Nuclear Systematics

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» Lecture 1 Slides (PDF)
The lecture slides printed 4 X 4. We suggest you print these out and bring them to the lecture for annotation (~650 KB).

» Lecture 2 Slides
PDF of lecture 2 slides for annotation (1 MB). Print this up for annotation during lectures.

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A nice descriptive article about what kind of conditions our solar system may have been born in.

» Lecture 3 Slides
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» Lecture 4 Slides
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» Bateman's classic paper
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» Lecture 5 Slides
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» Basic Nuclear Physics
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» Stellar Nucleosynthesis
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» All about SN 1987A
A wiki page on SuperNova 1987A

Nuclear Systematics

This section of the course is intended to give the student a firm understanding of the underlying principles that determine the abundance, stability, and nature of the isotopes. We delve into the mechanisms and timing of the creation of the nuclides and the evidence behind our knowldege of these crucial processes. We investigate the mechanics and systematics of radioactive decay and its application to dating methods. We finish up with a problem solving session applying these techiques to determining the age of the elements (for our solar system).

Lecture 1, The Basics

Our starting point is to examine the cosmic abundance of the elements. From this, we embark on a quest to understand the factors underlying the stability of elements and isotopes, and the relation to their cosmic abundances. This also leads to a foundation for explaining the origin of the elements and isotopes (nucleosynthesis). We will outline the nature and relationship of the four fundamental forces, discuss the relativistic and quantum-mechanical principles underlying our understanding of the universe, and the factors controlling nuclear stability. We will also briefly discuss the modes of radioactive decay (more on that in Lecture 3).

Lecture 2, Nucleosynthesis

We aim to understand how the elements and isotopes came to be, within the context of the principles presented in Lecture 1, and how theses processes are reflected in the cosmic abunance of the elements and isotopes. We start on a wonderful journey that begins with the big bang (primoridal nucleosynthesis), through galactic evolution (generations of stars and galactic nuceosynthesis), and arrives at the amazing processes of stellar evolution and nucleosynthesis. We describe how our detailed knowledge of this incredible story is woven into the chart of the nuclides (isotopes) and outline the various nucleosynthetic pathways that lead to very stuff that we (and the earth) are made of.

Lecture 3, Radioactive Decay

The learning goals for this lecture are the derivation of the isochron equation (simple decay), a basic understanding of how radioactive decay can be used as a dating tool (isochron diagram), and an understanding of some of the pitfalls involved in dating (confusion with mixing lines).  We will also cover a special case where two decay systems of a single element leads to two stable isotopes of the same element (238U to 206Pb, 235U to 207Pb), and how these systematics can be used in an isochron diagram (Geochron, growth curves).

Lecture 4, Radioactive Decay Series

The learning goals for this lecture are to understand the more complex decay schemes that involve a series of coupled decays - so-called "decay series" -, the concept of secular equilibrium and disequilibrium, and how decay series can be used to constrain dates in closed vs. open systems.  We will introduce the Bateman equations and different equilibrium/disequilibrium diagrams that show the versatility and complexity of decay series dating.  The very different half-lives of the nuclides involved imply very different nuclide concentrations at secular equilibrium.  As the number of atoms available for analyses strongly influences analytical precision, we will also discuss analytical options (counting vs mass spectrometry) and their influence of analytical precision.

Lecture 5, Radioactive Decay - Extinct Radionuclides

We will review review simple decay and decay series systematics as an introduction into "extinct radionuclides".  The learning goals for this lecture are an understanding of the utility of nuclear reactions that involve nuclides with such short half-lifes that they do not exist anymore (unless newly produced by nuclear reactions) on Earth.  Such nuclides provide the foundation for relative dating of processes during the dawn of the Solar System.  These systematics will provide the basis for the next lecture(s) on the evolution of the Solar System and our home planet.

Lecture 6

We start solving the first problem of Problem Set 1 in class, using strategies for solving problems (carefully reading questions, graphical representation of concepts, simplifying equations, significant figures and uncertainties, dimensional analysis, etc.).


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Last updated September 29, 2012
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