section: Relevant Scales and Further Assumptionsmentioning

confidence: 99%

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Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Sumino

2009

J. High Energy Phys.

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Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum Abstract: Koide's mass formula is an empirical relation among the charged lepton masses which holds with a striking precision. We present a model of charged lepton sector within an effective field theory with U(3) × SU(2) family gauge symmetry, which predicts Koide's formula within the present experimental accuracy. Radiative corrections as well as other corrections to Koide's mass formula have been taken into account. We adopt a known mechanism, through which the charged lepton spectrum is determined by the vacuum expectation value of a 9-component scalar field Φ. On the basis of this mechanism, we implement the following mechanisms into our model: (1) The radiative correction induced by family gauge interaction cancels the QED radiative correction to Koide's mass formula, assuming a scenario in which the U(3) family gauge symmetry and SU(2) L weak gauge symmetry are unified at 10 2 -10 3 TeV scale; (2) A simple potential of Φ invariant under U(3) × SU(2) leads to a realistic charged lepton spectrum, consistent with the experimental values, assuming that Koide's formula is protected; (3) Koide's formula is stabilized by embedding U(3) × SU(2) symmetry in a larger symmetry group. Formally fine tuning of parameters in the model is circumvented (apart from two exceptions) by appropriately connecting the charged lepton spectrum to the boundary (initial) conditions of the model at the cut-off scale. We also disucss some phenomenological implications.

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Section: Jhep05(2009)075supporting

confidence: 68%

Section: Jhep05(2009)075supporting

confidence: 55%

Section: Jhep05(2009)075mentioning

confidence: 99%

Section: Relevant Scales and Further Assumptionsmentioning

confidence: 99%

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Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Sumino

2009

J. High Energy Phys.

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“…with the help of equations (8) and (9). As in the framework of the standard solar model, we assumed that the number of 57 Fe nuclei per unit mass in the Sun is uniform, i.e., that N is independent of r. Using the standard solar model data for the temperature and mass density distributions in the Sun as functions of the radius r [44], we evaluated the integral in the above expression and found that…”

Section: Axion Emission From 57 Fe Nuclei In the Sunmentioning

confidence: 99%

Search for 14.4 keV solar axions emitted in the M1-transition of⁵⁷Fe nuclei with CAST

Andriamonje¹,

Aune²,

Autiero

et al. 2009

J. Cosmol. Astropart. Phys.

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Abstract. We have searched for 14.4 keV solar axions or more general axion-like particles (ALPs), that may be emitted in the M1 nuclear transition of 57 Fe, by using the axion-to-photon conversion in the CERN Axion Solar Telescope (CAST) with evacuated magnet bores (Phase I). From the absence of excess of the monoenergetic X-rays when the magnet was pointing to the Sun, we set model-independent constraints on the coupling constants of pseudoscalar particles that couple to two photons and to a nucleon g aγ | − 1.19 g 0 aN + g 3 aN | < 1.36 × 10 −16 GeV −1 for m a < 0.03 eV at the 95% confidence level.

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Weak Interaction

Hikasa

2009

Digital Encyclopedia of Applied Physics

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Review of Particle Physics

Cited by 4,761 publications

References 0 publications

Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Search for 14.4 keV solar axions emitted in the M1-transition of⁵⁷Fe nuclei with CAST

Weak Interaction

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Review of Particle Physics

Cited by 4,761 publications

References 0 publications

Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Family gauge symmetry as an origin of Koide's mass formula and charged lepton spectrum

Search for 14.4 keV solar axions emitted in the M1-transition of57Fe nuclei with CAST

Weak Interaction

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Search for 14.4 keV solar axions emitted in the M1-transition of⁵⁷Fe nuclei with CAST