As seen in the previous chapter, a measurement apparatus for time of flight is proposed, since the xy hit distributions of the (p, γ) fusion products, of both astrophysical reactions, have considerable overlap with the hit distributions of elatically scattered 33,34mCl beams, in order to obtain particle identification.
Also measurements form DRAGON [39] have shown that the energy resolution of a single silicon detector is not feasible for separating the fusion events from the elastic scattered background on the basis of a total energy measurement of each. Therefore, a coincidence measurement system has to be used.
A double-sided silicon strip detector (DSSD) could be used for a total energy measurement of the incident particle and a tof "stop" signal; while a multichannel plate (MCP) detector placed upstream of the DSSD would provide a tof "start" signal. The "start" signal is provided by electrons, that are produced by the ion beam hitting a thin carbon foil. The electrons are then bended away to the MCP, where they can be measured.
The DSSD and also the MCP would have to withstand the elastically scattered beam. Rates higher than 105 per second would destroy the detector. The elastic rates of scattered beam, as shown in Section 4.3, can be adjusted with the target density at least by factor of 10. Therefore it is permitted to use a DSSD and a MCP. With this adjustment all resonance energies of 33Cl(p, γ)34Ar and34Cl(p, γ)35Arcan be measured.
The total energy measurement combined with this local tof measurement would then allow mass identification of the ion species entering the DSSD detector. The timing resolution for both detector types are at least∼1 ns[40,41] which, from Figure4.5, should be sufficient to obtain clean separation between the elastically scattered beam and fusion events.
41
42 CHAPTER 5. CONCLUSION
Technische Universität München 42 Physics Department
Appendix A
Reference Index
43
44 APPENDIX A. REFERENCE INDEX
Technische Universität München 44 Physics Department
Bibliography
[1] S.˜W. Stahler and F Palla.The Formation of Stars, Wiley-VCH , January 2005. Wiley-VCH, 2005, p. 852.
[2] A. Bressan et al. ‘Evolutionary sequences of stellar models with new radiative opacities. II -Z = 0.02’. In: Astronomy and Astrophysics Supplement Series 100 (1993), pp. 647–664. doi: 10.1051/aas:1996144.
[3] Gregory Laughlin, Peter Bodenheimer and Fred C. Adams. ‘The End of the Main Sequence’. In:
The Astrophysical Journal 482.1 (June 1997), pp. 420–432.doi:10.1086/304125.
[4] H. L. Shipman. ‘Masses and radii of white-dwarf stars. III - Results for 110 hydrogen-rich and 28 helium-rich stars’. In:The Astrophysical Journal 228 (1979), p. 240.doi:10.1086/156841.
[5] S.˜O. Kepler et al. ‘The White Dwarf Mass Distribution’. In:15th European Workshop on White Dwarfs. Vol. 372. 2007, p. 35. arXiv:0612277v2 [arXiv:astro-ph].
[6] Charles J Lada. ‘Stellar Multiplicity and the Initial Mass Function: Most Stars Are Single’. In:
The Astrophysical Journal 640.February (2006), pp. L63–L66. doi: 10 . 1086 / 503158. arXiv:
0601375 [astro-ph].
[7] Jordi José, Margarita Hernanz and Christian Iliadis. ‘Nucleosynthesis in classical novae’. In:
Nuclear Physics A 777.777 (2006), pp. 550–578. doi: 10.1016/j.nuclphysa.2005.02.121.
arXiv:0101343 [astro-ph].
[8] Margarita Karovska et al. ‘A Large X-Ray Outburst in Mira A’. In:The Astrophysical Journal 623.2 (2005), pp. L137–L140.doi:10.1086/430111. arXiv:0503050 [astro-ph].
[9] Chandra :: Educational Materials :: Stellar Evolution :: Stellar Evolution - Cycles of Formation and Destruction, http://chandra.harvard.edu/edu/formal/stellar_ev/story/index3.html.
[10] Jordi Jose and Margarita Hernanz. ‘Nucleosynthesis in Classical Novae: CO versus ONe White Dwarfs’. In:The Astrophysical Journal 494.2 (1998), pp. 680–690.doi:10.1086/305244.
[11] Sumner Starrfield et al. ‘CNO Abundances and Hydrodynamic Models of the Nova Outburst’.
In:Astrophysical Journal 176 (1972), p. 169.doi:10.1086/151619.
[12] Jordi José, Alain Coc and Margarita Hernanz. ‘Synthesis of intermediate-mass elements in classical novae: From Si to Ca’. In: Astrophys. J. 560 (2001), pp. 897–906. arXiv: 0106418v1 [arXiv:astro-ph].
[13] Jennifer Harbaugh."Mini Supernova" Explosion Could Have Big Impact. Tech. rep. 2015.
[14] S Starrfield, C Iliadis and W R Hix. ‘The Thermonuclear Runaway and the Classical Nova Outburst’. In:Publications of the Astronomical Society of the Pacific128.963 (2016), p. 051001.
doi:10.1088/1538-3873/128/963/051001. arXiv:1605.04294.
[15] Warren M. Sparks. ‘A New Method of Determining the Ejected Mass of Novae’. In: Springer, Dordrecht, 1995, pp. 211–216.doi:10.1007/978-94-011-0335-0_77.
[16] Ernst Zinner. ‘Stellar Nucleosynthesis and the Isotopic Composition of Presolar Grains From Primitive Meteorites’. In:Annual Review of Earth and Planetary Sciences 26.1 (1998), pp. 147–
188.doi:10.1146/annurev.earth.26.1.147.
[17] Sachiko Amari et al. ‘Presolar Grains from Novae’. In:The Astrophysical Journal 551.2 (2001), pp. 1065–1072.doi:10.1086/320235.
45
46 BIBLIOGRAPHY [18] Jordi José and Margarita Hernanz. ‘The origin of presolar nova grains’. In:Meteoritics & Plan-etary Science 42.7-8 (Aug. 2007), pp. 1135–1143.doi:10.1111/j.1945-5100.2007.tb00565.x.
[19] M. Lestinsky et al. ‘Physics book: CRYRING@ESR’. In: European Physical Journal: Special Topics 225.5 (2016), pp. 797–882.doi:10.1140/epjst/e2016-02643-6.
[20] Jordi Jose et al. ‘The imprint of nova nucleosynthesis in presolar grains’. In: The Astrophysical Journal 612 (2004), pp. 414–428.doi:10.1086/422569. arXiv:0405332v1 [arXiv:astro-ph].
[21] Alain Coc, Marie-Geneviève Porquet and Frédéric Nowacki. ‘Lifetimes of 26 Al and 34 Cl in an astrophysical plasma’. In: Physical Review C 61.1 (1999), p. 015801. doi:10.1103/PhysRevC.
61.015801. arXiv:9910186 [astro-ph].
[22] Mark D. Leising and Donald D. Clayton. ‘Positron Annihilation Gamma Rays from Novae’. In:
The Astrophysical Journal 323 (1987), pp. 159–169.doi:10.1086/165816.
[23] P.M. M. Endt. ‘Energy levels of A = 21-44 nuclei (VII)’. In: Nuclear Physics, Section A633.A (1990), pp. 1–830.doi:10.1016/0375-9474(90)90598-G.
[24] P.˜M. M Endt. ‘Supplement to Energy Levels of A=21-44 Nuclei (VII)’. In: Nuclear Physics A 633.1 (Apr. 1998), pp. 1–220. doi:DOI:10.1016/S0375-9474(97)00613-1.
[25] C A Bertulani. ‘Tunneling of Atoms, Nuclei and Molecules’. In: Few-Body Systems 56.11-12 (2015), pp. 727–736.doi:10.1007/s00601-015-0990-z. arXiv:1502.0074.
[26] Donald D. Clayton. Principles of stellar evolution and nucleosynthesis : with a new preface.
University of Chicago Press, 1983, p. 612.
[27] Christian Iliadis. Nuclear Physics of Stars. 2008, pp. 1–666.doi:10.1002/9783527618750.
[28] Helmut Wiedemann.Particle accelerator physics: Third edition. Springer, 2007, pp. 1–948.doi: 10.1007/978-3-540-49045-6.
[29] James B Rosenzweig and Edmund Wilson. Fundamentals of beam physics. 2002.
[30] Maschen.Direction cosine - Wikipedia. 2013.
[31] Yu.A. Litvinov et al. ‘Nuclear physics experiments with ion storage rings’. In: Nuclear Instru-ments and Methods in Physics Research Section B: Beam Interactions with Materials and Atoms 317 (2013), pp. 603–616. doi:10.1016/j.nimb.2013.07.025. arXiv:1312.7476.
[32] Bo Mei et al. ‘First measurement of the 96Ru(p,γ)97Rh cross section for the p process with a storage ring’. In:Physical Review C 92.3 (2015), p. 035803.doi:10.1103/PhysRevC.92.035803.
arXiv:1507.04916.
[33] N Iwasa et al. ‘MOCADI, a universal Monte Carlo code for the transport of heavy ions through matter within ion-optical systems’. In:Nuclear Instrum. Methods B 126.1-4 (1997), pp. 284–289.
doi:10.1016/S0168-583X(97)01097-5.
[34] N Iwasa, H Weick and H Geissel. ‘New features of the Monte-Carlo code MOCADI’. In:Nuclear Instruments and Methods in Physics Research, Section B: Beam Interactions with Materials and Atoms 269.8 (2011), pp. 752–758.doi: 10.1016/j.nimb.2011.02.007.
[35] M. Wang et al. ‘The AME2012 atomic mass evaluation(I)’. In: AIP Conference Proceedings.
Vol. 1484. 2012, pp. 79–84.doi:10.1063/1.4763377. arXiv:1011.1669v3.
[36] James Ziegler. SRIM & TRIM 2013. 2013.
[37] M Kü Hnel et al. ‘Low-Z internal target from a cryogenically cooled liquid microjet source’. In:
(2009).doi: 10.1016/j.nima.2008.12.212.
[38] N. Petridis et al. Technical Report: Design of the Target@HESR. Tech. rep. 2009.
[39] J. M. D’Auria et al. ‘The 21Na(p, ??)22Mg reaction from E c.m.=200 to 1103 keV in novae and x-ray bursts’. In: Physical Review C - Nuclear Physics 69.6 (2004), pp. 065803–1. doi: 10.1103/PhysRevC.69.065803.
[40] K. M. Kosev. ‘A High-Resolution Time-of-Flight Spectrometer for Fission Fragments and Ion Beams’. In: August 1975 (2007), p. 112.
[41] M Friedl, C Irmler and M Pernicka. ‘Time Resolution of a Few Nanoseconds in Silicon Strip Detectors Using the APV25 Chip’. In: LECC2006 proceedings(2006), pp. 460–464.
Technische Universität München 46 Physics Department
List of Figures
1.1 Left image [8]: Chandra image shows Mira A (right), a highly evolved red giant star, and Mira B (left), a white dwarf; right image [9]: an artist illustration of the same stellar object . . . 2 1.2 GK Persei; image contains x-rays from Chandra X-Ray Telescope (blue), optical data
from NASA’s Hubble Space Telescope (yellow), and radio data from the National Sci-ence Foundation’s Very Large Array (pink). The x-ray data show hot gas and the radio data show emissions from electrons that have been accelerated to extremely high energies by the nova shock wave. The optical data reveal clumps of material that were ejected in the nuclear explosion [13] . . . 3 1.3 The S-Cl burning cycle. β-decays are depicted with blue arrows and proton capture
reactions (p, γ) are depicted with vertical red arrows. The cyclic nature is depicted by the thick outer red arrow for the (p, α) (proton capture with prompt α emission) reaction on 35Cl [19] . . . 4 1.4 Nuclear level scheme of 33Cl(p, γ)34Ar [23] and 34Cl(p, γ)35Ar [24] product nuclei in
the range of the Gamow window (in red) for nova (0.1 GK), (0.3 GK) and X-ray bursts (1.0 GK) [19] . . . 6 2.1 Exponential factors of equation 2.10 and resulting "Gamow window" (dashed) with a
temperature of 1 keVto3 keV, where the peak is15 keVto 20 keV[26] . . . 9 2.2 The Gamow peak for the 12C(α, γ)16O reaction at a temperature of0.2 GKshown on
a linear scale (solid line). The maximum occurs atE0= 0.32 MeVwhile the maximum of the Maxwell–Boltzmann distribution is located at kT = 0.017 MeV (arrow). The dotted line shows the Gaussian approximation of the Gamow window [27] . . . 10 2.3 Locally defined right-handed coordinate system used with bending design. Here s is
the distance along the design orbit, xis the distance from this orbit along the radius of curvature, andy is the distance from the design orbit out of the bend plane. [29]. . 13 2.4 Particle trajectories in deflecting systems. Reference path z and individual particle
trajectoryshave in general different bending radii [28] . . . 13 2.5 Illustrations of the vector vdirection cosine representation [30] . . . 16 3.1 A schematic view of the Facility for Antiproton and Ion Research in Darmstadt. The
present GSI facility consisting of the UNILAC, SIS, FRS and ESR is shown together with the location of the CRYRING which is presently being commissioned [31]. . . 17 3.2 Top view of the CRYRING model in the new CRYRING@ESR configuration. Labels
indicate the section numbering and the dominant functions of each straight section. [19] 18
47
48 LIST OF FIGURES 3.3 Sections YR09 and YR10 of the CRYRING: secondary ion beam (blue) coming from
the left, marked are the possible detector positions for a detector (red arrows): at the dipole (grey box on the left): -3- and the angled detector position covered with two simulated detectors -4-, -5-, after the first quadrupole: minimum -7-, middle -8- and maximum position -9-; after the first hexapole: -10-. . . 19 3.4 Hit patterns in xand y for differentθ and φin CMS after the reaction has occurred
at the second possible detector position inside the dipole section -5-: Red: θ = 20◦, φ = 130◦; Blue: θ = 20◦, φ = 180◦; Green: θ = 20◦, φ = 310◦; Violet: θ = 20◦, φ= 360◦; Brown: θ= 30◦,φ= 220◦; Orange: θ= 30◦,φ= 50◦ . . . 24 3.5 Positioning of the two detector planes inside the beam pipe in comparison to a
circu-lating beam at the origin. . . 25 4.1 xy hit distribution for 33Cl(p, γ)34Ar at resonance energy Er = 201 keV: elastic
scat-tering (mostly green with a big spike at the middle, for θ ≥ 5◦) and fusion products (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector posi-tions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 29 4.2 xy hit distribution for 33Cl(p, γ)34Ar at resonance energy Er = 956 keV: elastic
scat-tering (mostly green with a big spike at the middle, for θ ≥ 5◦) and fusion products (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector posi-tions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 32 4.3 xyhit distribution for 34mCl(p, γ)35Arat resonance energyEr= 110 keV: elastic
scat-tering (mostly green with a big spike at the middle, for θ ≥ 5◦) and fusion products (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector posi-tions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 34 4.4 xyhit distribution for 34mCl(p, γ)35Arat resonance energyEr= 916 keV: elastic
scat-tering (mostly green with a big spike at the middle, for θ ≥ 5◦) and fusion products (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector posi-tions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 36 4.5 Kinetic energy versus Time of Flight from the target to the detector position
-9-(maximum position after first quadrupole) for 34mCl(p, γ)35Ar at lowest resonance (Er CMS = 110 keV): elastically scattered 34mCl (red, for θ ≥ 5◦) and 35Ar fusion products (blue).. . . 38 4.6 cos(x)versusxat detector position -9- for34mCl(p, γ)35Arat lowest resonance (Er CMS=
110 keV): elastically scattered34mCl (red, forθ≥5◦) and35Ar fusion products (blue), black rectangle: inside particles are chosen for cut: see text for more . . . 38 4.7 Energy versus Time of Flight from the target to the detector position -9- for34mCl(p, γ)35Ar
at lowest resonance (Er CMS = 110 keV) with cut according to Figure 4.6: elastically scattered 34mCl (red, forθ≥5◦) and35Ar fusion products (blue).. . . 38 B.1 cos(x)versusxat detector position -9- for33Cl(p, γ)34Arat lowest resonance (Er CMS=
201 keV): elastically scattered 33Cl (red, forθ ≥5◦) and 34Ar fusion products (blue);
black rectangle: inside particles are chosen for cut: see text for more . . . 57
Technische Universität München 48 Physics Department
LIST OF FIGURES 49 B.2 Energy versus Time of Flight from the target to the detector position -9- for33Cl(p, γ)34Ar
at lowest resonance (Er CMS = 201 keV) with cut according to figure B.1: elastically scattered 33Cl (red, forθ≥5◦) and 34Ar fusion products (blue) . . . 57 B.3 cos(x)versusxat detector position -9- for33Cl(p, γ)34Arat resonance energyEr CMS=
956 keV: elastically scattered 33Cl (red, for θ ≥ 5◦) and 34Ar fusion products (blue);
black rectangle: inside particles are chosen for cut: see text for more . . . 58 B.4 Energy versus Time of Flight from the target to the detector position -9- for33Cl(p, γ)34Ar
at resonance energy Er CMS = 956 keV with cut according to figure B.1: elastically scattered 33Cl (red, forθ≥5◦) and 34Ar fusion products (blue) . . . 58 B.5 cos(x)versusxat detector position -9- for34mCl(p, γ)35Arat resonance energyEr CMS=
916 keV: elastically scattered34mCl (red, forθ≥5◦) and 35Ar fusion products (blue);
black rectangle: inside particles are chosen for cut: see text for more . . . 59 B.6 Energy versus Time of Flight from the target to the detector position -9- for34mCl(p, γ)35Ar
at resonance energy Er CMS = 916 keV with cut according to figure 4.6: elastically scattered 34mCl (red, forθ≥5◦) and 35Ar fusion products (blue) . . . 59 B.7 xyhit distribution for33Cl(p, γ)34Arat resonance energyEr CMS= 201 keVwith
emit-tance enabled: elastic scattering (mostly green with a big spike at the middle, for θ≥5◦) and (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible de-tector positions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 62 B.8 xyhit distribution for33Cl(p, γ)34Arat resonance energyEr CMS= 956 keVwith
emit-tance enabled: elastic scattering (mostly green with a big spike at the middle, for θ≥5◦) and (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible de-tector positions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 63 B.9 xy hit distribution for 34mCl(p, γ)35Ar at resonance energy Er CMS = 110 keV with
emittance enabled: elastic scattering (mostly green with a big spike at the middle, for θ≥5◦) and (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector positions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 66 B.10xy hit distribution for 34mCl(p, γ)35Ar at resonance energy Er CMS = 916 keV with
emittance enabled: elastic scattering (mostly green with a big spike at the middle, for θ≥5◦) and (pattern superimposed on top of elastic scattered beam, on the right hand side) with two detector planes (big and small rectangle) on the different possible detector positions: dipole: a, b, c; after quadrupole: d, e, f; after first hexapole: g. The cutoffs are due to beam pipe restrictions. . . 67 B.11cos(x)versusxat detector position -9- for33Cl(p, γ)34Arat lowest resonance (Er CMS=
201 keV) and emittance enabled: elastically scattered 33Cl (red, forθ ≥5◦) and 34Ar fusion products (blue); black rectangle: inside particles are chosen for cut . . . 68 B.12 Energy versus Time of Flight from the target to the detector position -9- for33Cl(p, γ)34Ar
at lowest resonance (Er CMS = 201 keV) with cut according to figure B.11 and emit-tance enabled: elastically scattered 33Cl (red, for θ ≥ 5◦) and 34Ar fusion products (blue) . . . 68 B.13cos(x)versusxat detector position -9- for33Cl(p, γ)34Arat resonance energyEr CMS=
956 keV and emittance enabled: elastically scattered 33Cl (red, forθ ≥ 5◦) and 34Ar fusion products (blue); black rectangle: inside particles are chosen for cut . . . 69
Physics Department 49 Technische Universität München
50 LIST OF FIGURES B.14 Energy versus Time of Flight from the target to the detector position -9- for33Cl(p, γ)34Ar
at resonance energyEr CMS= 956 keVwith cut according to figure B.13 and emittance enabled: elastically scattered 33Cl (red, forθ≥5◦) and 34Ar fusion products (blue). . 69 B.15 Energy versus Time of Flight from the target to the detector position -9- for34mCl(p, γ)35Ar
at lowest resonance (Er CMS = 110 keV) and emittance enabled: elastically scattered
34mCl (red, forθ≥5◦) and35Ar fusion products (blue) . . . 69 B.16cos(x)versusxat detector position -9- for34mCl(p, γ)35Arat lowest resonance (Er CMS=
110 keV) and emittance enabled: elastically scattered34mCl (red, forθ≥5◦) and35Ar fusion products (blue); black rectangle: inside particles are chosen for cut . . . 70 B.17 Energy versus Time of Flight from the target to the detector position -9- for34mCl(p, γ)35Ar
at lowest resonance (Er CMS = 110 keV) with cut according to figure B.16 and emit-tance enabled: elastically scattered 34mCl (red, for θ ≥5◦) and 35Ar fusion products (blue) . . . 70 B.18cos(x)versusxat detector position -9- for34mCl(p, γ)35Arat resonance energyEr CMS=
916 keV and emittance enabled: elastically scattered 34mCl (red, forθ≥5◦) and 35Ar fusion products (blue); black rectangle: inside particles are chosen for cut . . . 70 B.19 Energy versus Time of Flight from the target to the detector position -9- for34mCl(p, γ)35Ar
at resonance energyEr CMS= 916 keVwith cut according to figure B.18 and emittance enabled: elastically scattered 34mCl (red, forθ≥5◦) and35Ar fusion products (blue) . 71
Technische Universität München 50 Physics Department
List of Tables
1.1 Resonance energies for 33Cl(p, γ)34Ar and 34mCl(p, γ)35Ar reactions and nuclear core levels for the product nuclei within the energy range according to Figure 1.4. . . 6 3.1 SRIM calculation stopping power output for a 34Cl passing through a hydrogen gas
target with a target density ofρt= 5.9·1017atmos/cm3 at different beam energies. . . 23 3.2 Calculated Rutherford elastic cross section for each resonance energy of 33Cl(p, γ)34Ar
and 34Cl(p, γ)35Arwithin 5◦ to180◦ . . . 25 4.1 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 201 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 29 4.2 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 303 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 30 4.3 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 561 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 30 4.4 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 646 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 30 4.5 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 878 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 31 4.6 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A34Ar, inside detector planes atEr= 956 keVfor different detector positions for 33Cl(p, γ)34Arreaction. Both reaction channels are simulated with 1000000 particles. 31 4.7 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A35Ar, inside detector planes atEr= 110 keVfor different detector positions for34mCl(p, γ)35Arreaction. Both reaction channels are simulated with 1000000 particles. 34
51
52 LIST OF TABLES 4.8 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A35Ar, inside detector planes atEr= 215 keVfor different detector positions for34mCl(p, γ)35Arreaction. Both reaction channels are simulated with 1000000 particles. 35 4.9 Fraction of scattered beam inside the detector plane, Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A35Ar, inside detector planes atEr= 588 keVfor different detector positions for34mCl(p, γ)35Arreaction. Both reaction channels are simulated with 1000000 particles. 35 4.10 Fraction of scattered beam inside the detector plane,Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A35Ar, inside detector planes atEr= 784 keVfor different detector positions for34mCl(p, γ)35Arreaction. Both reaction channels are simulated with 1000000 particles. 35 4.11 Fraction of scattered beam inside the detector plane,Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products,A35Ar, inside detector planes atEr= 916 keVfor different detector positions for34mCl(p, γ)35Arreaction. Both reaction channels are simulated with 1000000 particles. 36 4.12 Elastically scattered particle rates for a beam of106 ions circulating at100 kHzat the
detector position -9- for each resonance energy of 33Cl(p, γ)34Ar and 34Cl(p, γ)35Ar, with and without emittance for different detector sizes . . . 39 B.1 Fraction of scattered beam inside the detector plane,Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion products, A34Ar, with emittance enabled inside the detectors atEr = 201 keVfor dif-ferent detector positions and for 33Cl(p, γ)34Ar reaction. Both reaction channels are simulated with 1000000 particles. . . 60 B.2 Fraction of scattered beam inside the detector plane,Ndet/Ntot, and effective
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion
Ruther-ford cross section of elastic scattered particles, σReff, and detector coverage of fusion