Astronomy (from "Greek: ἀστρονομία) is a "natural science that studies "celestial objects and phenomena. It applies "mathematics, "physics, and "chemistry, in an effort to explain the origin of those objects and phenomena and their "evolution. Objects of interest include "planets, "moons, "stars, "galaxies, and "comets; while the phenomena include "supernova explosions, "gamma ray bursts, and "cosmic microwave background radiation. More generally, all astronomical phenomena that originate outside "Earth's atmosphere are within the purview of astronomy. A related but distinct subject, "physical cosmology, is concerned with the study of the "Universe as a whole.
Astronomy is one of the oldest of the natural sciences. The early civilizations in "recorded history, such as the "Babylonians, "Greeks, "Indians, "Egyptians, "Nubians, "Iranians, "Chinese, and "Maya performed methodical observations of the "night sky. Historically, astronomy has included disciplines as diverse as "astrometry, "celestial navigation, "observational astronomy and the making of "calendars, but professional astronomy is now often considered to be synonymous with "astrophysics.
During the 20th century, the field of professional astronomy split into "observational and "theoretical branches. Observational astronomy is focused on acquiring data from observations of astronomical objects, which is then analyzed using basic principles of physics. Theoretical astronomy is oriented toward the development of computer or analytical models to describe astronomical objects and phenomena. The two fields complement each other, with theoretical astronomy seeking to explain observational results and observations being used to confirm theoretical results.
Astronomy is one of the few sciences where amateurs still play an active role, especially in the discovery and observation of transient "phenomena. "Amateur astronomers have made and contributed to many important astronomical discoveries, such as finding new comets.
Astronomy (from the "Greek ἀστρονομία from ἄστρον astron, "star" and -νομία -nomia from νόμος nomos, "law" or "culture") means "law of the stars" (or "culture of the stars" depending on the translation). Astronomy should not be confused with "astrology, the belief system which claims that human affairs are correlated with the positions of celestial objects. Although the "two fields share a common origin, they are now entirely distinct.
Generally, either the term "astronomy" or "astrophysics" may be used to refer to this subject. Based on strict dictionary definitions, "astronomy" refers to "the study of objects and matter outside the Earth's atmosphere and of their physical and chemical properties" and "astrophysics" refers to the branch of astronomy dealing with "the behavior, physical properties, and dynamic processes of celestial objects and phenomena". In some cases, as in the introduction of the introductory textbook The Physical Universe by "Frank Shu, "astronomy" may be used to describe the qualitative study of the subject, whereas "astrophysics" is used to describe the physics-oriented version of the subject. However, since most modern astronomical research deals with subjects related to physics, modern astronomy could actually be called astrophysics. Few fields, such as astrometry, are purely astronomy rather than also astrophysics. Various departments in which scientists carry out research on this subject may use "astronomy" and "astrophysics," partly depending on whether the department is historically affiliated with a physics department, and many professional "astronomers have physics rather than astronomy degrees. Some titles of the leading scientific journals in this field include "The Astronomical Journal, "The Astrophysical Journal and "Astronomy and Astrophysics.
In early times, astronomy only comprised the observation and predictions of the motions of objects visible to the naked eye. In some locations, early cultures assembled massive artifacts that possibly had some astronomical purpose. In addition to their ceremonial uses, these "observatories could be employed to determine the seasons, an important factor in knowing when to plant crops, as well as in understanding the length of the year.
Before tools such as the telescope were invented, early study of the stars was conducted using the naked eye. As civilizations developed, most notably in "Mesopotamia, "Greece, "Persia, "India, "China, "Egypt, and "Central America, astronomical observatories were assembled, and ideas on the nature of the Universe began to be explored. Most of early astronomy actually consisted of mapping the positions of the stars and planets, a science now referred to as "astrometry. From these observations, early ideas about the motions of the planets were formed, and the nature of the Sun, Moon and the Earth in the Universe were explored philosophically. The Earth was believed to be the center of the Universe with the Sun, the Moon and the stars rotating around it. This is known as the "geocentric model of the Universe, or the "Ptolemaic system, named after "Ptolemy.
A particularly important early development was the beginning of mathematical and scientific astronomy, which began among "the Babylonians, who laid the foundations for the later astronomical traditions that developed in many other civilizations. The "Babylonians discovered that "lunar eclipses recurred in a repeating cycle known as a "saros.
Following the Babylonians, significant advances in astronomy were made in "ancient Greece and the "Hellenistic world. "Greek astronomy is characterized from the start by seeking a rational, physical explanation for celestial phenomena. In the 3rd century BC, "Aristarchus of Samos estimated the "size and distance of the Moon and Sun, and was the first to propose a "heliocentric model of the "solar system. In the 2nd century BC, "Hipparchus discovered "precession, calculated the size and distance of the Moon and invented the earliest known astronomical devices such as the "astrolabe. Hipparchus also created a comprehensive catalog of 1020 stars, and most of the "constellations of the northern hemisphere derive from Greek astronomy. The "Antikythera mechanism (c. 150–80 BC) was an early "analog computer designed to calculate the location of the "Sun, "Moon, and "planets for a given date. Technological artifacts of similar complexity did not reappear until the 14th century, when mechanical "astronomical clocks appeared in "Europe.
During the Middle Ages, astronomy was mostly stagnant in "medieval Europe, at least until the 13th century. However, "astronomy flourished in the Islamic world and other parts of the world. This led to the emergence of the first astronomical "observatories in the "Muslim world by the early 9th century. In 964, the "Andromeda Galaxy, the largest "galaxy in the "Local Group, was discovered by the Persian astronomer "Azophi and first described in his "Book of Fixed Stars. The "SN 1006 "supernova, the brightest "apparent magnitude stellar event in recorded history, was observed by the Egyptian Arabic astronomer "Ali ibn Ridwan and the "Chinese astronomers in 1006. Some of the prominent Islamic (mostly Persian and Arab) astronomers who made significant contributions to the science include "Al-Battani, "Thebit, "Azophi, "Albumasar, "Biruni, "Arzachel, "Al-Birjandi, and the astronomers of the "Maragheh and "Samarkand observatories. Astronomers during that time introduced many "Arabic names now used for individual stars. It is also believed that the ruins at "Great Zimbabwe and "Timbuktu may have housed an astronomical observatory. Europeans had previously believed that there had been no astronomical observation in pre-colonial Middle Ages "sub-Saharan Africa but modern discoveries show otherwise.
The Roman Catholic Church gave more financial and social support to the study of astronomy for over six centuries, from the recovery of ancient learning during the late Middle Ages into the Enlightenment, than any other, and, probably, all other, institutions. Among the Church's motives was finding the date for Easter.
During the "Renaissance, "Nicolaus Copernicus proposed a "heliocentric model of the "solar system. His work was defended, expanded upon, and corrected by "Galileo Galilei and "Johannes Kepler. Galileo used telescopes to enhance his observations.
Kepler was the first to devise a system that described correctly the details of the motion of the planets with the Sun at the center. However, Kepler did not succeed in formulating a theory behind the laws he wrote down. It was left to "Newton's invention of "celestial dynamics and his "law of gravitation to finally explain the motions of the planets. Newton also developed the "reflecting telescope.
The English astronomer "John Flamsteed catalogued over 3000 stars. Further discoveries paralleled the improvements in the size and quality of the telescope. More extensive star catalogues were produced by "Lacaille. The astronomer "William Herschel made a detailed catalog of nebulosity and clusters, and in 1781 discovered the planet "Uranus, the first new planet found. The distance to a star was first announced in 1838 when the "parallax of "61 Cygni was measured by "Friedrich Bessel.
During the 18–19th centuries, the study of the "three body problem by "Euler, "Clairaut, and "D'Alembert led to more accurate predictions about the motions of the Moon and planets. This work was further refined by "Lagrange and "Laplace, allowing the masses of the planets and moons to be estimated from their perturbations.
Significant advances in astronomy came about with the introduction of new technology, including the "spectroscope and "photography. "Fraunhofer discovered about 600 bands in the spectrum of the Sun in 1814–15, which, in 1859, "Kirchhoff ascribed to the presence of different elements. Stars were proven to be similar to the Earth's own Sun, but with a wide range of "temperatures, "masses, and sizes.
The existence of the Earth's galaxy, the "Milky Way, as a separate group of stars, was only proved in the 20th century, along with the existence of "external" galaxies. The observed recession of those galaxies led to the discovery of the expansion of the "Universe. Theoretical astronomy led to speculations on the existence of objects such as "black holes and "neutron stars, which have been used to explain such observed phenomena as "quasars, "pulsars, "blazars, and "radio galaxies. "Physical cosmology made huge advances during the 20th century, with the model of the "Big Bang, which is heavily supported by evidence provided by "cosmic microwave background radiation, "Hubble's law, and the "cosmological abundances of elements. "Space telescopes have enabled measurements in parts of the electromagnetic spectrum normally blocked or blurred by the atmosphere. In February 2016, it was revealed that the "LIGO project had detected evidence of "gravitational waves in the previous September.
Our main source of information about "celestial bodies and other objects is visible "light more generally "electromagnetic radiation. Observational astronomy may be divided according to the observed region of the "electromagnetic spectrum. Some parts of the spectrum can be observed from the "Earth's surface, while other parts are only observable from either high altitudes or outside the Earth's atmosphere. Specific information on these subfields is given below.
Radio astronomy uses radiation outside the visible range with "wavelengths greater than approximately one millimeter. Radio astronomy is different from most other forms of observational astronomy in that the observed "radio waves can be treated as "waves rather than as discrete "photons. Hence, it is relatively easier to measure both the "amplitude and "phase of radio waves, whereas this is not as easily done at shorter wavelengths.
Although some "radio waves are emitted directly by astronomical objects, a product of "thermal emission, most of the radio emission that is observed is the result of "synchrotron radiation, which is produced when "electrons orbit "magnetic fields. Additionally, a number of "spectral lines produced by "interstellar gas, notably the "hydrogen spectral line at 21 cm, are observable at radio wavelengths.
Infrared astronomy is founded on the detection and analysis of "infrared radiation, wavelengths longer than red light and outside the range of our vision. The infrared spectrum is useful for studying objects that are too cold to radiate visible light, such as planets, "circumstellar disks or nebulae whose light is blocked by dust. The longer wavelengths of infrared can penetrate clouds of dust that block visible light, allowing the observation of young stars embedded in "molecular clouds and the cores of galaxies. Observations from the "Wide-field Infrared Survey Explorer (WISE) have been particularly effective at unveiling numerous Galactic "protostars and their host "star clusters. With the exception of infrared "wavelengths close to visible light, such radiation is heavily absorbed by the atmosphere, or masked, as the atmosphere itself produces significant infrared emission. Consequently, infrared observatories have to be located in high, dry places on Earth or in space. Some molecules radiate strongly in the infrared. This allows the study of the chemistry of space; more specifically it can detect water in comets.
Historically, optical astronomy, also called visible light astronomy, is the oldest form of astronomy. Images of observations were originally drawn by hand. In the late 19th century and most of the 20th century, images were made using photographic equipment. Modern images are made using digital detectors, particularly using "charge-coupled devices (CCDs) and recorded on modern medium. Although visible light itself extends from approximately 4000 "Å to 7000 Å (400 "nm to 700 nm), that same equipment can be used to observe some "near-ultraviolet and "near-infrared radiation.
Ultraviolet astronomy employs "ultraviolet wavelengths between approximately 100 and 3200 Å (10 to 320 nm). Light at those wavelengths are absorbed by the Earth's atmosphere, requiring observations at these wavelengths to be performed from the upper atmosphere or from space. Ultraviolet astronomy is best suited to the study of thermal radiation and spectral emission lines from hot blue "stars ("OB stars) that are very bright in this wave band. This includes the blue stars in other galaxies, which have been the targets of several ultraviolet surveys. Other objects commonly observed in ultraviolet light include "planetary nebulae, "supernova remnants, and active galactic nuclei. However, as ultraviolet light is easily absorbed by "interstellar dust, an adjustment of ultraviolet measurements is necessary.
X-ray astronomy uses "X-ray wavelengths. Typically, X-ray radiation is produced by "synchrotron emission (the result of electrons orbiting magnetic field lines), "thermal emission from thin gases above 107 (10 million) "kelvins, and "thermal emission from thick gases above 107 Kelvin. Since X-rays are absorbed by the "Earth's atmosphere, all X-ray observations must be performed from "high-altitude balloons, "rockets, or "X-ray astronomy satellites. Notable "X-ray sources include "X-ray binaries, "pulsars, "supernova remnants, "elliptical galaxies, "clusters of galaxies, and "active galactic nuclei.
Gamma ray astronomy observes astronomical objects at the shortest wavelengths of the electromagnetic spectrum. Gamma rays may be observed directly by satellites such as the "Compton Gamma Ray Observatory or by specialized telescopes called "atmospheric Cherenkov telescopes. The Cherenkov telescopes do not detect the gamma rays directly but instead detect the flashes of visible light produced when gamma rays are absorbed by the Earth's atmosphere.
Most "gamma-ray emitting sources are actually "gamma-ray bursts, objects which only produce gamma radiation for a few milliseconds to thousands of seconds before fading away. Only 10% of gamma-ray sources are non-transient sources. These steady gamma-ray emitters include pulsars, "neutron stars, and "black hole candidates such as active galactic nuclei.
In addition to electromagnetic radiation, a few other events originating from great distances may be observed from the Earth.
In "neutrino astronomy, astronomers use heavily shielded "underground facilities such as "SAGE, "GALLEX, and "Kamioka II/III for the detection of "neutrinos. The vast majority of the neutrinos streaming through the Earth originate from the "Sun, but 24 neutrinos were also detected from "supernova 1987A. "Cosmic rays, which consist of very high energy particles (atomic nuclei) that can decay or be absorbed when they enter the Earth's atmosphere, result in a cascade of secondary particles which can be detected by current observatories. Some future "neutrino detectors may also be sensitive to the particles produced when cosmic rays hit the Earth's atmosphere.
"Gravitational-wave astronomy is an emerging field of astronomy that employs "gravitational-wave detectors to collect observational data about distant massive objects. A few observatories have been constructed, such as the Laser Interferometer Gravitational Observatory "LIGO. LIGO made its "first detection on 14 September 2015, observing gravitational waves from a "binary black hole. A second "gravitational wave was detected on 26 December 2015 and additional observations should continue but "gravitational waves require extremely sensitive instruments.
One of the oldest fields in astronomy, and in all of science, is the measurement of the positions of celestial objects. Historically, accurate knowledge of the positions of the Sun, Moon, planets and stars has been essential in "celestial navigation (the use of celestial objects to guide navigation) and in the making of "calendars.
Careful measurement of the positions of the planets has led to a solid understanding of gravitational "perturbations, and an ability to determine past and future positions of the planets with great accuracy, a field known as "celestial mechanics. More recently the tracking of "near-Earth objects will allow for predictions of close encounters or potential collisions of the Earth with those objects.
The measurement of "stellar parallax of nearby stars provides a fundamental baseline in the "cosmic distance ladder that is used to measure the scale of the Universe. Parallax measurements of nearby stars provide an absolute baseline for the properties of more distant stars, as their properties can be compared. Measurements of the "radial velocity and "proper motion motion of stars allows astronomers to plot the movement of these systems through the Milky Way galaxy. Astrometric results are the basis used to calculate the distribution of speculated "dark matter in the galaxy.
Theoretical astronomers use several tools including "analytical models and "computational "numerical simulations; each has its particular advantages. Analytical models of a process are generally better for giving broader insight into the heart of what is going on. Numerical models reveal the existence of phenomena and effects otherwise unobserved.
Theorists in astronomy endeavor to create theoretical models and from the results predict observational consequences of those models. The observation of a phenomenon predicted by a model allows astronomers to select between several alternate or conflicting models as the one best able to describe the phenomena.
Theorists also try to generate or modify models to take into account new data. In the case of an inconsistency between the data and model's results, the general tendency is to try to make minimal modifications to the model so that it produces results that fit the data. In some cases, a large amount of inconsistent data over time may lead to total abandonment of a model.
Phenomena modeled by theoretical astronomers include: "stellar dynamics and "evolution; "galaxy formation; "large-scale distribution of "matter in the "Universe; origin of "cosmic rays; "general relativity and "physical cosmology, including "string "cosmology and "astroparticle physics. Astrophysical relativity serves as a tool to gauge the properties of large scale structures for which gravitation plays a significant role in physical phenomena investigated and as the basis for "black hole (astro)"physics and the study of "gravitational waves.
A few examples of this process:
|Physical process||Experimental tool||Theoretical model||Explains/predicts|
|"Gravitation||"Radio telescopes||"Self-gravitating system||Emergence of a "star system|
|"Nuclear fusion||"Spectroscopy||"Stellar evolution||How the stars shine and how "metals formed|
|"The Big Bang||"Hubble Space Telescope, "COBE||"Expanding universe||"Age of the Universe|
|"Quantum fluctuations||"Cosmic inflation||"Flatness problem|
|"Gravitational collapse||"X-ray astronomy||"General relativity||"Black holes at the center of "Andromeda galaxy|
|"CNO cycle in stars||The dominant source of energy for massive star.|
At a distance of about eight light-minutes, the most frequently studied star is the "Sun, a typical main-sequence "dwarf star of "stellar class G2 V, and about 4.6 billion years (Gyr) old. The Sun is not considered a "variable star, but it does undergo periodic changes in activity known as the "sunspot cycle. This is an 11-year oscillation in "sunspot number. Sunspots are regions of lower-than- average temperatures that are associated with intense magnetic activity.
The Sun has steadily increased in luminosity by 40% since it first became a main-sequence star. The Sun has also undergone periodic changes in luminosity that can have a significant impact on the Earth. The "Maunder minimum, for example, is believed to have caused the "Little Ice Age phenomenon during the "Middle Ages.
The visible outer surface of the Sun is called the "photosphere. Above this layer is a thin region known as the "chromosphere. This is surrounded by a transition region of rapidly increasing temperatures, and finally by the super-heated "corona.
At the center of the Sun is the core region, a volume of sufficient temperature and pressure for "nuclear fusion to occur. Above the core is the "radiation zone, where the plasma conveys the energy flux by means of radiation. Above that is the "convection zone where the gas material transports energy primarily through physical displacement of the gas known as convection. It is believed that the movement of mass within the convection zone creates the magnetic activity that generates sunspots.
A solar wind of plasma particles constantly streams outward from the Sun until, at the outermost limit of the Solar System, it reaches the "heliopause. As the solar wind passes the Earth, it interacts with the "Earth's magnetic field ("magnetosphere) and deflects the solar wind, but traps some creating the "Van Allen radiation belts that envelop the Earth . The "aurora are created when solar wind particles are guided by the magnetic flux lines into the Earth's polar regions where the lines the descend into the "atmosphere.
Planetary science is the study of the assemblage of "planets, "moons, "dwarf planets, "comets, "asteroids, and other bodies orbiting the Sun, as well as extrasolar planets. The "Solar System has been relatively well-studied, initially through telescopes and then later by spacecraft. This has provided a good overall understanding of the formation and evolution of this planetary system, although many new discoveries are still being made.
The Solar System is subdivided into the inner planets, the "asteroid belt, and the outer planets. The inner "terrestrial planets consist of "Mercury, "Venus, "Earth, and "Mars. The outer "gas giant planets are "Jupiter, "Saturn, "Uranus, and "Neptune. Beyond Neptune lies the "Kuiper Belt, and finally the "Oort Cloud, which may extend as far as a light-year.
The planets were formed 4.6 billion years ago in the "protoplanetary disk that surrounded the early Sun. Through a process that included gravitational attraction, collision, and accretion, the disk formed clumps of matter that, with time, became protoplanets. The "radiation pressure of the "solar wind then expelled most of the unaccreted matter, and only those planets with sufficient mass retained their gaseous atmosphere. The planets continued to sweep up, or eject, the remaining matter during a period of intense bombardment, evidenced by the many "impact craters on the Moon. During this period, some of the protoplanets may have collided and one such collision may have "formed the Moon.
Once a planet reaches sufficient mass, the materials of different densities segregate within, during "planetary differentiation. This process can form a stony or metallic core, surrounded by a mantle and an outer crust. The core may include solid and liquid regions, and some planetary cores generate their own "magnetic field, which can protect their atmospheres from solar wind stripping.
A planet or moon's interior heat is produced from the collisions that created the body, by the decay of radioactive materials (e.g. "uranium, "thorium, and "26Al), or "tidal heating caused by interactions with other bodies. Some planets and moons accumulate enough heat to drive geologic processes such as "volcanism and tectonics. Those that accumulate or retain an "atmosphere can also undergo surface "erosion from wind or water. Smaller bodies, without tidal heating, cool more quickly; and their geological activity ceases with the exception of impact cratering.
The study of stars and "stellar evolution is fundamental to our understanding of the Universe. The astrophysics of stars has been determined through observation and theoretical understanding; and from computer simulations of the interior. "Star formation occurs in dense regions of dust and gas, known as "giant molecular clouds. When destabilized, cloud fragments can collapse under the influence of gravity, to form a "protostar. A sufficiently dense, and hot, core region will trigger "nuclear fusion, thus creating a "main-sequence star.
The characteristics of the resulting star depend primarily upon its starting mass. The more massive the star, the greater its luminosity, and the more rapidly it fuses its hydrogen fuel into helium in its core. Over time, this hydrogen fuel is completely converted into helium, and the star begins to "evolve. The fusion of helium requires a higher core temperature. A star with a high enough core temperature will push its outer layers outward while increasing its core density. The resulting "red giant formed by the expanding outer layers enjoys a brief life span, before the helium fuel in the core is in turn consumed. Very massive stars can also undergo a series of evolutionary phases, as they fuse increasingly heavier elements.
The final fate of the star depends on its mass, with stars of mass greater than about eight times the Sun becoming core collapse "supernovae; while smaller stars blow off their outer layers and leave behind the inert core in the form of a "white dwarf. The ejection of the outer layers forms a "planetary nebulae. The remnant of a supernova is a dense "neutron star, or, if the stellar mass was at least three times that of the Sun, a "black hole. Closely orbiting binary stars can follow more complex evolutionary paths, such as mass transfer onto a white dwarf companion that can potentially cause a supernova. Planetary nebulae and supernovae distribute the ""metals" produced in the star by fusion to the interstellar medium; without them, all new stars (and their planetary systems) would be formed from hydrogen and helium alone.
Our "solar system orbits within the "Milky Way, a "barred spiral galaxy that is a prominent member of the "Local Group of galaxies. It is a rotating mass of gas, dust, stars and other objects, held together by mutual gravitational attraction. As the Earth is located within the dusty outer arms, there are large portions of the Milky Way that are obscured from view.
In the center of the Milky Way is the core, a bar-shaped bulge with what is believed to be a "supermassive black hole at its center. This is surrounded by four primary arms that spiral from the core. This is a region of active star formation that contains many younger, "population I stars. The disk is surrounded by a "spheroid halo of older, "population II stars, as well as relatively dense concentrations of stars known as "globular clusters.
Between the stars lies the "interstellar medium, a region of sparse matter. In the densest regions, "molecular clouds of "molecular hydrogen and other elements create star-forming regions. These begin as a compact "pre-stellar core or "dark nebulae, which concentrate and collapse (in volumes determined by the "Jeans length) to form compact protostars.
As the more massive stars appear, they transform the cloud into an "H II region (ionized atomic hydrogen) of glowing gas and plasma. The "stellar wind and supernova explosions from these stars eventually cause the cloud to disperse, often leaving behind one or more young "open clusters of stars. These clusters gradually disperse, and the stars join the population of the Milky Way.
Kinematic studies of matter in the Milky Way and other galaxies have demonstrated that there is more mass than can be accounted for by visible matter. A "dark matter halo appears to dominate the mass, although the nature of this dark matter remains undetermined.
The study of objects outside our galaxy is a branch of astronomy concerned with the "formation and evolution of Galaxies, their morphology (description) and "classification, the observation of "active galaxies, and at a larger scale, the "groups and clusters of galaxies. Finally, the latter is important for the understanding of the "large-scale structure of the cosmos.
As the name suggests, an elliptical galaxy has the cross-sectional shape of an "ellipse. The stars move along "random orbits with no preferred direction. These galaxies contain little or no interstellar dust, few star-forming regions, and generally older stars. Elliptical galaxies are more commonly found at the core of galactic clusters, and may have been formed through mergers of large galaxies.
A spiral galaxy is organized into a flat, rotating disk, usually with a prominent bulge or bar at the center, and trailing bright arms that spiral outward. The arms are dusty regions of star formation within which massive young stars produce a blue tint. Spiral galaxies are typically surrounded by a halo of older stars. Both the "Milky Way and one of our nearest galaxy neighbors, the "Andromeda Galaxy, are spiral galaxies.
Irregular galaxies are chaotic in appearance, and are neither spiral nor elliptical. About a quarter of all galaxies are irregular, and the peculiar shapes of such galaxies may be the result of gravitational interaction.
An active galaxy is a formation that emits a significant amount of its energy from a source other than its stars, dust and gas. It is powered by a compact region at the core, thought to be a super-massive black hole that is emitting radiation from in-falling material.
A "radio galaxy is an active galaxy that is very luminous in the "radio portion of the spectrum, and is emitting immense plumes or lobes of gas. Active galaxies that emit shorter frequency, high-energy radiation include "Seyfert galaxies, "Quasars, and "Blazars. Quasars are believed to be the most consistently luminous objects in the known universe.
The "large-scale structure of the cosmos is represented by groups and clusters of galaxies. This structure is organized into a hierarchy of groupings, with the largest being the "superclusters. The collective matter is formed into "filaments and walls, leaving large "voids between.
"Cosmology (from the Greek κόσμος (kosmos) "world, universe" and λόγος (logos) "word, study" or literally "logic") could be considered the study of the Universe as a whole.
Observations of the "large-scale structure of the Universe, a branch known as "physical cosmology, have provided a deep understanding of the formation and evolution of the cosmos. Fundamental to modern cosmology is the well-accepted theory of the "big bang, wherein our Universe began at a single point in time, and thereafter "expanded over the course of 13.8 billion years to its present condition. The concept of the big bang can be traced back to the discovery of the "microwave background radiation in 1965.
In the course of this expansion, the Universe underwent several evolutionary stages. In the very early moments, it is theorized that the Universe experienced a very rapid "cosmic inflation, which homogenized the starting conditions. Thereafter, "nucleosynthesis produced the elemental abundance of the early Universe. (See also "nucleocosmochronology.)
When the first neutral "atoms formed from a sea of primordial ions, space became transparent to radiation, releasing the energy viewed today as the microwave background radiation. The expanding Universe then underwent a Dark Age due to the lack of stellar energy sources.
A hierarchical structure of matter began to form from minute variations in the mass density of space. Matter accumulated in the densest regions, forming clouds of gas and the earliest stars, the "Population III stars. These massive stars triggered the "reionization process and are believed to have created many of the heavy elements in the early Universe, which, through nuclear decay, create lighter elements, allowing the cycle of nucleosynthesis to continue longer.
Gravitational aggregations clustered into filaments, leaving voids in the gaps. Gradually, organizations of gas and dust merged to form the first primitive galaxies. Over time, these pulled in more matter, and were often organized into "groups and clusters of galaxies, then into larger-scale superclusters.
Fundamental to the structure of the Universe is the existence of "dark matter and "dark energy. These are now thought to be its dominant components, forming 96% of the mass of the Universe. For this reason, much effort is expended in trying to understand the physics of these components.
Astronomy and astrophysics have developed significant interdisciplinary links with other major scientific fields. "Archaeoastronomy is the study of ancient or traditional astronomies in their cultural context, utilizing "archaeological and "anthropological evidence. "Astrobiology is the study of the advent and evolution of biological systems in the Universe, with particular emphasis on the possibility of non-terrestrial life. "Astrostatistics is the application of statistics to astrophysics to the analysis of vast amount of observational astrophysical data.
The study of "chemicals found in space, including their formation, interaction and destruction, is called "astrochemistry. These substances are usually found in "molecular clouds, although they may also appear in low temperature stars, brown dwarfs and planets. "Cosmochemistry is the study of the chemicals found within the Solar System, including the origins of the elements and variations in the "isotope ratios. Both of these fields represent an overlap of the disciplines of astronomy and chemistry. As ""forensic astronomy", finally, methods from astronomy have been used to solve problems of law and history.
Astronomy is one of the sciences to which amateurs can contribute the most.
Collectively, amateur astronomers observe a variety of celestial objects and phenomena sometimes with "equipment that they build themselves. Common targets of amateur astronomers include the Sun, the Moon, planets, stars, comets, "meteor showers, and a variety of "deep-sky objects such as star clusters, galaxies, and nebulae. Astronomy clubs are located throughout the world and many have programs to help their members set up and complete observational programs including those to observe all the objects in the Messier (110 objects) or Herschel 400 catalogues of points of interest in the night sky. One branch of amateur astronomy, amateur "astrophotography, involves the taking of photos of the night sky. Many amateurs like to specialize in the observation of particular objects, types of objects, or types of events which interest them.
Most amateurs work at visible wavelengths, but a small minority experiment with wavelengths outside the visible spectrum. This includes the use of infrared filters on conventional telescopes, and also the use of radio telescopes. The pioneer of amateur radio astronomy was "Karl Jansky, who started observing the sky at radio wavelengths in the 1930s. A number of amateur astronomers use either homemade telescopes or use radio telescopes which were originally built for astronomy research but which are now available to amateurs (e.g. the "One-Mile Telescope).
Amateur astronomers continue to make scientific contributions to the field of astronomy and it is one of the few scientific disciplines where amateurs can still make significant contributions. Amateurs can make occultation measurements that are used to refine the orbits of minor planets. They can also discover comets, and perform regular observations of variable stars. Improvements in digital technology have allowed amateurs to make impressive advances in the field of astrophotography.
Although the scientific discipline of "astronomy has made tremendous strides in understanding the nature of the Universe and its contents, there remain some important unanswered questions. Answers to these may require the construction of new ground- and space-based instruments, and possibly new developments in theoretical and experimental physics.
third paragraph, "There is currently much ongoing research by scientists attempting to discover exactly what this dark matter is"
Astronomy has traditionally been among the most fertile fields for serious amateurs [...]
This poses a challenge to these models, because [...]