The Astronomical Universe
The present conception of the universe is
that of a vast complex system whose boundaries are unknown. To grasp
the immensity of the universe, one must appreciate the magnitude of
the units used to measure it. The most common unit is the light-year,
which is the distance that light, which travels at about 186,300 miles
(300,000 km) per second, travels in one year; one light-year is equal
to 5.88 trillion miles (9.46 trillion km). Another common unit of
astronomical measurement is the parsec, which is equal to 19.2 trillion
miles (30.8 trillion km), or 3.26 light-years. The nearest star to
the solar system, Proxima Centauri, is about 4.3 light-years (25
trillion miles; 41 trillion km) away. The most distant object yet
observed is a quasar that has been estimated to be about 18 billion
light-years (106,000 billion billion miles; 170,000 billion billion
km) from the earth. However, this is only the distance that the
largest optical telescopes allow man to see.
Like the size, the age and method of
formation of the universe are unknown. The age is estimated to be
between 10 billion and 20 billion years. Two models of the universe
vied for acceptance in the period after World War II. One, put forth
by Georges Lemaître in 1931, deals with an evolutionary universe that
originated in a primordial explosion called the big bang. The other,
introduced by Hermann Bondi and Thomas Gold in 1948, postulates a
steady-state universe in which matter is constantly being created.
Observational evidence obtained since the late 1960's has provided
strong support for the evolutionary, or big bang, model.
(See also Cosmology, Astronomical)
Astronomical studies of the universe can be
divided into four broad categories. These are the solar system, which
deals with the earth and its nearest neighbors in space, the sun, moon,
and planets; stars; interstellar matter; and galaxies. (See also
Interstellar Matter; Galaxies)
The Solar System
The solar system comprises the sun and the
numerous smaller bodies that revolve around it. These include the 9
principal planets and their natural satellites, or moons, of which
about 50 are known; the thousands of minor planets, or asteroids; the
comets; and the meteor swarms. The principal planets in order of
increasing distance from the sun are Mercury, Venus, the earth, Mars,
Jupiter, Saturn, Uranus, Neptune, and Pluto. The first two are called
inferior planets because they revolve inside the earth's orbit, and
the last six are called superior planets because they revolve outside
it. The inferior planets and the first three superior planets were
called wandering stars by the ancients since they were seen to move
against the background of fixed stars. (See also Solar System)
Motions of the planets reveal to the expert
in celestial mechanics the physical interrelationships in the solar
system, and offer subtle evidence bearing upon basic concepts such as
the theory of relativity. Skill in celestial mechanics is a key to
success in earth-satellite and space-rocket projects, where the
slightest miscalculations can result in expensive, discouraging
failure. Astrophysical studies of the planets yield data on their
dimensions, composition of their atmospheres, surface features
(especially as to Mars), possible presence of life, and future use of
planets and their satellites as space stations. (See also
Celestial Mechanics; Orbit)
Specialists in solar astronomy investigate
physical processes occurring in and near the sun, including
thermonuclear reactions and other high-temperature phenomena. Sunspots
and solar radiation, with their influences on the earth's weather,
climate, and inhabitants, are also studied. By intensive study of the
sun, the astrophysicist learns much about points of light in the
largest telescopes. (See also International Years of the Quiet Sun (IQSY); Sun)
Lunar astronomy was revolutionized in the
space age. Photographs of the moon's far side, which had never before
been viewed, were returned to the earth by the Soviet lunar probe
Lunik 3 in 1959, and close-up pictures with a resolution far superior
to that possible in photographs taken from the earth were returned by
U.S. probes of the Ranger series in 1964 and 1965. Experiments
performed by the unmanned Surveyor 5, 6, and 7 spacecraft, which
soft-landed on the moon in 1967 and 1968, first made possible an
estimate of the moon's chemical composition. Lunar rock and dust
samples brought back to earth by the U.S. manned Apollo landing
missions (1969-1972) and the Soviet robotic Luna landing missions
(1970-1976) made possible determinations of the moon's age, detailed
chemistry, and physical characteristics. The Apollo and Luna moon rocks
are still being studied by geologists and mineralogists. The moon,
with its craters, maria ("seas"), and mountain chains, is a
little-changed relic of the early days in the solar system, and clues
obtained as to its origin may well be clues to the origin of the solar
system itself. (See also Moon)
Meteors and meteorites, too, yield clues to
the origin and history of the solar system, because meteorites,
uranium-dated at about 4.5 billion years, may have changed little
since the system was born. Meteors and their occurrence are also of
obvious interest in the study of probable hazards to space travel.
Comets are related to meteors. They, too, are remnants of the early
days of the solar system and are studied for clues to the past.
(See also Comet; Meteor; Meteorite)
Stars
Along with the earth, moon, and sun, the
stars are the most familiar celestial objects. The ancients thought
of the stars as fixed in place, since they did not appear to move in
relation to one another, and mentally arranged them into groups to
form outlines of mythological animals and men, dippers, crosses, and
other patterns. They also believed that all the stars were at the
same distance from the earth and imbedded on the inner surface of a
sphere that rotated around it. (See also Celestial Sphere; Constellation)
Modern astronomy recognizes stars as being
fiery gaseous bodies like the sun, which is really a star of less than
average size and temperature. Like the sun, the stars shine all the
time, but they cannot be seen during the day because their light is
overpowered by that from the sun. Stars vary in their distances from
the earth, in their relative motions, and in color, volume, shape,
mass, temperature, luminosity, density, and chemical composition.
Because they are at such great distances from the earth, stars provide
a valuable reference background for study of the motions of members
of the solar system, and thus become a means by which to tell time. In
studies of the makeup of our galaxy, distances of stars are measured.
Distances of nearer stars are measured by triangulation; distances of
more remote stars can be inferred from the ratio of intrinsic
brightness (as indicated by the type of the star's spectrum) to
apparent brightness, since the latter decreases according to the
distance traveled by the starlight. Many studies center on stars
(totalling perhaps half of all stars), called binary systems, that have
been found to consist of two or more components. Doppler shifts in
stellar spectra are observed for clues as to stellar motions (usually
of the order of miles per second) and thus to past and present events
in the galaxy. The movements of star clusters and of their individual
members are plotted. Stars are spectroscopically analyzed and
classified as to their chemical composition and probable stage of
evolution. Evidence that the companion of Barnard's star, named after
its discoverer, Edward Emerson Barnard, may be a planet rather than a
second star points up the possible existence of numerous other "solar
systems," some of which could perhaps be inhabited by intelligent life.
The vicinities of certain nearby stars have been monitored by radio
telescopes, thus far unsuccessfully, for possible signals from
intelligent beings who may inhabit planets associated with these
stars. (See also Interstellar Communication)
Like our own sun, all stars are centers of
stupendous physical happenings impossible as yet to reproduce on the
earth. They represent billions of individual case histories, and each
appears as it existed at some moment in the past -- as many years ago
as it is light-years distant from the earth. Astronomy, from the
viewpoint of an instant in time, beholds a panorama of cosmic change
spanning millions and even billions of years. (See also
Cosmology, Astronomical; Star)
Interstellar Matter
Shrouding the stars and scattered through
interstellar space are cosmic gas and dust. This material is here and
there concentrated into the so-called diffuse nebulas, in some of
which -- as astronomers believe of the glowing region in Orion's sword
-- stars are now forming. These gigantic clouds, some dark, some
reflecting starlight, and others luminous like giant flourescent
bulbs, partly hiding the star-studded spiral arms of our Milky Way
galaxy, are frequent targets for the radio telescope and the
time-exposure camera. Radio noise from the interstellar clouds and
from objects behind them is a clue to events never suspected by the
observer at the optical telescope. It is the radio telescope that has
made possible, in recent years, the mapping of the major features of
the Milky Way galaxy. (See also Interstellar Matter; Milky Way; Nebula; Nova)
Galaxies
Beyond the Milky Way, at distances ranging
out to 6 billion light-years and beyond, are the uncountable billions
of other galaxies. Individual stars of certain nearer galaxies, those
that are not more than a few million light-years distant, can be
distinguished through large telescopes. The astrophysicist analyzes
the starlight and invisible radiation from these other systems,
finding them remarkably similar to our own, though they occur in a
vast range of sizes, shapes, and apparent stages of development. The
redshift in their spectra indicates that they are racing away from the
solar system at greater and greater speeds as their distances from it
increase. (See also Galaxies)
The discovery of exploding galaxies has
indicated that magnetic fields exist in interstellar and even
intergalactic space and that high-energy particles move through these
fields. The implications of these discoveries in the studies of cosmic
radiation and galactic evolution are of extreme importance. (See also
Cosmic Rays)
The use of radio telescopes has done more
than extend the boundaries of the known universe. They have yielded
valuable information concerning the tenuous hydrogen gas found in
interstellar and intergalactic space and the spatial distribution of
galaxies. Perhaps of even greater importance was the use of the radio
telescope to identify the mysterious quasars. Quasars, a contraction
for quasi-stellar radio sources, are far too bright to be stars and
far too small to be galaxies. Their enormous energy output cannot be
explained by any known mechanism. It is thought by many that the
explanation of the quasar's energy mechanism may also be the key to
the mechanism of the formation of the universe. (See also
Quasar)