Notes 2

Nuclear Astrophysics is a combination of nuclear physics and astrophysics. Nuclear physics is the study of atomic nuclei, their composition and their interactions, while astrophysics aims at studying galactic objects such as stars and galaxies. Nuclear astrophysics delves into the questions of where and when the elements were created and how nuclear reactions drive cosmic events.

The Nucleus

Atomic nuclei sizes are on the scale of $10^{-14}$ meters and form the (relatively) small centers of atoms while carrying most of the mass. The basic constituents of atomic nuclei are protons and neutrons. Protons and neutrons are comprised of three quarks each, fundamental particles on a size scale of $10^{-19}m$. The relevant interactions on this size/mass scale are the electro-weak and strong forces. The quarks in a nucleon are

    Since Becquerel and Rutherford, much has been learned about nuclear physics. We now know that the atom is much more complex than Bohr's planetary like model could hope to explain. For instance, matter is not the lone constituent of the universe. There is also antimatter (save dark energy and matter for another day) with identical spin and mass but opposite charge. It seems for each massive particle, there is an antimatter equivalent denoted with a bar over its symbol. 
    The composition of the nucleus is on the most basic level comprised of protons (Z) and neutrons (N)

Definitions for Abundance

The particle abundance of isotope $i$ is defined as

$X_{i}={\frac {n_{i}}{\sum _{j}n_{j}}}\,$

where $n_{i}$ is the the number density of particle $i$, and the sum is taken over all isotopes present. It is also useful to define a relative particle abundance, which is set logarithmically and normalized to the abundance of hydrogen:

$\epsilon _{i}=\log _{10}X_{i}+12\ .$

The mass fraction is the fraction of total mass in the sample constituted by species $i$:

$X_{i}={\frac {m_{i}}{m_{tot}}}={\frac {m_{i}n_{i}}{\rho }}\approx {\frac {A_{i}n_{i}}{\rho N_{A}}}$ ( Note that $m_{i}\approx A_{i}m_{u}\$ and $m_{u}={\frac {m_{12C}}{12}}={\frac {1}{N_{A}}}$ )

Denoting $Y_{i}\,$ the mass per baryon, as

$Y_{i}\equiv {\frac {X_{i}}{A_{i}}},$

allows us to define the particle's number density by the density of the sample and this baryon fraction,

$n_{i}=Y_{i}\rho N_{A}\ .$

Another useful quantity is the average mass number, or mean molecular weight, defined by

$\mu _{i}={\frac {\sum _{i}{A_{i}Y_{i}}}{\sum _{i}{Y_{i}}}}={\frac {\sum _{i}{N_{i}}}{\sum _{i}Y_{i}}}={\frac {1}{\sum _{i}{Y_{i}}}}$

The electron abundance

$Y_{e}=\sum _{i}Z_{i}Y_{i}\$ , which can also be written as $Y_{e}={\frac {\sum _{i}{Z_{i}Y_{i}}}{\sum _{i}{A_{i}Y_{i}}}},$

is the ratio of protons to nucleons in the sample, and similarly to nuclei, the electron number density is found by

$n_{e}=Y_{e}\rho N_{A}\ .$