OperaV1, PascalFrancis, Corpus, bibRecord, 000084

Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass

Identifieur interne : 000084 ( PascalFrancis/Corpus ); précédent : 000083; suivant : 000085

Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass

Auteurs : Daniele Fargion ; Daniele D'Armiento

Source :

Journal of physics. G. Nuclear and particle physics : (Print) [ 0954-3899 ] ; 2012.

RBID : Pascal:12-0326865

Descripteurs français

Pascal (Inist)
- CERN, Neutrino, Mélangeage, Masse neutrino, Supernova, Oscillation neutrino, Flaveur, Tachyon, Timing, Modèle, Détection neutrino, Graviton, Temps retard, Gravité, Neutronisation, Explosion supernova, Physique mathématique, Physique nucléaire, Particule sans masse, Masse particule élémentaire, Particule élémentaire.

English descriptors

KwdEn :
- CERN, Elementary particle mass, Elementary particles, Flavor, Gravitons, Gravity, Massless particles, Mathematical physics, Mixing, Models, Neutrino detection, Neutrino mass, Neutrino oscillations, Neutrinos, Neutronization, Nuclear physics, Supernovae, Supernovae explosion, Tachyons, Time delay, Timing.

Abstract

We tried to fit in any way the recent OPERA-CERN claims of a neutrino superluminal speed with the observed supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillations. We considered three main frameworks: (1) tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with the observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate the SN1987A burst but greatly disagrees with the energy-independent CERN-OPERA super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic v_e component and a superluminal v_μ) in an ad hoc frozen speed scenario that leads to the prompt neutrino de-coherence and rapid flavor mixing (between v_e and v_μ, v_τ) that are in conflict with most oscillation records. Therefore, we concluded that an error must be hidden in OPERA-CERN time calibration (as indeed recent rumors seem to confirm). We concluded recalling the relevance of the real guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a millisecond graviton-neutrino split time delay among the gravity burst and neutronization neutrino peak in any future supernova explosion in Andromeda recordable in the Megaton neutrino detector.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A11	`01`	`1`		`@1 FARGION (Daniele)`
A11	`02`	`1`		`@1 D'ARMIENTO (Daniele)`
A14	`01`			`@1 Physics Department, Rome University 1, Sapienza and INFN, Roma1 -PI A Moro 2 @2 00185 Rome @3 ITA @Z 1 aut. @Z 2 aut.`
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C01	`01`		`ENG`	@0 We tried to fit in any way the recent OPERA-CERN claims of a neutrino superluminal speed with the observed supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillations. We considered three main frameworks: (1) tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with the observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate the SN1987A burst but greatly disagrees with the energy-independent CERN-OPERA super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic v_e component and a superluminal v_μ) in an ad hoc frozen speed scenario that leads to the prompt neutrino de-coherence and rapid flavor mixing (between v_e and v_μ, v_τ) that are in conflict with most oscillation records. Therefore, we concluded that an error must be hidden in OPERA-CERN time calibration (as indeed recent rumors seem to confirm). We concluded recalling the relevance of the real guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a millisecond graviton-neutrino split time delay among the gravity burst and neutronization neutrino peak in any future supernova explosion in Andromeda recordable in the Megaton neutrino detector.
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C03	`03`	`3`	`ENG`	`@0 Mixing @5 28`
C03	`04`	`3`	`FRE`	`@0 Masse neutrino @5 29`
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C03	`05`	`3`	`FRE`	`@0 Supernova @5 30`
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C03	`06`	`3`	`FRE`	`@0 Oscillation neutrino @5 31`
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C03	`07`	`3`	`FRE`	`@0 Flaveur @5 32`
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C03	`09`	`3`	`FRE`	`@0 Timing @5 34`
C03	`09`	`3`	`ENG`	`@0 Timing @5 34`
C03	`10`	`X`	`FRE`	`@0 Modèle @5 35`
C03	`10`	`X`	`ENG`	`@0 Models @5 35`
C03	`10`	`X`	`SPA`	`@0 Modelo @5 35`
C03	`11`	`3`	`FRE`	`@0 Détection neutrino @5 36`
C03	`11`	`3`	`ENG`	`@0 Neutrino detection @5 36`
C03	`12`	`3`	`FRE`	`@0 Graviton @5 37`
C03	`12`	`3`	`ENG`	`@0 Gravitons @5 37`
C03	`13`	`3`	`FRE`	`@0 Temps retard @5 38`
C03	`13`	`3`	`ENG`	`@0 Time delay @5 38`
C03	`14`	`3`	`FRE`	`@0 Gravité @5 39`
C03	`14`	`3`	`ENG`	`@0 Gravity @5 39`
C03	`15`	`3`	`FRE`	`@0 Neutronisation @5 40`
C03	`15`	`3`	`ENG`	`@0 Neutronization @5 40`
C03	`16`	`X`	`FRE`	`@0 Explosion supernova @5 41`
C03	`16`	`X`	`ENG`	`@0 Supernovae explosion @5 41`
C03	`16`	`X`	`SPA`	`@0 Explosión supernova @5 41`
C03	`17`	`3`	`FRE`	`@0 Physique mathématique @5 42`
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C03	`18`	`3`	`FRE`	`@0 Physique nucléaire @5 43`
C03	`18`	`3`	`ENG`	`@0 Nuclear physics @5 43`
C03	`19`	`3`	`FRE`	`@0 Particule sans masse @5 44`
C03	`19`	`3`	`ENG`	`@0 Massless particles @5 44`
C03	`20`	`3`	`FRE`	`@0 Masse particule élémentaire @5 45`
C03	`20`	`3`	`ENG`	`@0 Elementary particle mass @5 45`
C03	`21`	`3`	`FRE`	`@0 Particule élémentaire @5 46`
C03	`21`	`3`	`ENG`	`@0 Elementary particles @5 46`
N21				`@1 247`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 12-0326865 INIST
ET :	Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass
AU :	FARGION (Daniele); D'ARMIENTO (Daniele)
AF :	Physics Department, Rome University 1, Sapienza and INFN, Roma1 -PI A Moro 2/00185 Rome/Italie (1 aut., 2 aut.)
DT :	Publication en série; Niveau analytique
SO :	Journal of physics. G. Nuclear and particle physics : (Print); ISSN 0954-3899; Coden JPGPED; Royaume-Uni; Da. 2012; Vol. 39; No. 8; 085002.1-085002.9; Bibl. 9 ref.
LA :	Anglais
EA :	We tried to fit in any way the recent OPERA-CERN claims of a neutrino superluminal speed with the observed supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillations. We considered three main frameworks: (1) tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with the observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate the SN1987A burst but greatly disagrees with the energy-independent CERN-OPERA super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic v_e component and a superluminal v_μ) in an ad hoc frozen speed scenario that leads to the prompt neutrino de-coherence and rapid flavor mixing (between v_e and v_μ, v_τ) that are in conflict with most oscillation records. Therefore, we concluded that an error must be hidden in OPERA-CERN time calibration (as indeed recent rumors seem to confirm). We concluded recalling the relevance of the real guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a millisecond graviton-neutrino split time delay among the gravity burst and neutronization neutrino peak in any future supernova explosion in Andromeda recordable in the Megaton neutrino detector.
CC :	001B20; 001B10
FD :	CERN; Neutrino; Mélangeage; Masse neutrino; Supernova; Oscillation neutrino; Flaveur; Tachyon; Timing; Modèle; Détection neutrino; Graviton; Temps retard; Gravité; Neutronisation; Explosion supernova; Physique mathématique; Physique nucléaire; Particule sans masse; Masse particule élémentaire; Particule élémentaire
ED :	CERN; Neutrinos; Mixing; Neutrino mass; Supernovae; Neutrino oscillations; Flavor; Tachyons; Timing; Models; Neutrino detection; Gravitons; Time delay; Gravity; Neutronization; Supernovae explosion; Mathematical physics; Nuclear physics; Massless particles; Elementary particle mass; Elementary particles
SD :	Modelo; Explosión supernova
LO :	INIST-577G.354000508344320050
ID :	12-0326865

Links to Exploration step

Pascal:12-0326865

Le document en format XML

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<front><div type="abstract" xml:lang="en">We tried to fit in any way the recent OPERA-CERN claims of a neutrino superluminal speed with the observed supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillations. We considered three main frameworks: (1) tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with the observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate the SN1987A burst but greatly disagrees with the energy-independent CERN-OPERA super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic v<sub>e</sub>
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, v<sub>τ</sub>
) that are in conflict with most oscillation records. Therefore, we concluded that an error must be hidden in OPERA-CERN time calibration (as indeed recent rumors seem to confirm). We concluded recalling the relevance of the real guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a millisecond graviton-neutrino split time delay among the gravity burst and neutronization neutrino peak in any future supernova explosion in Andromeda recordable in the Megaton neutrino detector.</div>
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 and v<sub>μ</sub>
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<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Neutronization</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE"><s0>Explosion supernova</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>Supernovae explosion</s0>
<s5>41</s5>
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<s5>41</s5>
</fC03>
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<s5>42</s5>
</fC03>
<fC03 i1="17" i2="3" l="ENG"><s0>Mathematical physics</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="3" l="FRE"><s0>Physique nucléaire</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="3" l="ENG"><s0>Nuclear physics</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Particule sans masse</s0>
<s5>44</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Massless particles</s0>
<s5>44</s5>
</fC03>
<fC03 i1="20" i2="3" l="FRE"><s0>Masse particule élémentaire</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="3" l="ENG"><s0>Elementary particle mass</s0>
<s5>45</s5>
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<fN21><s1>247</s1>
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<fN82><s1>OTO</s1>
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</pA>
</standard>
<server><NO>PASCAL 12-0326865 INIST</NO>
<ET>Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass</ET>
<AU>FARGION (Daniele); D'ARMIENTO (Daniele)</AU>
<AF>Physics Department, Rome University 1, Sapienza and INFN, Roma1 -PI A Moro 2/00185 Rome/Italie (1 aut., 2 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Journal of physics. G. Nuclear and particle physics : (Print); ISSN 0954-3899; Coden JPGPED; Royaume-Uni; Da. 2012; Vol. 39; No. 8; 085002.1-085002.9; Bibl. 9 ref.</SO>
<LA>Anglais</LA>
<EA>We tried to fit in any way the recent OPERA-CERN claims of a neutrino superluminal speed with the observed supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillations. We considered three main frameworks: (1) tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with the observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate the SN1987A burst but greatly disagrees with the energy-independent CERN-OPERA super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic v<sub>e</sub>
 component and a superluminal v<sub>μ</sub>
) in an ad hoc frozen speed scenario that leads to the prompt neutrino de-coherence and rapid flavor mixing (between v<sub>e</sub>
 and v<sub>μ</sub>
, v<sub>τ</sub>
) that are in conflict with most oscillation records. Therefore, we concluded that an error must be hidden in OPERA-CERN time calibration (as indeed recent rumors seem to confirm). We concluded recalling the relevance of the real guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a millisecond graviton-neutrino split time delay among the gravity burst and neutronization neutrino peak in any future supernova explosion in Andromeda recordable in the Megaton neutrino detector.</EA>
<CC>001B20; 001B10</CC>
<FD>CERN; Neutrino; Mélangeage; Masse neutrino; Supernova; Oscillation neutrino; Flaveur; Tachyon; Timing; Modèle; Détection neutrino; Graviton; Temps retard; Gravité; Neutronisation; Explosion supernova; Physique mathématique; Physique nucléaire; Particule sans masse; Masse particule élémentaire; Particule élémentaire</FD>
<ED>CERN; Neutrinos; Mixing; Neutrino mass; Supernovae; Neutrino oscillations; Flavor; Tachyons; Timing; Models; Neutrino detection; Gravitons; Time delay; Gravity; Neutronization; Supernovae explosion; Mathematical physics; Nuclear physics; Massless particles; Elementary particle mass; Elementary particles</ED>
<SD>Modelo; Explosión supernova</SD>
<LO>INIST-577G.354000508344320050</LO>
<ID>12-0326865</ID>
</server>
</inist>
</record>

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Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass

Inconsistency in super-luminal CERN-OPERA neutrino speed with the observed SN1987A burst and neutrino mixing for any imaginary neutrino mass

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