Lower and upper bounds on CSL parameters from latent image formation and IGM heating

Journal of Physics A: Mathematical and Theoretical

Volumn 40, Issue 12, 2007, Pages 2935-2957

  Adler, Stephen L ^a  

^a INSTITUTE FOR ADVANCED STUDY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 49749085667     PISSN: 17518113     EISSN: 17518121     Source Type: Journal    
DOI: 10.1088/1751-8113/40/12/S03     Document Type: Article

References (70)

1. For reviews and references, see BassiAand GhirardiGC 2003 Dynamical reductionmodels Phys. Rep. 379 257
2. Pearle P 1999 Collapse models Open Systems and Measurements in Relativistic Quantum Field Theory (Lecture Notes in Physics vol 526) ed H-P Breuer and F Petruccione (Berlin: Springer)
3. See also reference [6] of Bassi A, Ippoliti I and Adler S L 2005 Phys. Rev. Lett. 94 030401
4. Adler S L 2004 Quantum Theory as an Emergent Phenomenon (Cambridge: Cambridge University Press) chapter 6
5. Alternative choices of the correlation function are discussed in Weber T 1990 Nuovo Cimento B 106 1111
6. Bassi A, Ippoliti I and Adler S L 2005 Phys. Rev. Lett. 94 030401
7. Adler S L, Bassi A and Ippoliti I 2005 J. Phys. A: Math. Gen. 38 2715
8. Adler S L 2005 J. Phys. A: Math. Gen. 38 2729
9. For a review of tests of quantum mechanics from a viewpoint not specifically focused on dynamical reduction models, see Leggett A J 2002 J. Phys.: Condens. Matter 14 R415
10. Gisin N and Percival I C 1993 J. Phys. A: Math. Gen. 26 2245
11. Collett B and Pearle P 2003 Found. Phys. 33 1495
12. See also Collett B, Pearle P, Avignone F and Nussinov S 1995 Found. Phys. 25 1399
13. Pearle P, Ring J, Collar J and Avignone F 1999 Found. Phys. 29 465
14. Pearle P 2005 Phys. Rev. A 71 032101
15. Pearle P and Squires E 1994 Phys. Rev. Lett. 73 1 (The parameter 1/T of Pearle and Squires, when their m0 is taken as the nucleon mass, corresponds to the parameter λ used here. With this identification, their equation (10) gives equation (7) above)
16. Adler S L 2005 J. Phys. A: Math. Gen. 38 2729 (This paper gives the energy loss rate in terms of a parameter η, that for a nucleon is given by η = γ/(16π3/2r5C) = λ/ (2r2c ). Equation (12) ofAdler [6] and the corresponding equation (6.58) of Bassi and Ghirardi [1] both give the energy loss rate in one dimension, and so must be multiplied by 3 to give equation (7) above)
17. -5 s for the ionic stage of latent image formation)
18. Avan L, AvanM, Blanc D and Teyssier J-L 1973 Ionographie: Émulsions-Détecteurs Solides de Traces (Paris: Doin Editeurs) (Figure II.1 on p 75 gives a descriptive rendition of the Gurney-Mott process, and grain spacing estimates of 1.6-5 μm are given on p 102. Table VIII.1 on p 268 gives estimates of etchable track diameters, and table VIII.3 on p 278 gives times t for various stages of the track formation process)
19. Berg W F 1946-7 Rep. Prog. Phys. 11 248 (Size of grains is given on p 249, along with a spacing estimate of 1 μm; an estimate of 30 silver atoms to produce a latent image speck is given on p 272; an ionic step time of 4 × 10-5 s is given on p 290)
20. Hamilton J F and Urbach F 1966 The mechanism of the formation of the latent image The Theory of the Photographic Process 3rd edn, ed C E K Mees and T H James (New York/London: Macmillan/Collier- Macmillan) (An estimate of 3-6 silver atoms for 50% development probability is given on p 102; figure 5.4, showing the extent of halogen diffusion into the gelatine, is on p 94)
21. Gurney R W and Mott N F 1938 Proc. R. Soc. 164 151
22. Durrani S A and Bull R K 1987 Solid State Nuclear Track Detection (Oxford: Pergamon) (See pp 34, 37 and 38 for a discussion of latent track geometry, and p 44 for the minimum time for a track to form)
23. Katz R and Kobetich E J 1968 Phys. Rev. 170 401 (Information on the δ-ray energies is given on p 403)
24. Arndt M, Nairz O, Vos-Andreae J, Keller C, van der Zouw G and Zeilinger A 1999 Nature 401 680
25. Nairz O, Arndt M and Zeilinger A 2000 J. Mod. Opt. 47 2811
26. Nairz O, Brezger B, Arndt M and Zeilinger A 2001 Phys. Rev. Lett. 87 160401
27. Buffa M, Nicrosini O and Rimini A 1995 Found. Phys. Lett. 8 105
28. Rimini A 1995 Spontaneous localization and superconductivity Advances in Quantum Phenomena ed E Beltrametti and J-M Lévy-Leblond (New York: Plenum)
29. Rae A I M 1990 J. Phys. A: Math Gen. 23 L57
30. Tinkham M 1996 Introduction to Superconductivity 2nd edn (New York: McGraw-Hill) p 2 For original papers
31. Quinn D J and Ittner W B 1962 J. Appl. Phys. 33 748
32. Broom R F 1961 Nature 190 992
33. Collins S C as quoted in Crowe J W 1957 IBM J. Res. Dev. 1 294 (The best direct measurement of the time constant for supercurrent decay gives ∼250 years; the estimate 105 years is obtained by scaling this result up using the results of resistivity measurements on thin film superconductors, taken over periods of 3-7 h)
34. Fu Q 1997 Phys. Rev. A 56 1806
35. Samui S, Subramanian K and Srianand R 2005 Preprint astro-ph/0505590 (opening paragraph, compilation of data, and references cited)
36. Hui L and Haiman Z 2003 Astrophys. J. 596 9
37. Theuns T et al 2002 Mon. Not. R. Astron. Soc. 332 367
38. Ricotti M, Gnedin N and Shull J 2000 Astrophys. J. 534 41 (table 7)
39. Hui L and Gnedin N 1997 Mon. Not. R. Astron. Soc. 292 27
40. Spitzer L 1978 Physical Processes in the Interstellar Medium (New York: Wiley) chapter 6 p 143
41. Dalgarno A and Mc Cray R 1972 Ann. Rev. Astron. Astrophys. 10 375, 383 Note that the recombination cooling rate curves graphed in the last two references apply only when the degree of ionization is low; when the IGM is highly ionized, recombination cooling is several orders of magnitude smaller than that suggested by these curves, and is in fact small relative to adiabatic cooling. I wish to thank Nick Gnedin for a conversation which clarified this point.
42. Kaplan S A and Pikelner S B 1970 The Interstellar Medium (Cambridge, MA: Harvard University Press) pp 211-2
43. de Pater I and Lissauer J J 2001 Planetary Sciences (Cambridge: Cambridge University Press) pp 224-5
44. Bassi A, Ippoliti E and Vacchini B 2005 J. Phys. A: Math. Gen. 38 8017
45. Halliwell J and Zoupas A 1995 Phys. Rev. D 52 7294
46. Gallis M R and Fleming G N Phys. Rev. A 43 5778
47. Benatti F, Ghirardi G C, Rimini A and Weber T 1988 Nuovo Cimento B 101 333
48. Joos E and Zeh H D 1985 Z. Phys. B 59 223 (see equations (3.58), (3.59), and table 2)
49. Corrections to the analysis of Joos and Zeh are given in Gallis M R and Fleming G N 1990 Phys. Rev. A 42 38
50. Dodd P J and Halliwell J J 2003 Phys. Rev. D 67 105018
51. Hornberger K and Sipe J E 2003 Phys. Rev. A 68 012105
52. Davson H 1980 Physiology of the Eye 4th edn (New York: Academic) p 167
53. Marshall W, Simon C, Penrose R and Bouwmeester D 2003 Phys. Rev. Lett. 91 130401
54. Bernád J Z, Diósi L and Geszti T 2006 Preprint quant-ph/0604157
55. LaHaye M D, Buu O, Camarota B and Schwab K C 2004 Science 304 74
56. Abramovici A et al 1992 Science 256 325
57. Barish B C and Weiss R 1999 Phys. Today 52 44
58. Shawhan P S Am. Sci. 92 350
59. Alberto J 2004 LISA Preprint gr-qc/0404079
60. Irion R 2002 Science 297 1113
61. Adler S L 2006 Preprint quant-ph/0607109
62. Ghirardi G C, Rimini A and Weber T 1986 Phys. Rev. D 34 470
63. Braginsky V B and Khalili F Ya 1992 Quantum Measurements (Cambridge: Cambridge University Press)
64. Caves C M, Thorne K S, Drever R W, Sandberg V D and Zimmerman M 1980 Rev. Mod. Phys. 52 341 (I have used the definition of standard quantum limit given in equation (3.2) of the Caves et al article; the definition of Braginsky and Khalili is a factor of v2 smaller)
65. Albert D Z and Vaidman L 1989 Phys. Lett. A 139 1
66. Aicardi F, Borsellino A, Ghirardi G C and Grassi R 1991 Found. Phys. Lett. 4 109
67. Thaheld F 2005 Preprint quant-ph/0509042
68. Thaheld F 2006 Preprint quant-ph/0604181
69. Rieke F and Baylor D 1998 Rev. Mod. Phys. 70 1027
70. Kittel C 1996 Introduction to Solid State Physics 7th edn (New York: Wiley) appendix J, pp 662-5