Discoveries in nuclear physics have led to applications in many fields. This includes nuclear power, nuclear weapons, nuclear medicine and magnetic resonance imaging, industrial and agricultural isotopes, ion implantation in materials engineering, and radiocarbon dating in geology and archaeology. Such applications are studied in the field of nuclear engineering.
Particle physics evolved out of nuclear physics and the two fields are typically taught in close association. Nuclear astrophysics, the application of nuclear physics to astrophysics, is crucial in explaining the inner workings of stars and the origin of the chemical elements.
Particle physics evolved out of nuclear physics and the two fields are typically taught in close association. Nuclear astrophysics, the application of nuclear physics to astrophysics, is crucial in explaining the inner workings of stars and the origin of the chemical elements.
History
Since 1920s cloud chambers played an important role of particle detectors and eventually lead to the discovery of positron, muon and kaon.
The history of nuclear physics as a discipline distinct from atomic physics starts with the discovery of radioactivity by Henri Becquerel in 1896, while investigating phosphorescence in uranium salts. The discovery of the electron by J. J. Thomson
a year later was an indication that the atom had internal structure. At
the beginning of the 20th century the accepted model of the atom was J.
J. Thomson's "plum pudding" model in which the atom was a positively charged ball with smaller negatively charged electrons embedded inside it.
In the years that followed, radioactivity was extensively investigated, notably by Marie and Pierre Curie as well as by Ernest Rutherford and his collaborators. By the turn of the century physicists had also discovered three types of radiation emanating from atoms, which they named alpha, beta, and gamma radiation. Experiments by Otto Hahn in 1911 and by James Chadwick in 1914 discovered that the beta decay spectrum
was continuous rather than discrete. That is, electrons were ejected
from the atom with a continuous range of energies, rather than the
discrete amounts of energy that were observed in gamma and alpha decays.
This was a problem for nuclear physics at the time, because it seemed
to indicate that energy was not conserved in these decays.
The 1903 Nobel Prize
in Physics was awarded jointly to Becquerel for his discovery and to
Marie and Pierre Curie for their subsequent research into radioactivity.
Rutherford was awarded the Nobel Prize in Chemistry in 1908 for his
"investigations into the disintegration of the elements and the
chemistry of radioactive substances".
In 1905 Albert Einstein formulated the idea of mass–energy equivalence.
While the work on radioactivity by Becquerel and Marie Curie predates
this, an explanation of the source of the energy of radioactivity would
have to wait for the discovery that the nucleus itself was composed of
smaller constituents, the nucleons.
Rutherford's team discovers the nucleus
In 1906 Ernest Rutherford published "Retardation of the α Particle from Radium in passing through matter." Hans Geiger expanded on this work in a communication to the Royal Society
with experiments he and Rutherford had done, passing alpha particles
through air, aluminum foil and gold leaf. More work was published in
1909 by Geiger and Ernest Marsden, and further greatly expanded work was published in 1910 by Geiger.
In 1911–1912 Rutherford went before the Royal Society to explain the
experiments and propound the new theory of the atomic nucleus as we now
understand it.
The key experiment behind this announcement was performed in 1910 at the University of Manchester: Ernest Rutherford's team performed a remarkable experiment in which Geiger and Marsden under Rutherford's supervision fired alpha particles (helium nuclei) at a thin film of gold foil. The plum pudding model
had predicted that the alpha particles should come out of the foil with
their trajectories being at most slightly bent. But Rutherford
instructed his team to look for something that shocked him to observe: a
few particles were scattered through large angles, even completely
backwards in some cases. He likened it to firing a bullet at tissue
paper and having it bounce off. The discovery, with Rutherford's
analysis of the data in 1911, led to the Rutherford model of the atom,
in which the atom had a very small, very dense nucleus containing most
of its mass, and consisting of heavy positively charged particles with
embedded electrons in order to balance out the charge (since the neutron
was unknown). As an example, in this model (which is not the modern
one) nitrogen-14 consisted of a nucleus with 14 protons and 7 electrons
(21 total particles) and the nucleus was surrounded by 7 more orbiting
electrons.
Around 1920, Arthur Eddington anticipated the discovery and mechanism of nuclear fusion processes in stars, in his paper The Internal Constitution of the Stars. At that time, the source of stellar energy was a complete mystery; Eddington correctly speculated that the source was fusion of hydrogen into helium, liberating enormous energy according to Einstein's equation E = mc2.
This was a particularly remarkable development since at that time
fusion and thermonuclear energy, and even that stars are largely
composed of hydrogen, had not yet been discovered.
The Rutherford model worked quite well until studies of nuclear spin were carried out by Franco Rasetti at the California Institute of Technology in 1929. By 1925 it was known that protons and electrons each had a spin of +/-1⁄2.
In the Rutherford model of nitrogen-14, 20 of the total 21 nuclear
particles should have paired up to cancel each other's spin, and the
final odd particle should have left the nucleus with a net spin of 1⁄2. Rasetti discovered, however, that nitrogen-14 had a spin of 1.
James Chadwick discovers the neutron
In 1932 Chadwick realized that radiation that had been observed by Walther Bothe, Herbert Becker, Irène and Frédéric Joliot-Curie was actually due to a neutral particle of about the same mass as the proton, that he called the neutron (following a suggestion from Rutherford about the need for such a particle). In the same year Dmitri Ivanenko suggested that there were no electrons in the nucleus — only protons and neutrons — and that neutrons were spin 1⁄2
particles which explained the mass not due to protons. The neutron spin
immediately solved the problem of the spin of nitrogen-14, as the one
unpaired proton and one unpaired neutron in this model each contributed a
spin of 1⁄2 in the same direction, giving a final total spin of 1.
With the discovery of the neutron, scientists could at last calculate what fraction of binding energy
each nucleus had, by comparing the nuclear mass with that of the
protons and neutrons which composed it. Differences between nuclear
masses were calculated in this way. When nuclear reactions were
measured, these were found to agree with Einstein's calculation of the
equivalence of mass and energy to within 1% as of 1934.
Proca's equations of the massive vector boson field
Alexandru Proca was the first to develop and report the massive vector boson field equations and a theory of the mesonic field of nuclear forces. Proca's equations were known to Wolfgang Pauli
who mentioned the equations in his Nobel address, and they were also
known to Yukawa, Wentzel, Taketani, Sakata, Kemmer, Heitler, and
Fröhlich who appreciated the content of Proca's equations for developing
a theory of the atomic nuclei in Nuclear Physics.
Yukawa's meson postulated to bind nuclei
In 1935 Hideki Yukawa proposed the first significant theory of the strong force to explain how the nucleus holds together. In the Yukawa interaction a virtual particle, later called a meson,
mediated a force between all nucleons, including protons and neutrons.
This force explained why nuclei did not disintegrate under the influence
of proton repulsion, and it also gave an explanation of why the
attractive strong force had a more limited range than the electromagnetic repulsion between protons. Later, the discovery of the pi meson showed it to have the properties of Yukawa's particle.
With Yukawa's papers, the modern model of the atom was complete.
The center of the atom contains a tight ball of neutrons and protons,
which is held together by the strong nuclear force, unless it is too
large. Unstable nuclei may undergo alpha decay, in which they emit an
energetic helium nucleus, or beta decay, in which they eject an electron
(or positron).
After one of these decays the resultant nucleus may be left in an
excited state, and in this case it decays to its ground state by
emitting high energy photons (gamma decay).
The study of the strong and weak nuclear forces (the latter explained by Enrico Fermi via Fermi's interaction in 1934) led physicists to collide nuclei and electrons at ever higher energies. This research became the science of particle physics, the crown jewel of which is the standard model of particle physics which describes the strong, weak, and electromagnetic forces.
Modern nuclear physics
A heavy nucleus can contain hundreds of nucleons. This means that with some approximation it can be treated as a classical system, rather than a quantum-mechanical one. In the resulting liquid-drop model, the nucleus has an energy which arises partly from surface tension
and partly from electrical repulsion of the protons. The liquid-drop
model is able to reproduce many features of nuclei, including the
general trend of binding energy with respect to mass number, as well as the phenomenon of nuclear fission.
Superimposed on this classical picture, however, are quantum-mechanical effects, which can be described using the nuclear shell model, developed in large part by Maria Goeppert Mayer and J. Hans D. Jensen. Nuclei with certain numbers of neutrons and protons (the magic numbers 2, 8, 20, 28, 50, 82, 126, ...) are particularly stable, because their shells are filled.
Other more complicated models for the nucleus have also been proposed, such as the interacting boson model, in which pairs of neutrons and protons interact as bosons, analogously to Cooper pairs of electrons.
Ab initio methods try to solve the nuclear many-body problem from the ground up, starting from the nucleons and their interactions.
Much of current research in nuclear physics relates to the study of nuclei under extreme conditions such as high spin and excitation energy. Nuclei may also have extreme shapes (similar to that of Rugby balls or even pears)
or extreme neutron-to-proton ratios. Experimenters can create such
nuclei using artificially induced fusion or nucleon transfer reactions,
employing ion beams from an accelerator.
Beams with even higher energies can be used to create nuclei at very
high temperatures, and there are signs that these experiments have
produced a phase transition from normal nuclear matter to a new state, the quark–gluon plasma, in which the quarks mingle with one another, rather than being segregated in triplets as they are in neutrons and protons.
Nuclear decay
Eighty elements have at least one stable isotope which is never observed to decay, amounting to a total of about 254 stable isotopes. However, thousands of isotopes
have been characterized as unstable. These "radioisotopes" decay over
time scales ranging from fractions of a second to trillions of years.
Plotted on a chart as a function of atomic and neutron numbers, the
binding energy of the nuclides forms what is known as the valley of stability.
Stable nuclides lie along the bottom of this energy valley, while
increasingly unstable nuclides lie up the valley walls, that is, have
weaker binding energy.
The most stable nuclei fall within certain ranges or balances of
composition of neutrons and protons: too few or too many neutrons (in
relation to the number of protons) will cause it to decay. For example,
in beta decay a nitrogen-16 atom (7 protons, 9 neutrons) is converted to an oxygen-16 atom (8 protons, 8 neutrons) within a few seconds of being created. In this decay a neutron in the nitrogen nucleus is converted by the weak interaction into a proton, an electron and an antineutrino. The element is transmuted to another element, with a different number of protons.
In alpha decay
(which typically occurs in the heaviest nuclei) the radioactive element
decays by emitting a helium nucleus (2 protons and 2 neutrons), giving
another element, plus helium-4. In many cases this process continues
through several steps of this kind, including other types of decays
(usually beta decay) until a stable element is formed.
In gamma decay, a nucleus decays from an excited state into a lower energy state, by emitting a gamma ray. The element is not changed to another element in the process (no nuclear transmutation is involved).
Other more exotic decays are possible (see the first main article). For example, in internal conversion
decay, the energy from an excited nucleus may eject one of the inner
orbital electrons from the atom, in a process which produces high speed
electrons, but is not beta decay, and (unlike beta decay) does not transmute one element to another.
Nuclear fusion
In nuclear fusion,
two low mass nuclei come into very close contact with each other, so
that the strong force fuses them. It requires a large amount of energy
for the strong or nuclear forces
to overcome the electrical repulsion between the nuclei in order to
fuse them; therefore nuclear fusion can only take place at very high
temperatures or high pressures. When nuclei fuse, a very large amount of
energy is released and the combined nucleus assumes a lower energy
level. The binding energy per nucleon increases with mass number up to nickel-62. Stars like the Sun are powered by the fusion of four protons into a helium nucleus, two positrons, and two neutrinos.
The uncontrolled fusion of hydrogen into helium is known as
thermonuclear runaway. A frontier in current research at various
institutions, for example the Joint European Torus (JET) and ITER,
is the development of an economically viable method of using energy
from a controlled fusion reaction.
Nuclear fusion is the origin of the energy (including in the form of
light and other electromagnetic radiation) produced by the core of all
stars including our own Sun.
Nuclear fission
Nuclear fission
is the reverse process to fusion. For nuclei heavier than nickel-62 the
binding energy per nucleon decreases with the mass number. It is
therefore possible for energy to be released if a heavy nucleus breaks
apart into two lighter ones.
The process of alpha decay is in essence a special type of spontaneous nuclear fission.
It is a highly asymmetrical fission because the four particles which
make up the alpha particle are especially tightly bound to each other,
making production of this nucleus in fission particularly likely.
From certain of the heaviest nuclei whose fission produces free
neutrons, and which also easily absorb neutrons to initiate fission, a
self-igniting type of neutron-initiated fission can be obtained, in a chain reaction.
Chain reactions were known in chemistry before physics, and in fact
many familiar processes like fires and chemical explosions are chemical
chain reactions. The fission or "nuclear" chain-reaction, using fission-produced neutrons, is the source of energy for nuclear power plants and fission type nuclear bombs, such as those detonated in Hiroshima and Nagasaki, Japan, at the end of World War II. Heavy nuclei such as uranium and thorium may also undergo spontaneous fission, but they are much more likely to undergo decay by alpha decay.
For a neutron-initiated chain reaction to occur, there must be a critical mass
of the relevant isotope present in a certain space under certain
conditions. The conditions for the smallest critical mass require the
conservation of the emitted neutrons and also their slowing or moderation so that there is a greater cross-section or probability of them initiating another fission. In two regions of Oklo, Gabon, Africa, natural nuclear fission reactors were active over 1.5 billion years ago.[24]
Measurements of natural neutrino emission have demonstrated that around
half of the heat emanating from the Earth's core results from
radioactive decay. However, it is not known if any of this results from
fission chain reactions.
Production of "heavy" elements
According to the theory, as the Universe cooled after the Big Bang
it eventually became possible for common subatomic particles as we know
them (neutrons, protons and electrons) to exist. The most common
particles created in the Big Bang which are still easily observable to
us today were protons and electrons (in equal numbers). The protons
would eventually form hydrogen atoms. Almost all the neutrons created in
the Big Bang were absorbed into helium-4 in the first three minutes after the Big Bang, and this helium accounts for most of the helium in the universe today.
Some relatively small quantities of elements beyond helium
(lithium, beryllium, and perhaps some boron) were created in the Big
Bang, as the protons and neutrons collided with each other, but all of
the "heavier elements" (carbon, element number 6, and elements of
greater atomic number) that we see today, were created inside stars during a series of fusion stages, such as the proton-proton chain, the CNO cycle and the triple-alpha process. Progressively heavier elements are created during the evolution of a star.
Since the binding energy per nucleon
peaks around iron (56 nucleons), energy is only released in fusion
processes involving smaller atoms than that. Since the creation of
heavier nuclei by fusion requires energy, nature resorts to the process
of neutron capture. Neutrons (due to their lack of charge) are readily
absorbed by a nucleus. The heavy elements are created by either a slow neutron capture process (the so-called s-process) or the rapid, or r-process. The s
process occurs in thermally pulsing stars (called AGB, or asymptotic
giant branch stars) and takes hundreds to thousands of years to reach
the heaviest elements of lead and bismuth. The r-process is thought to occur in supernova explosions
which provide the necessary conditions of high temperature, high
neutron flux and ejected matter. These stellar conditions make the
successive neutron captures very fast, involving very neutron-rich
species which then beta-decay to heavier elements, especially at the
so-called waiting points that correspond to more stable nuclides with
closed neutron shells (magic numbers).
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