Measurements of Radioactivity

Total Page:16

File Type:pdf, Size:1020Kb

Measurements of Radioactivity Measurements of Radioactivity United States Department of Commerce National Bureau of Standards Circular 476 UNITED STATES DEPARTMENT OF COMMERCE • Charles Sawyer, Secretary NATIONAL BUREAU OF STANDARDS • E. U. Condon, Director Measurements of Radioactivity by Leon F. Curtiss National Bureau of Standards Circular 476 Issued October 15, 1949 For sale by the Superintendent of Documents, U. S. Government Printing Office, Washington 25, D. C. Price .Q^ Preface This publication is a compilation of information intended to be useful to those starting out in research on problems in radioactivity and nuclear physics. An effort has been made to provide, in brief form, most of the essential background for all phases of experimental investigations in this general field. The number of topics involved limits the space that could be given to each, and the author is aware that for many items this has resulted in the elimination of important information. This defect may be corrected in future revisions, when criticisms and suggestions have indi- cated the direction of most useful expansion. This Circular is issued in its present form to provide a convenient source of the information contained and to provide an opportunity for those interested in this field to offer critical comments that can serve as the basis of an improved compilation. E. U. Condon, Director. Conlents Preface 11 VI. Radioactive radiations 37 1. Neutrons — 37 I. Introduction 1 2. Production of neutrons 37 1. Discovery 1 3. Mass of the neutron 37 2 . Statistical nature 1 4. Measurements of neutrons 38 3. Radioactive radiations 5 5. Fast neutrons 38 4. Artificial radioactivity 6 6. Slow neutrons 38 7. Counting alpha particles produced by II. Detection and measurement of radioactive neutron-induced distintegration 38 radiations 8 8. Counting gamma rays resulting from 1. Photographic emulsions 8 neutron capture 38 2. Crystals 9 9. Induced activities 39 3. Ionization of gases 10 10. Cross sections for reactions with 4. Measurement of charge transported by neutrons 39 alpha and beta rays 12 11. Radioactivity produced by neutrons 40 5. 12 Counting methods 12. Proton 41 6. Ionization chambers 12 13. Production of protons 41 7. Proportional counters 14 14. Detection and measurement of protons 41 8. Geiger-Muller counters 15 15. Radioactivity produced by proton 9. Electron multiplier 18 bombardment 42 10. Wilson cloud chamber 18 16. Deuterons 43 11. Calorimetric methods of measuring 17. Deuteron reactions 43 radioactive radiations 19 18. Alpha particles 44 III. Measurement of ionization currents 20 19. Range of alpha particles 44 1. Electroscopes 20 20. Bragg curve 45 2. Quartz fiber electroscopes 21 21. Stopping power 46 3. Electrometers 21 22. Geiger-Nuttall law 46 4. String electrometers 23 23. Scattering of alpha particles 47 5. Portable electrometers 23 24. Emission of alpha particles from the nucleus 47 6. Electrometer tubes 24 25. Beta particles 48 7. Vibrating reed electrometers 24 26. Measurement of beta rays 49 8. Ionization chambers 25 27. Measurements of beta rays with end window counters 49 IV. Radioactive substances 26 28. Beta-ray standards 50 1. Natural radioactivity 26 29. Electroscopes 50 2. Artificial radioactivity 28 30. Ionization chambers 51 3. Disintegration by protons 29 31. Beta-ray spectra 51 4. Disintegration by deuterons 30 32. Magnets for semicircular beta-ray 5. Disintegration by alpha particles 30 spectrographs 52 6. Distintegration by neutrons 30 33. Magnetic electron lens spectrometer 53 7. Disintegration by photons 30 34. Continuous beta-ray spectra 53 8. Alternate methods for producing a given 35. Neutrino 55 radioisotope 31 36. Fermi theory of beta-ray decay 55 9. Decay of artificially radioactive sub- 37. Absorption of beta particles 56 stances 31 38. Scattering of beta particles 56 10. Positron emission 31 39. Range of beta particles 56 11. Electron capture 31 40. Absorption method for determining 12. Isomeric transitions 31 energies of beta rays 57 41. Beta-ray energies by magnetic deflec- V. Equipment for producing artificially radio- tion 57 active isotopes 32 42. Positron 58 1. Voltage multiplier 32 43. Annihilation radiation and pair pro- 2. Cascade transformers 33 duction 58 3. Van de Graaf generator 34 44. Mesotrons 59 4. Linear accelerator 34 45. Artificial production of mesotrons 59 5. Cyclotron 35 46. Gamma rays 59 6. Betatron 35 47. Disintegration schemes 61 7. Synchrotron 36 48. Coincidence measurements 62 8. Uranium reactors 36 49. Absolute calibration of gamma-ray 9. Fission products 36 sources by coincidence 63 iii 50. Measurement of gamma radiation..... 64 4. Neutron standards 76 51. Counting gamma rays 65 5. Units used in radioactive measurements 76 52. Fission particles 65 in geology 79 53. Measurement of half-value periods 67 IX. Radioactivity ratio 79 54. Counter measurement of short half- 1. Uranium lead value periods 68 2. Helium content 79 55. Measurement of half-value periods with 3. Age of terrestial matter 79 counters 69 4. Determination of radium and thorium in 56. Determination of very long half-periods 70 rocks 80 57. Half-periods from true coincidence 5. Pleochroic halves 80 measurements 71 6. Generation of heat in the earth 80 58. Statistical error in measurement of half-value periods with counters 71 X. Health protection 81 1. Nature of radiation injuries 81 VII. Radioactive tracers 72 2. Genetic effects of radiation 81 1. Preparation and measurement of tracer 3. Visible evidence of injury from radiation 82 samples 73 4. Tolerance limits 82 2. Absolute measurements of tracer tolerance levels 82 samples 73 5. Measurements of 6. Alpha radiation 82 7. Protective precautions for substances VIII. Radioactive standards and units 74 emitting alpha rays 83 1. Alpha-ray standards 74 8. Protection from gamma rays 83 2. Beta-ray standards 74 3. Gamma-ray standards 75 XI. References 84 IV MEASUREMENTS OF RADIOACTIVITY I. INTRODUCTION 1. Discovery the limit of which, as x approaches zero, is e. Therefore The discovery of radioactivity illustrates how q'=e-^K 1 an incorrect hypothesis may stimulate experi- ( ) ments that lead to the discovery of new phenom- If at the time t—0 there is a large number No ena. After Roentgen had announced the dis- of radioactive atoms present, the number N, covery of X-rays in 1895, a search was insti- at any subsequent time t, is given by tuted by other physicists for substances that might emit naturally a similar radiation. Bec- N=No (2) querel concluded that since X-rays stimulated certain substances to a strong phosphorescence, This relation expresses the law of exponential such substances would be likely to emit a radia- decay so widely established experimentally in tion having the properties of X-radiation. Ac- the study of radioactivity, where A is the dis- cordingly, he exposed photographic plates, integration constant. wrapped in black paper, to a number of phos- Differentiating eq. 2 with respect to t, we ob- phorescent substances with uniformly negative tain for the rate of disintegration results until he tried salts of uranium. The suc- cess of this trial, announced in 1896, marks the dN discovery of radioactivity. =aNo e-^*=-AN, (3) dt 2. Statistical Nature the negative sign indicating that the number The fundamental nature of radioactivity can of unchanged atoms is decreasing. be described as a probability that the atoms of It has become customary to identify the rates a substance will undergo a transmutation spon- of disintegrations of radioactivity atoms by taneously into atoms of another element with a specifying the time required to decay to one- release of energy in the form of various types half the initial activity. This time is known as of radiation. If this probability is very small the half-value period, T. This period is the time, the substance is either stable or weakly radio- T, required for A/’/N(,=l/2=e“^^; or loge 2= active. If it is large it is strongly radioactive. -\T, from which r=0.693/a. To test this view, let us assume that the prob- Another constant that may be derived from ability that an atom of a given substance will the fundamental equation is the mean life, L, of disintegrate in an interval of time A is p, which the whole group of atoms. The number of atoms is the same for all atoms of the substance and transformed in time dt is given by \Ndt= independent of their age. For very small values xNq 6“^* dt. Each atom has a life t, hence the of A the probability, p, will be proportional to average life of all of them is the length of the interval so that p=AA, where A is a constant representing the probability that t\N(, dt an atom will disintegrate in unit time. Now the L=of oo =0/ 00 t\e-\* dt=l/\. probability, q, that an atom will not disinte- No grate in an interval A is q'=1-p= 1-AA. For a finite time t=/cA, the probability that an atom . (a) . Successive transformations —It is of in- will not be transformed is g'=(l-AA)*'= terest to determine the relative amounts of ( 1-AA ) which may be written radioactive substances when atoms of one type disintegrate successively into other types. These q'=[(l-AA) can be determined from the relation N=No for a number of conditions that are important Now let A become infinitely small while keep- in practice. To derive these relations we will ing the product A: A constant, that is t constant. assume that we have a radioactive chain con- sisting of three types of atoms. A, B, and C, in which A disintegrates to form B, which in turn disintegrates into C with the respective disin- tegration constants A^, A 2 , and Ag.
Recommended publications
  • Excitation Temperature, Degree of Ionization of Added Iron Species, and Electron Density in an Exploding Thin Film Plasma
    SpectmchimiccrACIO. Vol. MB. No. II. Pp.10814096. 1981. 0584-8547/81/111081-16SIZ.CNI/O Printedin Great Britain. PerpmonPress Ltd. Excitation temperature, degree of ionization of added iron species, and electron density in an exploding thin film plasma S. Y. SUH* and R. D. SACKS Department of Chemistry, University of Michigan, Ann Arbor, Ml 48109, U.S.A. (Received 7 April 1981) Abstract-Time and spatially resolved spectra of a cylindrically symmetric exploding thin film plasma were obtained with a rotating mirror camera and astigmatic imaging. These spectra were deconvoluted to obtain relative spectral emissivity profiles for nine Fe(H) and two Fe(I) lines. The effective (electronic) excitation temperature at various positions in the plasma and at various times during the first current halfcycle was computed from the Fe(H) emissivity values using the Boltzmann graphical method. The Fe(II)/Fe(I) emissivity ratios together with the temperature were used to determine the degree of ionization of Fe. Finally, the electron density was estimated from the Saha equilibrium. Electronic excitation temperatures range from lO,OOO-15,OOOKnear the electrode surface at peak discharge current to 700&10.000K at 6-10 mm above the electrode surface at the first current zero. Corresponding electron densities range from 10’7-10u cm-’ at peak current to 10’~-10’6cm-3 near zero current. Error propagation and criteria for thermodynamic equilibrium are discussed. 1. IN-~R~DU~~ION THE HIGH-TEMPERATURE plasmas produced by the rapid electrical vaporization of Ag thin films recently have been used as atomization cells and excitation sources for the direct determination of selected elements in micro-size powder samples [ 11.
    [Show full text]
  • Ionization Balance in EBIT and Tokamak Plasmas N
    Ionization balance in EBIT and tokamak plasmas N. J. Peacock, R. Barnsley, M. G. O’Mullane, M. R. Tarbutt, D. Crosby et al. Citation: Rev. Sci. Instrum. 72, 1250 (2001); doi: 10.1063/1.1324755 View online: http://dx.doi.org/10.1063/1.1324755 View Table of Contents: http://rsi.aip.org/resource/1/RSINAK/v72/i1 Published by the American Institute of Physics. Related Articles Bragg x-ray survey spectrometer for ITER Rev. Sci. Instrum. 83, 10E126 (2012) Novel energy resolving x-ray pinhole camera on Alcator C-Mod Rev. Sci. Instrum. 83, 10E526 (2012) Measurement of electron temperature of imploded capsules at the National Ignition Facility Rev. Sci. Instrum. 83, 10E121 (2012) South pole bang-time diagnostic on the National Ignition Facility (invited) Rev. Sci. Instrum. 83, 10E119 (2012) Temperature diagnostics of ECR plasma by measurement of electron bremsstrahlung Rev. Sci. Instrum. 83, 073111 (2012) Additional information on Rev. Sci. Instrum. Journal Homepage: http://rsi.aip.org Journal Information: http://rsi.aip.org/about/about_the_journal Top downloads: http://rsi.aip.org/features/most_downloaded Information for Authors: http://rsi.aip.org/authors Downloaded 08 Aug 2012 to 194.81.223.66. Redistribution subject to AIP license or copyright; see http://rsi.aip.org/about/rights_and_permissions REVIEW OF SCIENTIFIC INSTRUMENTS VOLUME 72, NUMBER 1 JANUARY 2001 Ionization balance in EBIT and tokamak plasmas N. J. Peacock,a) R. Barnsley,b) and M. G. O’Mullane Euratom/UKAEA Fusion Association, Culham Science Centre, Abingdon, Oxon OX14 3DB, United Kingdom M. R. Tarbutt, D. Crosby, and J. D. Silver The Clarendon Laboratory, University of Oxford, Parks Road, Oxford OX1 3PU, United Kingdom J.
    [Show full text]
  • How the Saha Ionization Equation Was Discovered
    How the Saha Ionization Equation Was Discovered Arnab Rai Choudhuri Department of Physics, Indian Institute of Science, Bangalore – 560012 Introduction Most youngsters aspiring for a career in physics research would be learning the basic research tools under the guidance of a supervisor at the age of 26. It was at this tender age of 26 that Meghnad Saha, who was working at Calcutta University far away from the world’s major centres of physics research and who never had a formal training from any research supervisor, formulated the celebrated Saha ionization equation and revolutionized astrophysics by applying it to solve some long-standing astrophysical problems. The Saha ionization equation is a standard topic in statistical mechanics and is covered in many well-known textbooks of thermodynamics and statistical mechanics [1–3]. Professional physicists are expected to be familiar with it and to know how it can be derived from the fundamental principles of statistical mechanics. But most professional physicists probably would not know the exact nature of Saha’s contributions in the field. Was he the first person who derived and arrived at this equation? It may come as a surprise to many to know that Saha did not derive the equation named after him! He was not even the first person to write down this equation! The equation now called the Saha ionization equation appeared in at least two papers (by J. Eggert [4] and by F.A. Lindemann [5]) published before the first paper by Saha on this subject. The story of how the theory of thermal ionization came into being is full of many dramatic twists and turns.
    [Show full text]
  • 1 Introduction
    i i Karl-Heinz Spatschek: High Temperature Plasmas — Chap. spatscheck0415c01 — 2011/9/1 — page 1 — le-tex i i 1 1 Introduction A plasma is a many body system consisting of a huge number of interacting (charged and neutral) particles. More precisely, one defines a plasma as a quasineu- tral gas of charged and neutral particles which exhibits collective behavior. In many cases, one considers quasineutral gases consisting of charged particles, namely electrons and positively charged ions of one species. Plasmas may contain neutral atoms. In this case, the plasma is called partially or incompletely ionized. Other- wise the plasma is said to be completely or fully ionized. The term plasma is not limited to the most common electron–ion case. One may have electron–positron plasmas, quark-gluon plasmas, and so on. Semiconductors contain plasma con- sisting of electrons and holes. Most of the matter in the universe occurs in the plasma state. It is often said that 99% of the matter in the universe is in the plasma state. However, this estimate may not be very accurate. Remember the discussion on dark matter. Nevertheless, the plasma state is certainly dominating the universe. Modern plasma physics emerged in 1950s, when the idea of thermonuclear re- actor was introduced. Fortunately, modern plasma physics completely dissociated from weapons development. The progression of modern plasma physics can be retraced from many monographs, for example, [1–15]. In simple terms, plasmas can be characterized by two parameters, namely, charged particle density n and temperature T. The density varies over roughly 28 6 34 3 orders of magnitude, for example, from 10 to 10 m .
    [Show full text]
  • Lecture 8: Statistical Equilibria, Saha Equation
    Statistical Equilibria: Saha Equation We are now going to consider the statistics of equilibrium. Specifically, suppose we let a system stand still for an extremely long time, so that all processes can come into balance. We then measure the fraction of particles that are in each of several states (e.g., if we have a pure hydrogen gas, we might want to know the ionization fraction). How can we compute this fraction? We’ll take a look at this in several different ways. We will then step back and ask ourselves when these equilibrium formulae do not apply. This is important! To paraphrase Clint Eastwood, “An equation’s got to know its limitations”. In virtually all astronomical problems we deal with approximations, so we always need a sense of when those approximations fail. This serves a double purpose: it keeps us from making errors, but it also keeps us from applying too complex an approach to a simple problem. Let’s start out with a simple case. We consider a column of isothermal gas (temperature T ) in a constant gravitational acceleration g. Each molecule has mass m. If we can treat this like an ideal gas, Ask class: how do we figure out how the pressure vary with height h? An ideal gas has pressure P = nkT , where n is the number density. In equilibrium the pressure gradient balances the weight of the gas, so dP/dh = −ρg. Using ρ = nm = P m/kT and the constancy of T , we have dP/dh = −(mg/kT )P , so P = P0 exp(−mgh/kT ), where P0 is defined as the pressure at h = 0.
    [Show full text]
  • Example 1 Nicotinic Acid Is a Monoprotic Acid
    Weak acids and bases Example 1 Nicotinic acid is a monoprotic acid. A solution that is 0.012 M in nicotinic acid has a pH of 3.39. What is the acid ionization constant (Ka)? What is the degree of ionization of nicotinic acid in this solution? Solution When we say the solution is 0.012 M, this refers to how the solution is prepared. The solution is made up by adding 0.012 mol of substance to enough water to give a liter of solution. Once the solution is prepared, some molecules ionize, so the actual concentration is somewhat less than 0.012 M. - + We start with 0.012 M of acid (HNic) before ionization, i.e. [Nic ]=0 before ionization. The H3O concentration at the start is that from the self-ionization of water. It is usually much smaller than that obtained from the acid (unless the solution is extremely dilute or Ka is quite small), so you can write + + – [H3O ] = ~ 0 (meaning approximately zero). If x mol HNic ionizes, x mol each of H3O and Nic is formed, leaving (0.012 - x) mol HNic in solution. You can summarize the situation in the table: + – Concentration (M) HNic(aq) + H2O(l) <==> H3O (aq) + Nic (aq) Starting 0.012 ~0 0 Change -x +x +x Equilibrium 0.012 - x x x The equilibrium-constant equation is + – [H3O ][Nic ] Ka = [HNic] When you substitute the expressions for the equilibrium concentrations, you get x2 Ka = (0.012 - x) The value of x equals the numerical value of the molar hydronium-ion concentration, and can be obtained from the pH of the solution.
    [Show full text]
  • Lecture Notes in Physics Introduction to Plasma Physics
    Lecture Notes in Physics Introduction to Plasma Physics Michael Gedalin ii Contents 1 Basic definitions and parameters 1 1.1 What is plasma . 1 1.2 Debye shielding . 2 1.3 Plasma parameter . 4 1.4 Plasma oscillations . 5 1.5 ∗Ionization degree∗ ............................ 5 1.6 Summary . 6 1.7 Problems . 7 2 Plasma description 9 2.1 Hierarchy of descriptions . 9 2.2 Fluid description . 10 2.3 Continuity equation . 10 2.4 Motion (Euler) equation . 11 2.5 State equation . 12 2.6 MHD . 12 2.7 Order-of-magnitude estimates . 14 2.8 Summary . 14 2.9 Problems . 15 3 MHD equilibria and waves 17 3.1 Magnetic field diffusion and dragging . 17 3.2 Equilibrium conditions . 18 3.3 MHD waves . 19 3.4 Alfven and magnetosonic modes . 22 3.5 Wave energy . 23 3.6 Summary . 24 3.7 Problems . 24 iii CONTENTS 4 MHD discontinuities 27 4.1 Stationary structures . 27 4.2 Discontinuities . 28 4.3 Shocks . 29 4.4 Why shocks ? . 31 4.5 Problems . 32 5 Two-fluid description 33 5.1 Basic equations . 33 5.2 Reduction to MHD . 34 5.3 Generalized Ohm’s law . 35 5.4 Problems . 36 6 Waves in dispersive media 37 6.1 Maxwell equations for waves . 37 6.2 Wave amplitude, velocity etc. 38 6.3 Wave energy . 40 6.4 Problems . 44 7 Waves in two-fluid hydrodynamics 47 7.1 Dispersion relation . 47 7.2 Unmagnetized plasma . 49 7.3 Parallel propagation . 49 7.4 Perpendicular propagation . 50 7.5 General properties of the dispersion relation .
    [Show full text]
  • 193 9Ap J. the PHYSICAL STATE of INTERSTELLAR HYDROGEN Co
    CDco CMLO OC CO THE PHYSICAL STATE OF INTERSTELLAR J. HYDROGEN 9Ap BENGT STRÖMGREN 193 ABSTRACT The discovery, by Struve and Elvey, of extended areas in the Milky Way in which the Balmer lines are observed in emission suggests that hydrogen exists, in the ionized state, in large regions of space. The problem of the ionization and excitation of hydro- gen is first considered in a general way. An attempt is then made to arrive at a picture of the actual physical state of interstellar hydrogen. It is found that the Balmer-line emission should be limited to certain rather sharply bounded regions in space surround- ing O-type stars or clusters of O-type stars. Such regions may have diameters of about zoo parsecs, which is in general agreement with the observations. Certain aspects of the problem of the ionization of other elements and of the problem of the relative abundance of the elements in interstellar space are briefly discussed. The interstellar density of hydrogen is of the order of A = 3 cm-3. The extent of the emission regions at right angles to the galactic plane is discussed and is found to be small. I The recent discovery, by Struve and Elvey,1 of extended regions in the Milky Way showing hydrogen-hne emission has opened up new and highly important possibilities for the study of the properties of interstellar matter. From the observed strength of Z7a in the emission regions, Struve2 has calculated the density of interstellar hydrogen. Also, he has analyzed the problem of the ionization of interstellar calcium and sodium, taking account of the presence of ionized hydrogen.
    [Show full text]
  • Lecture Note 1
    Lecture Note 1 1.1 Plasma 99% of the matter in the universe is in the plasma state. Solid -> liquid -> Gas -> Plasma (The fourth state of matter) Recall: Concept of Temperature A gas in thermal equilibrium has particles of all velocities, and the most probable distribution of these velocities is known as the Maxwellian distribution. The average kinetic energy Eav equals 1/2kT per degree of freedom. k is Boltzmann’s constant. Since T and Eav are so closed related, it is customary in plasma physics to give temperatures in units of energy. To avoid confusion on the number of dimensions involved, it is not Eav , but the energy corresponding to kT that is used to denote the temperature. For kT = 1 eV = 1.6 x 10-19 J, we have 1.6× 10−19 T ==11,600 1.38× 10−23 Thus the conversion factor is 1eV = 11,600 K A plasma is a gas in which an important fraction of the atoms in ionized, so that the electrons and ions are separately free. When does this ionization occur? When the temperature is hot enough. Saha Equation: Which tells us the amount of ionization to be expected in a gas in thermal equilibrium: 3/2 ni 21 T ≈×2.4 10 exp( −UkTi / ) nnni 3 Here ni and nn are, respectively, the number density (number per m ) of ionized atoms and of neutral atoms, T is the gas temperature in K, k is Boltzmann’s constant, and Ui is the ionization energy of the gas—that is, the number of ergs required to remove the outmost electron from an atom.
    [Show full text]
  • Statistical Equilibria: Saha Equation Initial Questions: What Sets the Temperature of the Warm Interstellar Medium? What Determi
    Statistical Equilibria: Saha Equation Initial questions: What sets the temperature of the warm interstellar medium? What determines the epoch from which we see the CMB? We are now going to consider the statistics of equilibrium. Specifically, suppose we let a system stand still for an extremely long time, so that all processes can come into balance. We then measure the fraction of particles that are in each of several states (e.g., if we have a pure hydrogen gas, we might want to know the ionization fraction). How can we compute this fraction? We’ll take a look at this in several different ways. We will then step back and ask ourselves when these equilibrium formulae do not apply. This is important! To paraphrase Clint Eastwood, “An equation’s got to know its limitations”. In virtually all astronomical problems we deal with approximations, so we always need a sense of when those approximations fail. This serves a double purpose: it keeps us from making errors, but it also keeps us from applying too complex an approach to a simple problem. Let’s start out with a simple case. We consider a column of isothermal gas (temperature T ) in a constant gravitational acceleration g. Each molecule has mass m. If we can treat this like an ideal gas, Ask class: how do we figure out how the pressure varies with height h? An ideal gas has pressure P = nkT , where n is the number density. In equilibrium the pressure gradient balances the weight of the gas, so dP/dh = −ρg. Using ρ = nm = Pm/kT and the constancy of T , we have dP/dh = −(mg/kT )P , so P = P0 exp(−mgh/kT ), where P0 is defined as the pressure at h = 0.
    [Show full text]
  • Charge and Energy Interactions Between Nanoparticles and Low Pressure Plasmas
    Charge and Energy Interactions between Nanoparticles and Low Pressure Plasmas A DISSERTATION SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY Federico Galli IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Prof. Uwe R. Kortshagen, Adviser May 2010 © Federico Galli May 2010 Acknowledgments I would like to thank my adviser, Professor Uwe Kortshagen, for his guidance and mentoring during the years of my graduate career. To my colleagues and friends in the HTPL group and at the University of Minnesota: thank you for five years of intellectual and personal enrichment. To all the friends and people that I had the opportunity to meet here in Minnesota: you made me feel like at home. Last but first in my heart: thank you family, for everything. i Abstract In this work, the interactions between low-pressure plasmas and nanoparticles are studied with numerical models aimed at understanding the phenomena that affect the nanoparticles charge, charge distribution, heating, and crystallization dinamycs. At the same time other phenomena that affect the plasma properties resulting from the presence of nanoparticles are also studied: they include the power-coupling to the plasmas, the ion energy distribution and the electron energy distribution. An analytical model predicting the nano-particle charge and temperature distribu- tions in a low pressure plasma is developed. The model includes the effect of collisions between ions and neutrals in proximity of the particles. In agreement with experi- mental evidence for pressures of a few Torr a charge distribution that is less negative than the prediction from the collisionless orbital motion limited theory is obtained.
    [Show full text]
  • Diagnostic Studies of Ion Beam Formation in Inductively Coupled Plasma Mass Spectrometry with the Collision Reaction Interface Jeneé L
    Iowa State University Capstones, Theses and Graduate Theses and Dissertations Dissertations 2015 Diagnostic studies of ion beam formation in inductively coupled plasma mass spectrometry with the collision reaction interface Jeneé L. Jacobs Iowa State University Follow this and additional works at: https://lib.dr.iastate.edu/etd Part of the Analytical Chemistry Commons Recommended Citation Jacobs, Jeneé L., "Diagnostic studies of ion beam formation in inductively coupled plasma mass spectrometry with the collision reaction interface" (2015). Graduate Theses and Dissertations. 14814. https://lib.dr.iastate.edu/etd/14814 This Dissertation is brought to you for free and open access by the Iowa State University Capstones, Theses and Dissertations at Iowa State University Digital Repository. It has been accepted for inclusion in Graduate Theses and Dissertations by an authorized administrator of Iowa State University Digital Repository. For more information, please contact [email protected]. i Diagnostic studies of ion beam formation in inductively coupled plasma mass spectrometry with the collision reaction interface by Jeneé L. Jacobs A dissertation submitted to the graduate faculty in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY Major: Analytical Chemistry Program of Study Committee: Robert S. Houk, Major Professor Young-Jin Lee Emily Smith Patricia Thiel Javier Vela Iowa State University Ames, Iowa 2015 Copyright © Jeneé L. Jacobs, 2015. All right reserved. ii TABLE OF CONTENTS ABSTRACT vi CHAPTER 1. GENERAL INTRODUCTION 1 Inductively Coupled Plasma Mass Spectrometry 1 ICP 1 Ion Extraction 3 Polyatomic Ion Interferences 4 Polyatomic Ion Mitigation Techniques 5 Characteristics of Collision Technology 7 Dissertation Organization 8 References 9 Figures 14 CHAPTER 2.
    [Show full text]