Neutrino Oscillations Hint at a New Fundamental Interaction

Transcription

1 Nutrino Oscillations Hint at a Nw Fundamntal Intraction Mario Evraldo d Souza Dpartamnto d Física, Univrsidad Fdral d Srgip, São Cristóvão, Srgip, Brazil Abstract It is suggstd that nutrino oscillations do not xist and, in th light of th latst rsults of July 2016 of th Daya Bay Collaboration and th rcnt discovry of a nw fundamntal intraction, it is proposd that th nutrino production at th Sun s cor in th pp and CNO cycls ar much largr than what is prdictd by th Standard Solar Modl, xactly bcaus of this nw intraction. Thrfor, th claimd nutrino dficits on Earth ar compltly mislading. 1. Introduction Elctron nutrinos ar copiously producd in th intriors of stars. In stars lik th sun thy ar mainly producd in th pp cycl which dominats th fusion procss in cool stars pp d pp d 7 7 B Li 8 7 * B B This procss gnrats a crtain lctron nutrino flux E which would b xpctd to b dtctd at th Earth. Th Supr- Kamiokand data [1,2] show that only about 45% of th prdictd flux for 8 B lctron nutrinos is actually dtctd. Othr xprimnts with atmosphric lctron nutrinos hav also rportd lctron nutrino fluxs with dficits compard to th prdictd fluxs by th standard solar modl [3-8]. Thr ar also rports of lctron nutrino dficits from ractors [9,10]. Th nutrino oscillation proposal xplains th abov problm by supposing that th lctron

2 nutrinos ar changd into th othr nutrino flavors, muon and tau nutrinos, spcially to tau nutrinos, through th Mikhyv Smirnov Wolfnstin mchanism [11-13]. 2. A Gnral Critiqu for th nutrino Oscillation Proposal Th nutrino oscillation proposal has many flaws. I prsnt blow only 3 vry rlvant ons. 2.1 Lack of dtction of tau nutrino fluxs Th nhancmnt in tau nutrino fluxs du to nutrino oscillations has not bn masurd. Actually only th DONUT collaboration [14,15] from Frmilab dtctd tau nutrinos from th annihilation of pairs and th OPERA collaboration [16] found on tau nutrino in its qust for nutrino oscillations. Th lack of fluxs invalidats th claim for th nutrino oscillations and. 2.2 Lpton Numbr Violation Dcays According to th nutrino oscillation proposal th thr nutrino flavors would b rsonant stats of th sam particl. If this wr tru w would obsrv, for xampl, th wak dcays n p n p but ths dcays hav not bn obsrvd at all.

3 2.3 Why th strang prfrnc for th tau nutrino? If th disapparanc of lctron solar nutrinos wr causd by oscillations w would dtct a vry high flux of muon nutrinos, but what has bn rportd is xactly th opposit, that is, thr is also a muon nutrino dficit [17]. Why would both nutrinos prfr to chang to and which, according to th nutrino oscillation proposal, would b th most massiv nutrino? Why not th opposit, that is, th oscillation of and to? In such a cas w obsrv highr fluxs of. 3. Rport of a Nw fundamntal Intraction On th othr hand thr hav bn thortical proposals for a fifth forc of natur [18] and a rcnt rport on th obsrvation of a nw fundamntal intraction of mattr [19,20] mdiatd by a light boson. Th data of rfrnc 19 was carfully analyzd in dtail by Fng t al. [20]. Thy rinforc th ida of a nw fundamntal forc of natur mdiatd by mans of a light vctor boson with a mass of about 17 MV which, although producd through hadronic couplings, only dcays to, and. Thrfor, it is xpctd that nutrinos should intract with mattr by mans of this intraction. It is also xpctd that thr should b an intrplay btwn this nw intraction and th wak intraction bcaus both intractions involv lptons. It is important at this point to commnt on th Daya Bay rsults. This collaboration had rportd in 2012 [10] a disapparanc of about 6% in th lctron antinutrino flux along a distanc of 1648 m with rspct to th producd flux according to th currnt modls of nuclar thory, but in a papr that has just bn publishd [21] th collaboration corrcts th prvious rsults bcaus thy hav now found that th actual production is 6% largr than that on xpctd from th thortical nuclar modls, and thus, this invalidats thir prvious disapparanc claims. 4. Tntativ Solution to th Solar Nutrino Puzzl Although w do not know much yt on this nw intraction abov discussd, which will b th subjct of many xprimnts throughout th world in th nar futur, w can propos that th lctron

4 nutrinos intract with mattr in th Sun s cor and that this is th rason for th disapparanc of part of thir flux producd in th pp and CNO cycls, and thir disapparanc in xprimnts with nutrino fluxs on Earth. Bcaus of th intrplay abov mntiond btwn th nw intraction and th wak intraction, w should also xpct disapparanc of a crtain nutrino flavor du to th intractions in th mdium and apparanc of anothr flavor du to intraction in th sam mdium, as has bn obsrvd by T2K [22] and OPERA collaborations [16]. It is important to mphasiz this important conclusion by OPERA: W thrfor claim th obsrvation of a first candidat CC intraction. Its significanc, basd on our bst consrvativ knowldg of th background, xcds two. This dos not allow yt claiming th obsrvation of _oscillation. Givn its snsitivity, th OPERA xprimnt will rquir th dtction of a fw mor candidat vnts in ordr to firmly stablish nutrino oscillations in dirct apparanc mod through th idntification of th final chargd lpton. W mak us blow of th concpt of particl transparncy in a mdium and us it for th lctron nutrinos in th Sun s cor. Extnding th concpt of transparncy dvlopd by Shapiro and Tukolsky [23] in thir analysis of nutrino transparncy in stars with 9 cor tmpraturs smallr than 10 K, w can say that th ffctiv man fr path of a nutrino in th Sun s cor is givn by in which n and 1/3 ff n ar th nutrino man fr paths du to lastic scattring off nutrons and th wak inlastic scattring, rspctivly, and intraction. is th nutrino man fr path du to th nw Lt us try to find an stimat for th nw intraction cross sction by making th following considrations. In ordr to diminish th lctron nutrino flux to half in th Sun s cor w should hav 8 R ln R ln m whr R c is th cor radius ff c of th Sun and R is th Sun s radius, assuming that th nutrino flux diminishs xponntially along th travlld distanc. product n is givn by th following rlation [23] 7/6 5 1/2 5 nucl 10 n 2 10 km E 5/2 Th

5 whr E is th nutrino nrgy in lctron-volt, 14 nucl g/cm 3 is th nuclar dnsity and 100g/cm 3 is th Sun s cor dnsity. For 8 B nutrinos th nrgy spctrum [24] gos from zro up to 14 MV, and th nutrino flux paks around 7 MV [25]. Thus, making E 7 MV w obtain 1/ m w hav thn ff n fr path 36 n m 2, and from th rlation m. Th man is rlatd to th inlastic cross sction du to th nw intraction by th quation 1 n N whr n N is th numbr of nuclons pr unit volum. For th Sun s cor th dnsity of 100 g/cm 3 hnc, w obtain cm 2. mans nuclons/cm 3 and, As 1 ( n ) and 1 ( n ) dpnd on th lctron and nutron n n n dnsitis, w should tak th abov calculation with caution bcaus th lctron and nutron dnsitis dpnd strongly on th distanc from th cor cntr [26], and thus, is an avrag numbr. A vry important fact raisd by Lops and Turck-Chièz [26] is that diffrnt lctron nutrinos ar gnratd in diffrnt shlls in th Sun s cor, and thus, w cannot compar th diffrnt valus for and from th nutrino data of diffrnt collaborations whn thy rfr to diffrnt nutrinos, but bcaus of th conclusion blow w do not nd to mak such comparisons. Th problm with th abov calculation is that cm 2 is too larg to b tru. And as w saw abov, although th nw intraction is producd through hadronic couplings, its boson only dcays to, and. This mans that not only th nutrino, but also th lctron would intract strongly by mans of this nw intraction, but this has not bn sn for th lctron. All this mans that has to b much smallr than th abov numbr. Rinforcing this rasoning it is worth rcalling that th strong intraction btwn two protons has a cross sction of about 40 mbarn, and thus, would b about tims largr than th strong intraction cross sction. Thrfor, th solar nutrino problm may hav only th othr solution prsntd blow.

6 4. A Possibl Lin of Solution to th Solar Nutrino Puzzl In th light of th rcnt rsults of th Daya Bay Collaboration (21) and of th discovry of th nw intraction abov mntiond, w can propos that th actual production of lctron nutrinos in th Sun s cor is much largr than what has bn prdictd by th Standard Solar Modl, xactly bcaus of this nw intraction. For xampl, if th production of 8 B lctron nutrinos in th pp cycl wr 55% largr than what is prdictd by th Standard Solar Modl, th solar nutrino puzzl would b solvd. Thrfor, it is urgnt to invstigat furthr this nw intraction and find out th ordr of magnitud of its cross sction for th diffrnt lptons. And this nw intraction may also hav an important rol in th bginning of th Univrs. 5. Conclusion Taking into account th discovry of a nw fundamntal intraction of mattr which involvs nutrinos and th latst rsults of th Daya Bay Collaboration [21], I propos a compltly diffrnt solution to th solar nutrino dficits which is mor logical than th nutrino oscillation solution. My proposal is that mor nutrinos ar gnratd in th pp and CNO cycls in th Sun s cor in such proportions that thr ar cancllations with th claimd nutrino dficits. W should invstigat furthr th xistnc of this nw fundamntal intraction and th rol that it plays in th pp and CNO cycls in th Sun s cor for modifying th Solar Modl accordingly. Th abov simpl calculations provid a rational for th dfinitiv solution to th solar nutrino puzzl. REFERENCES 1. S. Fukuda t al. (Th Supr-Kamiokand Collaboration), Solar 8B and hp Nutrino Masurmnts from 1258 Days of Supr-Kamiokand Data, Phys. Rv. Ltt. 86, 5651, S. Fukuda t al. (Th Supr-Kamiokand Collaboration), Constraints on Nutrino Oscillations Using 1258 Days of Supr-Kamiokand Solar Nutrino Data, Phys. Rv. Ltt. 86, 5656 (2001).

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