Constraining supernova neutrino detection with weak decay available data

Transcription

1 Constraining suprnova nutrino dtction with wak dcay availabl data Arturo R. Samana in collaboration with Francisco Krmpotic, Aljandro Mariano, Csar Barbro UNLP -Argntina Carlos A. Brtulani -Txas A&M Univrsity Commrc-USA Nils Paar Univrsity of Zagrb Croatia 08/15/2016 INT-16-61W Sattl- USA

2 Outlin Motivation - On nutrino physics and nuclar structur. - Dtction of suprnova nutrinos Wak-Nuclar intraction formalism Nuclar Modls QRPA & RQRPA Som numrical rsults / 56F and 40Ar cross sction Summary

3 Motivation KARMEN ( ) LSND ( ) KARMEN, no oscillation signal LSND xprimnt obsrvs xcsss of vnts for both th and oscillation. ( J f ) n( E ) ( E, J f ) de A. Samana, F. Krmpotic, A. Mariano,R. Zukanovich Funchal/ Phys. Ltt B642(2006)100

4 (10-40 cm 2 ) Motivation -nuclus cross sction ar important to constrain paramtrs in nutrino oscillations. * Incras probability oscillations. * Confidnc lvl rgion is diminishd by diffrnc in btwn PQRPA and CRPA, PLB (2005) 100

5 Suprnova Nutrinos Signal Dtction Numbr of targt nucli N N v t 0 SNO d p p Nutrino flux F( E ) ( E ) ( E ) de Intraction cross sction p n Efficincy LVD ( E ) F ( E ) LVD Supr-K O O F N C C F F N B Co Mn BOREXino

6 Suprnova Nutrinos Signal Dtction LArTPC - Liquid Argon Tim Projction Chambrs: -40 Ar RPA: Martinz-Pindo, Kolb & Langank K, priv. comm. in Gil-Botlla & Rubbia, JCAP10 (2003) 009 SM : T. Suzuki & M. Honma, arxiv: v1 [nucl-th] 17 Nov 2012 QRPA : M. Choun tal, Phys. Rv. C 83, (2011) PQRPA: actual calculations 6

7 Wak nuclar intraction Chargd Currnt 12 C 12 N Nutral Currnt 12 C A( Z, N) A A( Z, N) A * * ( Z 1, N ( Z 1, N 1) 1) (i)o Connll, Donlly & Walcka, PR6,719 (1972) (ii) Kuramoto tal. NPA 512, 711 (1990) (iii) Luytn tal. NP41,236 (1963) (iv) Krmpotic tal. PRC71, (2005). 12 C * ALL ARE EQUIVALENTS. 7

8 1 1 ), ( ) (cos ) 1, ( 2 ), ( f l l l f l J k T d E Z F E p J E r k r k k k J J J i r ik f.. ),, (, Ø Nuclar Matrix Elmnt, Lpton tracs L b Transfr momntum, with k= k ž. i f l i f M M i s s M M i i W f f i f L J G M J H M J J J k b b ), ( 2 2 r ik W l J G r H 2 ) ( l A Z A Z l ) 1, ( ), ( Raction: Wak hamiltonian: Nutrino-nuclus cross sction (Frmi s Goldn Rul): p l :Lpton momntum, E l : Lpton nrgy, F(Z+1,E): Frmi function Transition amplitud Wak nuclar intraction

9 Wak nuclar intraction Non-rlativistic approximation of hadronic currnt Nuclar coupling constant g A ~1 FNS ffct: g g 2 2 k 2 2 =850 MV Transfr momntum, with k= k ž. Elmntary Oprators :

10 Wak nuclar intraction L ; L M L ;0 Lpton Tracs For natural parity stats with =(-) J,i.., 0 +, 1 -, 2 +, 3 -. For unnatural parity stats with =(-) J+1,i.., 0 -, 1 +,2 -, 3 +. (i) dforst Jr.& Walcka, Adv.Phys15, 1(1966) (ii) Kuramoto tal. NPA 512, 711 (1990) (iii) Luytn tal. NP41,236 (1963)(-captur) (iv) Krmpotic tal. PRC71, (2005). all ar quivalnts.

11 Nuclar Structur Modls (i) Modls with microscopical formalism with dtaild nuclar structur, solvs th microscopic quantum-mchanical Schrodingr or Dirac quation, provids nuclar wav functions and (g.s.-shap E sp, J, log (ft), t 1/2 ) Exampls: Shll Modl (Martinz t al. PRL83, 4502(1999)) RPA modls Slf-Consistnt Skyrm-HFB+QRPA (Engl tal. PRC60, (1999)) QRPA, Projctd QRPA (Krmpotic tal. PLB319(1993)393.) Rlativistic QRPA (N. Paar t al., Phys. Rv. C 69, (2004)) Dnsity Functional+Finit Frmi Syst. (Borzov tal. PRC62, (2000)) (ii) Modls dscribing ovrall nuclr proprtis statistically whr th paramtrs ar adjustd to xp. data, no nuclar wav funct., polynomial or algbraic xprss. Exampls: Frmi Gas Modl, Gross Thory of b-dcay (GTBD) Takahashi tal. PTP41,1470 (1969) Nw xponntial law for b... (Zhang tal. PRC73,014304(2006)) t 1/2 (Kar tal., astro-ph/ (2006)) 11

12 Nuclar Structur Modls QRPA: Quasiparticl Random Phas Approximation ( t )( u t 2 t v 2 t ) u v t t t 0, PQRPA: Projctd QRPA Particl numbr is consrvd xactly. Krmpotic tal. PLB319(1993)

13 Nuclar Structur Modls RQRPA: Rlativistic Quasiparticl Random Phas * Approximation 2 2 )( u v ) u v 0, ( t t t t t t t * N. Paar t al., Phys. Rv. C 69, (2004)

14 Wak Obsrvabl Constrains QRPA/PQRPA in 12 C Gamow -Tllr Strngths of Bta dcay O J=0+ =1, O J=1+ = Volp t al. PRC 62, (2000)``difficultis in choosing th g.s. of 12N bcaus th lowst stat is not th most collctiv on QRAP Quasiparticl RAndom Phas cod A. Samana, F. Krmpotic & C. Brtulani Comp. Phys. Comm. 181 (2010) p - 1h 2p - 2h 3p - 3h PH-channl paramtrs from a systmatic study GT rsonancs, F.K.&S.S. NPA 572, 329(1994) P (I) : v ph s = v pair, v ph t = v ph s /0.6 P(II): v ph s =27, v ph t =64 14

15 (10-42 cm 2 ) Wak Obsrvabl Constrains QRPA/PQRPA in 12 C 1p - 1h 2p - 2h 3p - 3h Projction Procdur is Important! Krmpotic tal. PRC71, (2005). CRPA, Kolb tal., PRC71, (2005). EPT, Mintz, PRC25,1671(1982). PQRPA, Krmpotic tal., PRC71, (2005). Exp, LSND coll., PRC55, 2078(1997). 15

16 Summary Nutrino/antinutrino cross sctions 12 C QRPA/PQRPA in 12 C 16

17 Summary Nutrino/antinutrino cross sctions 12 C QRPA/PQRPA in 12 C 17

18 Summary Nutrino/antinutrino cross sctions 12 C QRPA/PQRPA in 12 C (10-40 cm 2 ) -nuclus cross sction ar important to constrain paramtrs in nutrino oscillations. * Incras probability oscillations. * Confidnc lvl rgion is diminishd by diffrnc in btwn PQRPA and CRPA, A.Samana,t al.,plb (2005) 100

19 Summary Nutrino/antinutrino cross sctions 12 C QRPA/PQRPA/RQRPA in 12 C 19

20 Summary Nutrino/antinutrino cross sctions 56 F QRPA/PQRPA in 56 F 12 s.p. lvls: 2, 3 and 4 ħ, 3ħ, s.p. of 56 Ni, 2&4 s.p.. H.O. v pair s (p,n) to (p,n) xprimntal. v ph s =24, v ph t =64,(MV.fm 3 ) GT rsonanc in 48 Ca [NPA572,329(1994)].and t =0, B(GT-) =17.7 ~ B(GT-)=18.68 Skyrm [NPA716,230(2003)] ovrstimats xp [NPA410,371(1983)]. 2 ( E ) E KARMEN A.Samana & C.Brtulani, PRC78, (2008) 20

21 21 Summary Nutrino/antinutrino cross sctions 56 F QRPA/PQRPA Bta dcay strngths and Inclusiv muon captur rats 12 s.p. lvls: 2, 3 and 4 ħ, 3ħ, s.p. of 56 Ni, 2&4 s.p.. H.O.

22 Suprnova Nutrinos To stimat vnts in suprnova dtctors.. ) ( ) ( ), ( ) (, ) ( ) ( ), ( ) ( 0 0 ~ ~ 0 0 de E E T E F N T N N de E E T E F N T N N x x x t t Tim-intgratd nrgy Nutrino nrgy Distanc to suprnova Pinching paramtr, 1 (0) 4 ), 0,,, ( / T E E F D T L D L T E F Effctiv tmpratur Norm.factor D~ 10 kpc, L =E b. 1/6, E b =3x10 53 rg, {,, t } T( x )/T( )=1.5, T( )/T( )=0.8, T( )=5 MV 22 Summary Summary Nutrino/antinutrino cross sctions 56 F QRPA/PQRPA in 56 F

23 Summary * F Co Nutrino/antinutrino cross sctions 56 F A.S.& C.B., PRC 78, (2008) 23

24 Summary Nutrino/antinutrino cross sctions 56 F QRPA/PQRPA in 56 F PQRPA & QRPA, PRC 78, (2008) RQRPA DD-ME2, PRC 77, (2008) 24

25 Summary Nutrino/antinutrino cross sctions 40 Ar QRPA/PQRPA in 40 Ar Wak obsrvabls constrains - Gamow -Tllr Strngths of Bta dcay : low nrgy GT rsonancs & IAS - Inclusiv xclusiv muon captur rats: high nrgy MV muon mass PH-channl paramtrs from a systmatic study GT rsonancs, F.Krmpotic & S. Sharma NPA 572, 329 (1994) v ph s =27, v ph t =64 25

26 Summary Nutrino/antinutrino cross sctions 40 Ar QRPA/PQRPA 26

27 Summary Nutrino/antinutrino cross sctions 40 Ar PQRPA/RQRPA systmatic calculations Muon captur rats within th projctd QRPA Danilo Sand Santos, Arturo R. Samana, Francisco Krmpotic, Aljandro J. Dimarco WNP_120.pdf Ratios of thortical to xprimntal inclusiv muon captur rats for diffrnt nuclar modls, as function of th mass numbr A. Th prsnt QRPA and PQRPA rsults, as wll as th RQRPA calculation [13] wr don with ga = 1.135, whil in th RPA+BCS modl [11] was usd th unqunchd valu ga = 1.26 for all multipol oprators, xcpt for th GT ons whr it was rducd to ga 1. Rlativistic quasiparticl random-phas approximation calculation of total muon captur rats, T. Marktin, N. Paar, T. Nikˇsi c, and D. Vrtnar, PHYSICAL REVIEW C 79, (2009) Ratio of th calculatd and xprimntal total muon captur rats, as function of th proton numbr Z. Circls corrspond to rats calculatd with th fr-nuclon wak form factors Eqs. (10) (13) [21], and diamonds dnot valus obtaind by qunching th fr nuclon axial-vctor coupling constant ga =1.262 to ga = for all oprators, i.., in all multipol channls. 27

28 Nutrino/antinutrino cross sctions 40 Ar PQRPA - Inclusiv muon captur rats 28

29 Summary Nutrino/antinutrino cross sctions 40 Ar QRPA Choun t al. PRC83, (2011)/ PQRPA 29

30 Suprnova Nutrinos Signal Dtction SM + RPA (Suzuki & Honma) PRC87, (2013) ~1.4 PQRPA ~

31 Summary Nutrino/antinutrino cross sctions 40 Ar 31

32 Summary Nutrino/antinutrino cross sctions 40 Ar Foldd cross sction with SN fluxs 32

33 Summary All th formalism to dscrib wak-nuclar intraction prsnt in th litratur ar quivalnts! (i)o Connll, Donlly & Walcka, PR6,719 (1972) (ii) Kuramoto tal. NPA 512, 711 (1990), up to ( k /M) 3 (iii) Luytn tal. NP41,236 (1963), (iv) Krmpotic tal. PRC71, (2005) QRPA-typ Modls disadvantags: Low nrgy nutrino rgions up to 250 MV, Skyrm intraction not good nough to mak dcisiv improvmnt, Gogny intraction to chck Skyrm, sphrical nucli, fw QRPA modl to non-sphrical nucli advantags: slf-consistncy, larg spac, xcllnt agrmnt with xclusiv raction as wll as SM, wll dscription inclusiv raction and it s possibl dscrib up to 600 MV nutrino nrgy with RQRPA, good option for astrophysical systmatic calculations, main tool for 2 bta dcay in th last 30 yars improvmnts: through th Univrsal Nuclar Dnsity Functional UNEDF, non-sphrical nucli, Larg Scal Shll Modl disadvantags: only magic nucli (N=50, 82, 126); only GT-dcay; only sphrical, grat computational task, som cut du to a big configurational spac somtims this could b dangrous advantags: svral ssntial corrlations includd; tratmnt of vn and odd isotops. improvmnts: Ab-initio shll modl, nw advancs in nucli as 12C,16O and 48Ca 33

34 Summary Du th univrsality of th wak hamiltonian, th nuclar modls could b dscrib rasonably good th wak procsss: GT strngths for b+ and b- (low nrgy rgion up to 40 MV) and th inclusiv muon captur rats (up to 100 MV). A fin tunning rquirs agrmnts with xclusiv ractions, as such as xclusiv muon captur rats to first lowst stats. Scarc data availabl. Not for 40Ar. Thr is anothr possibility to obtain information about th allowd and forbiddn stats, ths ar th bta-bam xprimnts proposd by Lazauskus& Volp and Balantkin. Thr ar svral paramtrs in th nuclar modl, on of th most mor important is g A that gos from 1 to 1.27, laving an avragd rror up to 20 % in th GT-NME or CS. Som yars ago G. McLaughlin talk m about to mak a gross avragd of th CS for svral nuclar modls in 56F. I disagr in that momnt, nvrthlss I chang of ida du th difficult to obtain an rror in th nuclar modls. In LArTPC dtctors th most rlvant cross is CC 40Ar(,-)40K that has nvr bn masurd xprimntally, but is was proposd by F. Cavana in NUINT 12 to b prformd in NuSNS. P. Möllr thr is no corrct modl in nuclar physics. Any modling of nuclarstructur proprtis involvs approximations to obtain a formulation that can b solvd, but that rtains th ssntial faturs of th tru systm. Thanks! 34