Big Bang
Theory
Big Bang Theory, currently accepted explanation
of the beginning of the universe. The big bang theory proposes that the
universe was once extremely compact, dense, and hot. Some original event, a
cosmic explosion called the big bang, occurred about 13.7 billion years ago,
and the universe has since been expanding and cooling.
The theory is based on
the mathematical equations, known as the field equations, of the general
theory of relativity set forth in 1915 by Albert Einstein. In 1922 Russian
physicist Alexander Friedmann provided a set of solutions to the field equations.
These solutions have served as the framework for much of the current
theoretical work on the big bang theory. American astronomer Edwin Hubble
provided some of the greatest supporting evidence for the theory with his 1929
discovery that the light of distant galaxies was universally shifted toward the
red end of the spectrum (see Redshift). Once “tired light” theories—that
light slowly loses energy naturally, becoming more red over time—were
dismissed, this shift proved that the galaxies were moving away from each
other. Hubble found that galaxies farther away were moving away proportionally
faster, showing that the universe is expanding uniformly. However, the
universe’s initial state was still unknown.
In the 1940s Russian-American
physicist George Gamow worked out a theory that fit with Friedmann’s solutions
in which the universe expanded from a hot, dense state. In 1950 British
astronomer Fred Hoyle, in support of his own opposing steady-state theory,
referred to Gamow’s theory as a mere “big bang,” but the name stuck. Indeed, a
contest in the 1990s by Sky & Telescope magazine to find a better
(perhaps more dignified) name did not produce one.
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HISTORY
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The overall framework of the big
bang theory came out of solutions to Einstein’s general relativity field
equations and remains unchanged, but various details of the theory are still
being modified today. Einstein himself initially believed that the universe was
static. When his equations seemed to imply that the universe was expanding or
contracting, Einstein added a constant term to cancel out the expansion or
contraction of the universe. When the expansion of the universe was later
discovered, Einstein stated that introducing this “cosmological constant” had
been a mistake.
After Einstein’s work of 1917,
several scientists, including the abbé Georges Lemaître in Belgium, Willem de
Sitter in Holland, and Alexander Friedmann in Russia, succeeded in finding
solutions to Einstein’s field equations. The universes described by the
different solutions varied. De Sitter’s model had no matter in it. This model
is actually not a bad approximation since the average density of the universe
is extremely low. Lemaître’s universe expanded from a “primeval atom.” Friedmann’s
universe also expanded from a very dense clump of matter, but did not involve
the cosmological constant. These models explained how the universe behaved
shortly after its creation, but there was still no satisfactory explanation for
the beginning of the universe.
In the 1940s George Gamow
was joined by his students Ralph Alpher and Robert Herman in working out
details of Friedmann’s solutions to Einstein’s theory. They expanded on Gamow’s
idea that the universe expanded from a primordial state of matter called ylem
consisting of protons, neutrons, and electrons in a sea of radiation. They
theorized the universe was very hot at the time of the big bang (the point at
which the universe explosively expanded from its primordial state), since
elements heavier than hydrogen can be formed only at a high temperature. Alpher
and Hermann predicted that radiation from the big bang should still exist.
Cosmic background radiation roughly corresponding to the temperature predicted
by Gamow’s team was detected in the 1960s, further supporting the big bang
theory, though the work of Alpher, Herman, and Gamow had been forgotten.
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THE THEORY
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The big bang theory seeks
to explain what happened at or soon after the beginning of the universe.
Scientists can now model the universe back to 10-43 seconds after
the big bang. For the time before that moment, the classical theory of gravity
is no longer adequate. Scientists are searching for a theory that merges
gravity (as explained by Einstein's general theory of relativity) and quantum
mechanics but have not found one yet. Many scientists have hope that string
theory, also known as M-theory, will tie together gravity and quantum
mechanics and help scientists explore further back in time (see Physics:
Unified Field Theory).
Because scientists cannot look
back in time beyond that early epoch, the actual big bang is hidden from them.
There is no way at present to detect the origin of the universe. Further, the
big bang theory does not explain what existed before the big bang. It may be
that time itself began at the big bang, so that it makes no sense to discuss
what happened “before” the big bang.
According to the big bang
theory, the universe expanded rapidly in its first microseconds. A single force
existed at the beginning of the universe, and as the universe expanded and
cooled, this force separated into those we know today: gravity,
electromagnetism, the strong nuclear force, and the weak nuclear force. A
theory called the electroweak theory now provides a unified explanation of
electromagnetism and the weak nuclear force theory (see Unified Field
Theory). Physicists are now searching for a grand unification theory to also
incorporate the strong nuclear force. String theory seeks to incorporate the
force of gravity with the other three forces, providing a theory of everything
(TOE).
One widely accepted version
of big bang theory includes the idea of inflation. In this model, the
universe expanded much more rapidly at first, to about 1050 times
its original size in the first 10-32 second, then slowed its
expansion. The theory was advanced in the 1980s by American cosmologist Alan
Guth and elaborated upon by American astronomer Paul Steinhardt, Russian
American scientist Andrei Linde, and British astronomer Andreas Albrecht. The
inflationary universe theory (see Inflationary Theory) solves a number
of problems of cosmology. For example, it shows that the universe now appears
close to the type of flat space described by the laws of Euclid’s geometry: We
see only a tiny region of the original universe, similar to the way we do not
notice the curvature of the earth because we see only a small part of it. The
inflationary universe also shows why the universe appears so homogeneous. If
the universe we observe was inflated from some small, original region, it is
not surprising that it appears uniform.
Once the expansion of the
initial inflationary era ended, the universe continued to expand more slowly.
The inflationary model predicts that the universe is on the boundary between
being open and closed. If the universe is open, it will keep expanding forever.
If the universe is closed, the expansion of the universe will eventually stop
and the universe will begin contracting until it collapses. Whether the
universe is open or closed depends on the density, or concentration of mass, in
the universe. If the universe is dense enough, it is closed.
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SUPPORTING EVIDENCE
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The universe cooled as it expanded.
After about one second, protons formed. In the following few minutes—often
referred to as the “first three minutes”—combinations of protons and neutrons
formed the isotope of hydrogen known as deuterium as well as some of the other
light elements, principally helium, as well as some lithium, beryllium, and
boron. The study of the distribution of deuterium, helium, and the other light
elements is now a major field of research. The uniformity of the helium
abundance around the universe supports the big bang theory and the abundance of
deuterium can be used to estimate the density of matter in the universe.
From about 380,000 to about
1 million years after the big bang, the universe cooled to about 3000°C (about
5000°F) and protons and electrons combined to make hydrogen atoms. Hydrogen
atoms can only absorb and emit specific colors, or wavelengths, of light. The
formation of atoms allowed many other wavelengths of light, wavelengths that
had been interfering with the free electrons prior to the cooling of the
universe, to travel much farther than before. This change set free radiation
that we can detect today. After billions of years of cooling, this cosmic
background radiation is at about 3 K (-270°C/-454°F).The cosmic background
radiation was first detected and identified in 1965 by American astrophysicists
Arno Penzias and Robert Wilson.
The Cosmic Background Explorer
(COBE) spacecraft, a project of the National Aeronautics and Space
Administration (NASA), mapped the cosmic background radiation between 1989 and
1993. It verified that the distribution of intensity of the background
radiation precisely matched that of matter that emits radiation because of its
temperature, as predicted for the big bang theory. It also showed that cosmic
background radiation is not uniform, that it varies slightly. These variations
are thought to be the seeds from which galaxies and other structures in the
universe grew.
Evidence indicates that the
matter that scientists detect in the universe is only a small fraction of all
the matter that exists. For example, observations of the speeds at which
individual galaxies move within clusters of galaxies show that a great deal of
unseen matter must exist to exert sufficient gravitational force to keep the
clusters from flying apart. Cosmologists now think that much of the universe is
dark matter—matter that has gravity but does not give off radiation that we can
see or otherwise detect. One kind of dark matter theorized by scientists is cold
dark matter, with slowly moving (cold) massive particles. No such particles
have yet been detected, though astronomers have made up fanciful names for
them, such as Weakly Interacting Massive Particles (WIMPs). Other cold dark
matter could be nonradiating stars or planets, which are known as MACHOs
(Massive Compact Halo Objects).
An alternative theory that
explains the dark-matter model involves hot dark matter, where hot
implies that the particles are moving very fast. Neutrinos, fundamental
particles that travel at nearly the speed of light, are the prime example of
hot dark matter. However, scientists think that the mass of a neutrino is so
low that neutrinos can only account for a small portion of dark matter. If the
inflationary version of big bang theory is correct, then the amount of dark
matter and of whatever else might exist is just enough to bring the universe to
the boundary between open and closed.
Scientists develop theoretical
models to show how the universe’s structures, such as clusters of galaxies,
have formed. Their models invoke hot dark matter, cold dark matter, or a
mixture of the two. This unseen matter would have provided the gravitational
force needed to bring large structures such as clusters of galaxies together.
The theories that include dark matter match the observations, although there is
no consensus on the type or types of dark matter that must be included.
Supercomputers are important for making such models.
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REFINING THE THEORY
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Astronomers continue to make new
observations that are also interpreted within the framework of the big bang
theory. No major problems with the big bang theory have been found, but
scientists constantly adjust the theory to match the observed universe. In particular,
a “standard model” of the big bang has been established by results from NASA's
Wilkinson Microwave Anisotropy Probe (WMAP), launched in 2001 (see Cosmology).
The probe studied the anisotropies, or ripples, in the temperature of cosmic
background radiation at a higher resolution than COBE was capable of. These
ripples indicate that regions of the young universe were very slightly hotter
or cooler, by a factor of about 1/1000, than adjacent regions. WMAP’s
observations suggest that the rate of expansion of the universe, called
Hubble’s constant, is about 71 km/s/Mpc (kilometers per second per million
parsecs, where a parsec is about 3.26 light-years). In other words, the
distance between any two objects in space that are separated by a million parsecs
increases by about 71 km every second in addition to any other motion they may
have relative to one another. In combination with previously existing
observations, this rate of expansion tells cosmologists that the universe is
“flat,” though flatness here does not refer to the actual shape of the universe
but rather that the geometric laws that apply to the universe match those of a
flat plane.
To be flat, the universe
must contain a certain amount of matter and energy, known as the critical
density. The distribution of sizes of ripples detected by WMAP show that
ordinary matter—like that making up objects and living things on Earth—accounts
for only 4.4 percent of the critical density. Dark matter makes up an
additional 23 percent. Astoundingly, the remaining 73 percent of the universe
is composed of something else—a substance so mysterious that nobody knows much
about it. Called “dark energy,” this substance provides the antigravity-like
negative pressure that causes the universe's expansion to accelerate rather
than slow down. This “accelerating universe” was detected independently by two
competing groups of astronomers in the last years of the 20th century. The
ideas of an accelerating universe and the existence of dark energy have caused
astronomers to substantially modify previous ideas of the big bang universe.
WMAP's results also show
that cosmic background radiation was set free about 389,000 years after the big
bang, later than was previously thought, and that the first stars formed about
200 million years after the big bang, earlier than anticipated. Further refinements
to the big bang theory are expected from WMAP, which continues to collect data.
An even more precise mission to study the beginnings of the universe, the
European Space Agency’s Planck spacecraft, is scheduled to be launched in 2007.
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