Evidence of Solar Influences on Nuclear Decay Rates

Transcription

1 Evidence of Solar Influences on Nuclear Decay Rates John Buncher Tom Gruenwald Jordan Heim Dan Javorsek Dennis Krause Anthony Lasenby Andrew Longman Jere Jenkins Ephraim Fischbach Peter Sturrock Ed Merritt Josh Mattes Tasneem Mohsinally Dan Mundy John Newport Ben Revis

2 Publications to date Jenkins, J.H. and E. Fischbach, Perturbation of nuclear decay rates during the solar flare of 2006 December 13. Astroparticle Physics, (6): p [doi: /j.astropartphys ] Jenkins, J.H., et al., Evidence of Correlations Between Nuclear Decay Rates and Earth-Sun Distance. Astroparticle Physics, (1): p [doi: /j.astropartphys ] Fischbach, E., et al., Time-Dependent Nuclear Decay Parameters: New Evidence for New Forces? Space Science Reviews, (3): p [doi: /s ] Jenkins, J.H., D.W. Mundy, and E. Fischbach, Analysis of environmental influences in nuclear half-life measurements exhibiting time-dependent decay rates. Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, (2-3): p [doi: /j.nima ] Sturrock, P.A., et al., Power spectrum analysis of BNL decay rate data. Astroparticle Physics, (2): p [doi: /j.astropartphys ] Lindstrom, R. M., et al., Study of the dependence of 198Au half-life on source geometry, Nucl. Instr. and Meth. A, 622 (2010) 93. [doi: /j.nima ] Javorsek II, D., et al., Power spectrum analyses of nuclear decay rates. Astroparticle Physics, (3): p [doi: /j.astropartphys ] Fischbach, E., et al., Evidence for Solar Influences on Nuclear Decay Rates. Proceedings of the Fifth Meeting on CPT and Lorentz Symmetry, editor V.A. Kostelecky, World Scientific, Singapore, In Press

3 Background

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6 116m In Decay y = x R 2 = Counts/10s ln(counts/10s) Time (s) Counts ln(counts) Linear (ln(counts))

7 116m In Decay Counts/10s y = e x R 2 = Time (s) T 56 min 12 Counts Expon. (Counts)

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9 Motivation

10 A New Test of Randomness

11 Decay Rate Fluctuations

12 Brookhaven National Laboratory Measurement of 32 Si Half-life David Alburger Garman Harbottle Eleanor Norton

13 D.E. Alburger, G. Harbottle, E.F. Norton, Earth and Planetary Science Letters 78 (1986) 168.

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15 D.E. Alburger, G. Harbottle, E.F. Norton, Earth and Planetary Science Letters 78 (1986) 168.

16 D.E. Alburger, G. Harbottle, E.F. Norton, Earth and Planetary Science Letters 78 (1986) 168.

17 D.E. Alburger, G. Harbottle, E.F. Norton, Earth and Planetary Science Letters 78 (1986) 168.

18 D.E. Alburger, G. Harbottle, E.F. Norton, Earth and Planetary Science Letters 78 (1986) 168.

19 Physikalisch-Technische Bundesanstalt (PTB) Europium Half-lives and Long Term Detector Stability Helmut Siegert Heinrich Schrader Ulrich Schoetzig

20 H. Siegert, H. Schrader, U. Schoetzig, Applied Radiation and Isotopes 49 (1998) 1397.

21 H. Siegert, H. Schrader, U. Schoetzig, Applied Radiation and Isotopes 49 (1998) 1397.

22 Purdue Experiments

23 T 1/2 =313.5d T 1/2 =1953d

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27 ( ) x 10 5 Events missing

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30 40 hours precursor

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32 5 Dec 2006: X-9 class flare

33 13 Dec 2006: X3/4B Flare

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36 16.3 Logarithmic Decay of 54 Mn for December ln(cr) /28 12/2 12/6 12/10 12/14 12/18 12/22 12/26 12/30 1/3 Date (2008) ln(gross) Linear (ln(gross))

37 16.28 Logarithmic Decay of 54 Mn for December ln(cr) /9 12/10 12/11 12/12 12/13 12/14 12/15 12/16 12/17 12/18 12/19 12/20 12/21 12/22 12/23 Date (2008) ln(gross) Linear (ln(gross))

38 SOLAR ACTIVITY: Hours ago, something on the far side of the sun exploded and hurled a massive cloud of debris (a CME) over the eastern limb. Using a coronagraph to block the sun's glare, the Solar and Heliospheric Observatory (SOHO) photographed the cloud expanding into space: NASA's Stereo-B spacecraft is stationed over the sun's eastern limb, but it was not taking pictures at the probable time of the eruption, so details of the blast are unknown. The CME could herald an active region (e.g., a sunspot or perhaps an unstable magnetic filament) turning to face Earth in the days ahead.

39 16.28 Logarithmic Decay of 54 Mn for December Non Earth-directed large CME recorded by SOHO at Dec 08 UT ln(cr) y = x R² = T 1/2 =307d y = x R² = T 1/2 =776d /9 12/10 12/11 12/12 12/13 12/14 12/15 12/16 12/17 12/18 12/19 12/20 12/21 12/22 12/23 Date (2008) ln(gross) 12/14-12/16 Linear (ln(gross)) Linear (12/14-12/16) Linear (12/14-12/16)

40 Solar Neutrinos? Super-K Data Correlation = 0.38, 181 points, prob=3x Normalized Nu-flux /R 2, a.u /28/95 3/11/97 7/24/98 12/6/99 4/19/01 9/1/02 Date 7 Pt Avgd Normalized Phi-nu 1/R^2 Data from Yoo, et al., Phys Rev D 68, (2003)

41 Eccentricity of Earth s Orbit

42 Back to BNL and PTB

43 Normalized BNL With Earth-Sun Distance BNL U(t) /81 02/82 09/82 03/83 10/83 04/84 11/84 06/85 12/85 07/86 1/R 2 (a.u. -2 ) 0.98 Representative 1σ Error for BNL Data Date Normalized Un-decayed BNL Uncertainty USNO 1/R^2 Pearson Correlation Coefficient r=0.52, N=239, Prob=4.17x10-18 Data from: Alburger, et al., Earth and Planet. Sci. Lett., 78, (1986)

44 7 Pt Avg'd Normalized BNL With Earth-Sun Distance Normalized BNL /81 02/82 09/82 03/83 10/83 04/84 11/84 06/85 12/85 07/86 1/R^2 (a.u.^2) Date Un-decayed 7pt avg USNO 1/R^2 Pearson Correlation Coefficient r=0.66, N=233, Prob=1.0x10-31 Data from: Alburger, et al., Earth and Planet. Sci. Lett., 78, (1986)

45 Raw Undecayed 226Ra PTB Data with Earth-Sun Distance Normalized 226 Ra Data /R 2 (a.u. -2 ) /23/83 3/22/84 3/22/85 3/22/86 3/22/87 3/21/88 3/21/89 3/21/90 3/21/91 3/20/92 3/20/93 3/20/94 3/20/95 3/19/96 3/19/97 3/19/98 3/19/99 3/18/ Date Normalized Undecayed USNO 1/R^2 Pearson Correlation Coefficient r=0.62, N=1974, Prob=5.13x Data from Siegert, et al., Appl. Radiat. Isot. 49, 1397 (1998) Fig. 1

46 7 Pt Avg Undecayed 226Ra PTB Data with Earth-Sun Distance /23/83 3/22/84 3/22/85 3/22/86 3/22/87 3/21/88 3/21/89 3/21/90 3/21/91 3/20/92 3/20/93 3/20/94 3/20/95 3/19/96 3/19/97 3/19/98 3/19/99 Normalized 226 Ra Data 3/18/ /R 2 (a.u. -2 ) 0.92 Date 7 pt avg normalized undecayed USNO 1/R^2 Pearson Correlation Coefficient r=0.65, N=1968, Prob=3.12x Data from Siegert, et al., Appl. Radiat. Isot. 49, 1397 (1998) Fig. 1

47 BNL/PTB Correlation

48 BNL 32Si and PTB 226Ra Data with Earth-Sun Distance BNL and PTB U(t) /R 2 (a.u. -2 ) Date Raw BNL Raw PTB USNO 1/R^2 Pearson Correlation Coefficient r=0.66, N=39, Prob=5.8x10-6

49 BNL 32Si and PTB 226Ra Data with Earth-Sun Distance BNL and PTB U(t) /R 2 (a.u. -2 ) Date 5 Pt Avg BNL 5 Pt Avg PTB USNO 1/R^2 Pearson Correlation Coefficient r=0.87, N=35, Prob=3.78x10-12

50 Data from other institutions

51 Data from other institutions ELLIS: CNRC

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53 1.006 CNRC 238 Pu/ 56 Mn Data with 1/R Normalized Decay Data /R 2 (a.u.-2 ) Date Data from K. Ellis, Phys. Med. Biol., 35, (1990) 0.96

54 Data from other institutions OSURR

55 Ohio State (Preliminary 36 Cl) Normalized Cl-36 Counts Heliolatitude and 1/R /31/2003 6/30/ /30/2004 6/30/ /30/2005 7/1/ /30/2006 7/1/ /31/2007 6/30/ /30/2008 6/30/ /30/2009 Date Normalized Cl-36 Counts Fxn F (Heliolatitude and 1/R2)

56 OSU Power Spectrum

57 Data from other institutions PARKHOMOV

58 Parkhomov, A.G., Researches of alpha and beta radioactivity at long-term observations, arxiv: v1 [physics.gen-ph], (2010)

59 Data from other institutions SIEGERT, PTB (EUROPIUM)

60 H. Siegert, et al., Appl. Rad. & Isot., 49 (1998)

61 Data Summary Experiment Detector Type Decay Type Measured Radiation Type Observed Variations PTB ( 226 Ra) Ion Chamber Gas α, β, γ γ Annual PTB ( 152 Eu) GeLi Solid State ε, γ γ Annual BNL ( 32 Si/ 36 Cl) Prop. Counter Gas β - β - Annual Purdue ( 54 Mn) NaI(Tl) Scintillator ε, γ γ Flare CNRC ( 56 Mn) NaI(Tl) Scintillator β -, γ γ Annual OSU ( 36 Cl) G-M Gas β - β - Annual Parkhomov ( 90 Sr/ 90 Y-I) G-M Gas β - β - Annual Parkhomov ( 90 Sr/ 90 Y-II) G-M Gas β - β - Annual Parkhomov ( 60 Co) G-M Gas β -, γ β -, γ Weak Annual Parkhomov ( 239 Pu) Si Solid State α α None

62 Possible Mechanisms

63 Possible Mechanisms and New Long Range Forces The Sun can influence nuclear decays either through new long-range fields or through particles such as neutrinos, axions, or other non-standard objects If the effect arises from a new long-range field, then any such field must have a range of ~1 a.u. Such spinindependent fields are highly constrained. If the sun influences nuclear decays through emission of particles, then these can influence nuclear decays through relatively short-range fields which tend to be less highly constrained. Spin-dependent long-range forces are relatively poorly constrained, and may provide an appropriate mechanism to explain time-varying decay rates.

64 Possible Mechanisms-I Spatial Variation of the Fine Structure Constant α This is an example of a mechanism whose existence depends on a field whose range is ~1 a.u. Such a field is strongly constrained by both 5 th force type experiments, and atomic physics experiments.

65 Spatial Variation of the Fine Structure Constant alpha For alpha decay (e.g., 226 Ra arrow 222 Rn + 4 He) δα δγ 1 v 3 δγ α Γ 4πZα c Γ From our 226 Ra data, δγ δα Γ α 3 5 This may be incompatible with existing WEP and 5th force constraints. References: D. J. Shaw, gr-qc/ ; J.D. Barrow and D. J. Shaw, arxiv:0806:4317; J.-P. Uzan, Rev. Mod. Phys. 75, 403 (2003)

66 Possible Mechanisms-II Spin-dependent long range force coupling to neutrinos This is an example of where a spindependent force of relatively short range could provide an explanation of the decay data.

67 Spin-dependent long range force coupling to neutrinos Δ

68 Variation in Solar Neutrino Flux For beta-decay, e 0 de where Gamma is extremely sensitive to small shifts in E 0 2. Assume E 0 arrow E 0 +Delat, where Delta arises from solar neutrinos, then 3. Next, assume where dγ E E m ( E E) ( E E) ( E E) + 2 ( E E) A = [3( σ ˆ ˆ 3 1 r)( σ2 r) σ1 σ2 r 1 = ν e, 2 = p,e,n,ν e 4. For an un-polarized sample, (E 0 E) 2 (E 0 E) 2 + 2

69 Variation in Solar Neutrino Flux (cont d) 5. Compare this to the change induced by m ν 2 0 (E 0 E) 2 (E 0 E) (E 0 E) 2 m v 2 1 For ( E0 E) m, m v v m = 100 ev to 10 ev v = 50 ev to 5 ev This may be compatible with current limits on neutrino magnetic dipole moments.

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