Dark Matter
Dark Matter
Dark matter is a still unidentified
substance that makes up about 23 percent of the universe. It is thought to
surround most galaxies, affecting their shapes by its gravity. Ordinarily it
cannot be seen. This composite picture of galaxy cluster 1E 0657-556 was
created from images taken by different space telescopes in X-ray and visible
light. The cluster is actually two giant groups of galaxies that collided
head-on. The dark matter around the groups of galaxies is indicated by the blue
regions, which bend the light from more distant galaxies in the background. The
pink regions are hot gas stripped away in the collision.
Dark Matter, in astronomy, designation
for matter that does not give off or reflect detectable electromagnetic
radiation, the radiant energy that includes visible light, radio waves,
infrared radiation, X rays, and gamma rays. Although dark matter is practically
invisible, astrophysicists have determined its existence by detecting its
gravitational interaction with matter that does give off detectable
electromagnetic radiation, such as stars, galaxies, and clusters of galaxies.
Dark matter has become a vital component of modern theories of cosmology and
elementary particle physics. Along with the phenomenon of dark energy, the
puzzle of what dark matter is represents one of the most important questions in
physics today.
II
|
THE DISCOVERY OF DARK MATTER
|
The existence of dark
matter was first suggested in the early 20th century by the Swiss American
astronomer Fritz Zwicky, but convincing and overwhelming evidence of its
existence was gathered by the American astronomer Vera Rubin in the 1970s. In
the early 1930s, Zwicky studied the rotational motions of thousands of galaxies
clustered together in a large group of galaxies known as the Coma Cluster. He
found that the orbital motion of the galaxies around their common center of
mass could only be explained by the presence of unseen matter, which astronomers
now call dark matter. Zwicky’s suggestion was not taken very seriously at first
because there was not a great amount of evidence to support such a radical
suggestion.
In the early 1970s, however,
Rubin studied the orbital motions of stars in a large number of galaxies. As
these stars orbited their galactic centers, Rubin noticed that the outlying
stars in the galaxies were moving so fast that they should have been flung out
of the galaxies. But since they were still part of the galaxies, Rubin proposed
that unseen matter was keeping them gravitationally bound to the galaxies. A
similar observation was reported in the early 1930s for the stars in our own
Milky Way Galaxy by Dutch astronomer Jan Oort, but the dark matter
interpretation was not considered at that time.
Following up on the observational
data gathered by Oort, Zwicky, Rubin, and other astronomers, two American
theoretical astrophysicists, Jeremiah P. Ostriker and P. J. E. Peebles,
contributed important theoretical analyses. The data and the analyses helped
scientists determine that dark matter probably constitutes as much as 90
percent of all the matter in the universe. Scientists verified that the orbital
motions of stars in galaxies cannot be explained by the mutual gravitational influence
of all the other visible stars. To explain this orbital motion, dark matter
must be present. Rubin and other astronomers and astrophysicists showed that
this dark matter seems to be distributed in a large envelope or “halo” around
the visible matter of the galaxy. As a result the galaxies are much larger than
what can actually be observed through a telescope.
Some scientists have theorized
that there may be other explanations for the orbital motions of stars besides
dark matter, such as a new type of force in nature that exerts itself over vast
distances or a modification of the law of gravity. But so far, neither a new
force nor a new understanding of gravity has been found. The hypothetical
existence of dark matter, however, does explain the observed interactions with
ordinary matter extremely well without resorting to a new long-range force.
III
|
WHAT IS DARK MATTER?
|
To gain a fuller understanding
of our universe, it is vital to determine exactly what dark matter is made of. Scientists
think that dark matter occurs in several different forms. Moreover,
observations and experiments place limits on the quantity and distribution of
each type. There are two broad categories of dark matter: “hot” dark matter,
which moves at speeds comparable to the speed of light (about 299,000 km per
second or 186,000 mi per second), and “cold” dark matter, which moves at speeds
well below that of light.
A
|
Hot Dark Matter
|
The elementary particle called
the neutrino, discovered in 1956, is an example of a hot dark matter candidate.
Various experiments and observations, such as those reported in 1998 by the
Super-Kamiokande experiment in Japan, have shown that the neutrino has mass.
Mass is the quality that causes gravitational attraction. The mass of the
neutrino is extremely small, which is why the particle travels at speeds
comparable to that of light. Neutrinos are extremely abundant in the universe
because they are produced in enormous numbers in nuclear interactions that take
place at the core of every star. For example, several trillion neutrinos pass
through each person on Earth each second as a result of the nuclear reactions
that cause the Sun to shine. Because neutrinos are electrically neutral they can
pass easily through ordinary matter, such as through people, and so are able to
spread throughout a region near ordinary matter. Their large numbers could
enable them to be a significant component of dark matter despite the tiny
amount of mass in an individual neutrino.
However, there is evidence
that dark matter cannot be made up mostly of neutrinos. This is due to two
reasons. First, their likely mass is still too small to provide enough matter
to account for the gravitational effects seen in the orbital motions of stars.
In addition, some form of dark matter was necessary in the early universe to
create the early structures that eventually led to the formation of stars and
galaxies. Neutrinos could not have played this role, in part because they could
not have been created in the required quantities until stars actually formed.
Secondly, neutrinos are too
energetic to have helped seed the process of star and galaxy formation. Some
other form of dark matter must have contributed to star and galaxy formation,
which developed from localized structures, or lumps, known as anisotropies.
These lumps have been detected in the cosmic microwave background radiation,
the radiation left over from the formation of the universe in the big bang
about 13.7 billion years ago.
Detailed observations of the cosmic
background radiation show that these localized lumps in the early universe were
too small to be seeded by fast-moving particles such as neutrinos. For the
anisotropies to have formed in the early universe, a large component of slower,
cold dark matter must have been present.
B
|
Cold Dark Matter
|
Another candidate for the dark
matter is known as baryonic cold dark matter. Baryonic cold dark matter is made
of protons and neutrons, the subatomic particles known as baryons that make up
ordinary matter and combine with electrons to form atoms. Baryonic cold dark
matter could be found in celestial objects that were not massive enough to
initiate the fusion processes that make stars shine. It could also be made of
matter that collapsed to form dense objects such as neutron stars or even black
holes (objects so dense that not even light can escape their gravitational
field). Such objects are collectively referred to as “MACHOs,” which means
“massive compact halo objects.”
Astronomical observations limit the
amount of MACHOs that could exist. For example, if they were numerous, such
objects would inevitably pass close to the line of sight between an observer on
Earth and a distant visible object. Albert Einstein’s theory of gravity, known
as the theory of general relativity, describes how light is bent by the
presence of mass and energy. Mass and energy set up a gravitational field
through which light passes. The MACHO object’s gravitational field would
therefore bend the light of a more distant visible object and produce a
distortion of its image. Such a process is called a gravitational lens. Several
such gravitational lenses have been observed, and the measured frequency of such
events has placed limits on how much dark matter can take the form of MACHOs.
From the observations that have been made by astronomers, it is now known that
MACHOs cannot be the dominant constituent of dark matter. There are simply not
enough such gravitational lenses.
Physicists suspect that a more
exotic form of cold dark matter must exist. This form is not baryonic. Like
neutrinos, this form barely interacts with ordinary matter, but is some type of
massive particle. Such candidates are often called WIMPs (for “weakly
interacting massive particles”).
Various theories of the
fundamental elementary particles and their interactions in nature predict the
existence of new particles that have not yet been discovered. These
hypothetical particles are excellent candidates for WIMPs. For example,
supersymmetric theories propose that a new fundamental symmetry of nature was
present when the universe was very young and energetic. If this symmetry
existed in the past, it requires the hypothetical particles to exist. The
symmetry would have disappeared as a result of natural dynamical effects as the
universe aged and became less energetic. See also Theory of Everything;
Unified Field Theory.
As a result we do not
observe this symmetry today. The loss of symmetry over time is very similar to
what happens as water freezes and turns to ice as it is cooled. Water is more
symmetrical than ice since its molecules point in all directions in space,
whereas ice forms a crystal lattice with the molecules pointing in the preferred
directions of the lattice. As the universe expands, it also cools, and this can
give rise to the disappearance of important symmetries in later epochs.
IV
|
FUTURE EXPERIMENTS
|
The supersymmetric theories
predict that relics of the earlier, more symmetric phase of the universe exist
and that they exist in the form of a very specific family of massive particles.
New experiments, such as those planned for the Large Hadron Collider (LHC), a
particle accelerator at the European Organization for Nuclear Research (CERN)
in Switzerland, are expected to be able to test some of these theories. The
experiments will try to create the predicted particles directly, using the
energetic collisions produced in the LHC. If the particles are discovered, the
LHC and other proposed experiments will systematically study their properties
to determine if they are indeed the sought-after principal components of dark
matter. This type of dark matter would be the key agent of structure formation
that gave rise to the galaxies and clusters of galaxies that constitute our
home in the universe.
In 2006 astronomers announced
what may be the first direct evidence for dark matter in the cosmos, based on
observations from the Chandra X-Ray Observatory telescope, the Hubble Space
Telescope (HST), and advanced telescopes on Earth. A collision between two
clusters of galaxies over 4 billion light-years away apparently caused visible
matter and dark matter to separate on a gigantic scale. Huge gas clouds between
and around the galaxies in each group smashed together as the two clusters
raced past each other, heating the gas to a plasma state and dragging it away
from the dark matter halos thought to surround the galaxies. The massive
presence of dark matter was detected by gravitational lensing that bent the
light from more-distant background galaxies in the telescopes’ line of sight.
The findings appear to support theories that dark matter exists and that
gravity behaves the same in giant clusters of galaxies as it does on Earth.
In early 2007 an international
team of astronomers published the results of the first search for dark matter
in a wide region of the sky using high-resolution images from the HST. Findings
from the Cosmic Evolution Survey (COSMOS) conducted with the HST were used to
create a three-dimensional map that shows the distribution of dark matter
through periods of time as far back as 6.5 billion years ago, almost halfway to
the big bang. The scientists studied the shapes of half a million galaxies to
find distortions in their apparent shapes caused by gravitational lensing
around large concentrations of mass lying between very distant galaxies and
Earth. Such concentrations of mass indicate the presence of dark matter. The
new map reveals how areas of dark matter provided the scaffolding for clusters
of galaxies made of visible matter. The galaxies accumulated in the densest
regions of dark matter as gravity gradually drew the dark matter into more
compact filaments that form a massive networklike structure.
No comments:
Post a Comment