Search for excited fermions with the H1 detector

Adloff, C.; Aïd, S.; Anderson, M.; Andreev, V.; Andrieu, Bernard; Arndt, C.; Babaev, A.; Bähr, J.; Bán, J.; Ban, Y.; Baranov, P.; Barrelet, E.; Barschke, R.; Bartel, W.; Barth, M.; Bassler, U.; Beck, M.; Beck, H. P.; Behrend, H. J.; Belousov, A.; Berger, Ch.; Bernardi, G.; Bertrand-Coremans, G.; Besançon, M.; Beyer, R.; Biddulph, P.; Bispham, P.; Bizot, J.C.; Blobel, V.; Borras, K.; Botterweck, F.; Boudry, V.; Braemer, A.; Braunschweig, W.; Brisson, V.; Brückner, W.; Bruel, P.; Bruncko, D.; Brune, C. R.; Buchholz, R.; Büngener, L.; Bürger, J.; Büsser, F.W.; Buniatian, A.; Bürke, S.; Burton, M. J.; Calvet, D.; Campbell, A.; Carli, T.; Charlet, M.; Clarke, D.; Clegg, A.B.; Clerbaux, B.; Cocks, S.; Contreras, J. G.; Cormack, C. M.; Coughlan, J. A.; Courau, A.; Cousinou, M. C.; Cozzika, G.; Criegee, L.; Cussans, D.; Cvach, J.; Dagoret, S.; Dainton, J. B.; Dau, W.D.; Daum, K.; David, M.; Davis, C. L.; Delcourt, B.; Roeck, A. De; Wolf, E. A. De; Dirkmann, M.; Dixon, P.; Nezza, P. 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W.; Henschel, H.; Herynek, I.; Heß, M.; Hewitt, K.; Hildesheim, W.; Hiller, K. H.; Hilton, C.D.; Hladký, J.; Höppner, M.; Hoffmann, D.; Holtom, T.; Horisberger, R.; Hudgson, V. L.; Hütte, M.; Ibbotson, M.; Itterbeck, H.; Jachołkowska, A.; Jacobsson, C.; Jaffré, M.; Janoth, J.; Jansen, D. M.; Jansen, Thomas L. C.; Jönsson, L.; Johnson, D.P.; Jung, H.; Kalmus, P. I. P.; Kander, M.; Kant, D.; Kaschowitz, R.; Kathage, U.; Katzy, J.; Kaufmann, H. H.; Kaufmann, O.; Kausch, M.; Kazarian, Shahé S.; Kenyon, I. R.; Kermiche, S.; Keuker, C.; Kiesling, C.; Klein, M.; Kleinwort, C.; Knies, G.; Köhler, Thomas; Köhne, J. H.; Kolanoski, H.; Kolya, S. D.; Korbel, V.; Kostka, P.; Kotelnikov, S.K.; Krämerkämper, T.; Krasny, M. W.; Krehbiel, H.; Krücker, D.; Küster, H.; Kuhlen, M.; Kurča, T.; Kurzhöfer, J.; Lacour, D.; Laforge, B.; Landon, M. P. 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G.; Wittek, C.; Wobisch, M.; Wünsch, E.; Žáček, J.; Zarbock, D.; Zhang, Z.; Zhokin, A.; Zini, P.; Zomer, F.; Zsembery, J.; Zuber, Κ.; zurNedden, M.

doi:10.1016/s0550-3213(96)00591-3

Cited by 77 publications

(138 citation statements)

References 18 publications

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“…The value of this parameter depends on the infrared matching scale. For µ I = 2 GeV, fits of event shapes of untagged events gave α 0 ≃ 0.5 [1,9,[11][12][13].…”

Section: Merging Perturbative and Non-perturbative Contributionsmentioning

confidence: 99%

“…Although the magnitude of the correction cannot be predicted by perturbative means, the power p and the relative coefficients among different observables can be calculated using the assumption of infrared freezing. This universality hypothesis has proved to give a phenomenologically fairly consistent picture of power corrections [8][9][10][11][12][13], and the same results could be derived using a different method, the so-called renormalon approach [14,15].…”

Section: Introductionmentioning

confidence: 99%

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Calculation of power corrections to hadronic event shapes of tagged b events

Trocsanyi¹

2000

J. High Energy Phys.

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We compute power corrections to mean values of hadronic event shapes -the thrust and the C parameter -of tagged b quark events in electron positron annihilation, using the dispersive approach. We find that the leading power corrections are of the same type of 1/Q corrections as for event shapes in the massless case, with the same non-perturbative coefficient times a perturbatively calculable mass-dependent coefficient. The effect of the mass correction in the power correction is to reduce the latter by 10-30 % for tagged b events, for centre-of-mass energies ranging from the Z 0 peak down to 20 GeV.

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“…The value of this parameter depends on the infrared matching scale. For µ I = 2 GeV, fits of event shapes of untagged events gave α 0 ≃ 0.5 [1,9,[11][12][13].…”

Section: Merging Perturbative and Non-perturbative Contributionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Calculation of power corrections to hadronic event shapes of tagged b events

Trocsanyi¹

2000

J. High Energy Phys.

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“…In Fig. 5 we show by stars quantum limits given by Compton wave length, by white triangles electromagnetic experimental upper limits coming mainly from reaction e + e − − − → γγ(γ) [37], by shaded squares experimental electro-weak limits [38], by dark triangles geometrical limits on sizes calculated from Eq. (33) with ρ 0 of the electro-weak scale 246 GeV, and by dark squares the most stringent lower limits on sizes of particles as extended objects.…”

Section: Test 1: Limits On Sizes Of Fundamental Particlesmentioning

confidence: 99%

Cosmological Term, Mass, and Space-Time Symmetry

Dymnikova

2004

Beyond the Desert 2003

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In the spherically symmetric case the requirements of regularity of density and pressures and finiteness of the ADM mass m, together with the weak energy condition, define the family of asymptotically flat globally regular solutions to the Einstein minimally coupled equations which includes the class of metrics asymptotically de Sitter as r → 0. A source term connects smoothly de Sitter vacuum in the origin with the Minkowski vacuum at infinity and corresponds to anisotropic vacuum defined macroscopically by the algebraic structure of its stress-energy tensor which is invariant under boosts in the radial direction. Dependently on parameters, geometry describes vacuum nonsingular black holes, and self-gravitating particle-like structures whose ADM mass is related to both de Sitter vacuum trapped in the origin and smooth breaking of space-time symmetry. The geometry with the regular de Sitter center has been applied to estimate geometrical limits on sizes of fundamental particles, and to evaluate the gravito-electroweak unification scale from the measured mass-squared differences for neutrino. * Talk I. THE EINSTEIN COSMOLOGICAL TERMWhich arrow does fly forever? An arrow which hits the goal.Vladimir NabokovIn 1917 Einstein introduced a cosmological term into his equations describing gravity as space-time geometry (G-field) generated by matterto make them consistent with Mach's principle, one of his basic motivations [1], which reads: some matter has the property of inertia only because there exists also some other matter in the Universe [2]. When Einstein found that Minkowski geometry is the regular solution to (1) without source termperfectly describing inertial motion in the absence of a matter, he modified his equations by adding the cosmological term Λg µν in the hope that modified equationswill have reasonable regular solutions only when mattaer is present (if matter is the source of inertia, then in case of its absence there should not be any inertia [3]). The by-product of this hypothesis was the static Einstein cosmology in which the task of Λ was to make a universe The story of abandoning Λ by Einstein is typically told as dominated by successes of FRW cosmology confirmed by Hubble's discovery of the Universe expansion.In reality the first reason was de Sitter solution: soon after introducing Λg µν , in the same year 1917, de Sitter found quite reasonable solution to the equation (3) with T µν = 0,which made evident that a matter is not necessary to produce the property of inertia [4]. In de Sitter geometry [5]Λ must be constant by virtue of the contracted Bianchi identitiesIt plays the role of a universal repulsion whose physical sense remained obscure during several decades when de Sitter geometry has been mainly used as a simple testing ground for developing the quantum field technics in a curved space-time. In 1965 two papers shed some light on the physical nature of the de Sitter geometry. In the first Sakharov suggested that gravitational effects can dominate an equation of state at superhigh densi...

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“…The H1 data [15] give for the q * → qg decay channel a compositeness scale Λ. For a q * of mass 100 GeV the limit on Λ moves from 60 GeV to 290 GeV.…”

Section: Experimental Limits On the Sizes Of Fundamental Particlesmentioning

confidence: 99%

“…The H1 data [15] describe for the e * case the electromagnetic and weak decay channel. For the ν * the channel ν * → νγ is measured.…”

Section: Experimental Limits On the Sizes Of Fundamental Particlesmentioning

confidence: 99%

Limits on sizes of fundamental particles and on gravitational mass of a scalar

Dymnikova

Ulbricht

Zhao

2001

AIP Conference Proceedings

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Abstract. We review the experimental limits on mass of excited fundamental particles and contact interaction energy scale parameters Λ for QCD, QED and electroweak reactions. In particular we have focused on the QED reaction e + e − → γγ(γ) at the energies from 91GeV to 202GeV using the differential cross-sections measured by the L3 Collaboration from 1991 to 1999. A global fit leads to lower limits at 95% CL on Λ > 1687 GeV, which restricts the characteristic QED size of the interaction region to R e < 1.17 × 10 −17 cm. All the interaction regions are found to be smaller than the Compton wavelength of the fundamental particles. This constraint is used to estimate a lower limit on the size of a fundamental particle related to gravitational interaction, applying the model of self-gravitating particle-like structure with the de Sitter vacuum core. It gives r τ ≥ 2.3 × 10 −17 cm and r e ≥ 1.5 × 10 −18 cm, if leptons get masses at the electroweak scale, and r τ ≥ 3.3 × 10 −27 cm, r e ≥ 4.9 × 10 −26 cm, as the most stringent limits required by causality arguments. This sets also an upper limit on the gravitational mass of a scalar m scalar ≤ 154 GeV at the electroweak scale and m scalar ≤ 3/8m P l as the most stringent limit.

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Search for excited fermions with the H1 detector

Cited by 77 publications

References 18 publications

Calculation of power corrections to hadronic event shapes of tagged b events

Calculation of power corrections to hadronic event shapes of tagged b events

Cosmological Term, Mass, and Space-Time Symmetry

Limits on sizes of fundamental particles and on gravitational mass of a scalar

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