Outer space, or simply space, is the void that exists between celestial bodies, including the Earth. It is not completely empty, but consists of a hard vacuum containing a low density of particles: predominantly a plasma of hydrogen and helium, as well as electromagnetic radiation, magnetic fields, and neutrinos. The baseline temperature, as set by the background radiation from the Big Bang, is 2.7 kelvin (K). Plasma with a density of less than one hydrogen atom per cubic meter and a temperature of millions of kelvin in the space between galaxies accounts for most of the baryonic (ordinary) matter in outer space; local concentrations have condensed into stars and galaxies. In most galaxies, observations provide evidence that 90% of the mass is in an unknown form, called dark matter, which interacts with other matter through gravitational but not electromagnetic forces. Data indicates that the majority of the mass-energy in the observable Universe is a poorly understood vacuum energy of space which astronomers label dark energy. Intergalactic space takes up most of the volume of the Universe, but even galaxies and star systems consist almost entirely of empty space.
There is no firm boundary where space begins. However the Kármán line, at an altitude of 100 km (62 mi) above sea level, is conventionally used as the start of outer space in space treaties and for aerospace records keeping. The framework for international space law was established by the Outer Space Treaty, which was passed by the United Nations in 1967. This treaty precludes any claims of national sovereignty and permits all states to freely explore outer space. In 1979, the Moon Treaty made the surfaces of objects such as planets, as well as the orbital space around these bodies, the jurisdiction of the international community. Despite the drafting of UN resolutions for the peaceful uses of outer space, anti-satellite weapons have been tested in Earth orbit.
Humans began the physical exploration of space during the 20th century with the advent of high-altitude balloon flights, followed by manned rocket launches. Earth orbit was first achieved by Yuri Gagarin of the Soviet Union in 1961 and unmanned spacecraft have since reached all of the known planets in the Solar System. Achieving low Earth orbit requires a minimum velocity of 28,100 km/h (17,500 mph), much faster than any conventional aircraft. Outer space represents a challenging environment for human exploration because of the dual hazards of vacuum and radiation. Microgravity has a negative effect on human physiology, causing muscle atrophy and bone loss. Space travel has been limited to low Earth orbit and the Moon for manned flight, and the vicinity of the Solar System for unmanned vehicles. In August 2012, Voyager 1 became the first man-made craft to enter interstellar space.
- 1 Discovery
- 2 Formation and state
- 3 Environment
- 4 Boundary
- 5 Legal status
- 6 Earth orbit
- 7 Regions
- 8 Exploration and applications
- 9 See also
- 10 References
- 11 External links
In 350 BC, Greek philosopher Aristotle suggested that nature abhors a vacuum, a principle that became known as the horror vacui. This concept built upon a 5th-century BCE ontological argument by the Greek philosopher Parmenides, who denied the possible existence of a void in space. Based on this idea that a vacuum could not exist, in the West it was widely held for many centuries that space could not be empty. As late as the 17th century, the French philosopher René Descartes argued that the entirety of space must be filled.
In ancient China, there were various schools of thought concerning the nature of the heavens, some of which bear a resemblance to the modern understanding. In the 2nd century, astronomer Zhang Heng became convinced that space must be infinite, extending well beyond the mechanism that supported the Sun and the stars. The surviving books of the Hsüan Yeh school said that the heavens were boundless, "empty and void of substance". Likewise, the "sun, moon, and the company of stars float in the empty space, moving or standing still".
The Italian scientist Galileo Galilei knew that air had mass and so was subject to gravity. In 1640, he demonstrated that an established force resisted the formation of a vacuum. However, it would remain for his pupil Evangelista Torricelli to create an apparatus that would produce a vacuum in 1643. This experiment resulted in the first mercury barometer and created a scientific sensation in Europe. The French mathematician Blaise Pascal reasoned that if the column of mercury was supported by air then the column ought to be shorter at higher altitude where the air pressure is lower. In 1648, his brother-in-law, Florin Périer, repeated the experiment on the Puy-de-Dôme mountain in central France and found that the column was shorter by three inches. This decrease in pressure was further demonstrated by carrying a half-full balloon up a mountain and watching it gradually inflate, then deflate upon descent.
In 1650, German scientist Otto von Guericke constructed the first vacuum pump: a device that would further refute the principle of horror vacui. He correctly noted that the atmosphere of the Earth surrounds the planet like a shell, with the density gradually declining with altitude. He concluded that there must be a vacuum between the Earth and the Moon.
Back in the 15th century, German theologian Nicolaus Cusanus speculated that the Universe lacked a center and a circumference. He believed that the Universe, while not infinite, could not be held as finite as it lacked any bounds within which it could be contained. These ideas led to speculations as to the infinite dimension of space by the Italian philosopher Giordano Bruno in the 16th century. He extended the Copernican heliocentric cosmology to the concept of an infinite Universe filled with a substance he called aether, which did not cause resistance to the motions of heavenly bodies. English philosopher William Gilbert arrived at a similar conclusion, arguing that the stars are visible to us only because they are surrounded by a thin aether or a void. This concept of an aether originated with ancient Greek philosophers, including Aristotle, who conceived of it as the medium through which the heavenly bodies moved.
The concept of a Universe filled with a luminiferous aether remained in vogue among some scientists until the early 20th century. This form of aether was viewed as the medium through which light could propagate. In 1887, the Michelson–Morley experiment tried to detect the Earth's motion through this medium by looking for changes in the speed of light depending on the direction of the planet's motion. However, the null result indicated something was wrong with the concept. The idea of the luminiferous aether was then abandoned. It was replaced by Albert Einstein's theory of special relativity, which holds that the speed of light in a vacuum is a fixed constant, independent of the observer's motion or frame of reference.
The first professional astronomer to support the concept of an infinite Universe was the Englishman Thomas Digges in 1576. But the scale of the Universe remained unknown until the first successful measurement of the distance to a nearby star in 1838 by the German astronomer Friedrich Bessel. He showed that the star 61 Cygni had a parallax of just 0.31 arcseconds (compared to the modern value of 0.287″). This corresponds to a distance of over 10 light years. The distance to the Andromeda Galaxy was determined in 1923 by American astronomer Edwin Hubble by measuring the brightness of cepheid variables in that galaxy, a new technique discovered by Henrietta Leavitt. This established that the Andromeda galaxy, and by extension all galaxies, lay well outside the Milky Way.
The earliest known estimate of the temperature of outer space was by the Swiss physicist Charles É. Guillaume in 1896. Using the estimated radiation of the background stars, he concluded that space must be heated to a temperature of 5–6 K. British physicist Arthur Eddington made a similar calculation to derive a temperature of 3.18° in 1926. 1933 German physicist Erich Regener used the total measured energy of cosmic rays to estimate an intergalactic temperature of 2.8 K.
The modern concept of outer space is based on the "Big Bang" cosmology, first proposed in 1931 by the Belgian physicist Georges Lemaître. This theory holds that the observable Universe originated from a very compact form that has since undergone continuous expansion. The background energy released during the initial expansion has steadily decreased in density, leading to a 1948 prediction by American physicts Ralph Alpher and Robert Herman of a temperature of 5 K for the temperature of space.
The term outer space was used as early as 1842 by the English poet Lady Emmeline Stuart-Wortley in her poem "The Maiden of Moscow". The expression outer space was used as an astronomical term by Alexander von Humboldt in 1845. It was later popularized in the writings of H. G. Wells in 1901. The shorter term space is actually older, first used to mean the region beyond Earth's sky in John Milton's Paradise Lost in 1667.
Formation and state
According to the Big Bang theory, the Universe originated in an extremely hot and dense state about 13.8 billion years ago and began expanding rapidly. About 380,000 years later the Universe had cooled sufficiently to allow protons and electrons to combine and form hydrogen—the so-called recombination epoch. When this happened, matter and energy became decoupled, allowing photons to travel freely through space. The matter that remained following the initial expansion has since undergone gravitational collapse to create stars, galaxies and other astronomical objects, leaving behind a deep vacuum that forms what is now called outer space. As light has a finite velocity, this theory also constrains the size of the directly observable Universe. This leaves open the question as to whether the Universe is finite or infinite.
The present day shape of the Universe has been determined from measurements of the cosmic microwave background using satellites like the Wilkinson Microwave Anisotropy Probe. These observations indicate that the observable Universe is flat, meaning that photons on parallel paths at one point will remain parallel as they travel through space to the limit of the observable Universe, except for local gravity. The flat Universe, combined with the measured mass density of the Universe and the accelerating expansion of the Universe, indicates that space has a non-zero vacuum energy, which is called dark energy.
Estimates put the average energy density of the Universe at the equivalent of 5.9 protons per cubic meter, including dark energy, dark matter, and baryonic matter (ordinary matter composed of atoms). The atoms account for only 4.6% of the total energy density, or a density of one proton per four cubic meters. The density of the Universe, however, is clearly not uniform; it ranges from relatively high density in galaxies—including very high density in structures within galaxies, such as planets, stars, and black holes—to conditions in vast voids that have much lower density, at least in terms of visible matter. Unlike the matter and dark matter, the dark energy seems not to be concentrated in galaxies: although dark energy may account for a majority of the mass-energy in the Universe, dark energy's influence is 5 orders of magnitude smaller than the influence of gravity from matter and dark matter within the Milky Way.
Outer space is the closest natural approximation to a perfect vacuum. It has effectively no friction, allowing stars, planets and moons to move freely along their ideal orbits. However, even the deep vacuum of intergalactic space is not devoid of matter, as it contains a few hydrogen atoms per cubic meter. By comparison, the air we breathe contains about 1025 molecules per cubic meter. The sparse density of matter in outer space means that electromagnetic radiation can travel great distances without being scattered: the mean free path of a photon in intergalactic space is about 1023 km, or 10 billion light years. In spite of this, extinction, which is the absorption and scattering of photons by dust and gas, is an important factor in galactic and intergalactic astronomy.
Stars, planets and moons retain their atmospheres by gravitational attraction. Atmospheres have no clearly delineated boundary: the density of atmospheric gas gradually decreases with distance from the object until it becomes indistinguishable from the surrounding environment. The Earth's atmospheric pressure drops to about 3.2 × 10−2 Pa at 100 kilometres (62 miles) of altitude, compared to 100 kPA for the International Union of Pure and Applied Chemistry (IUPAC) definition of standard pressure. Beyond this altitude, isotropic gas pressure rapidly becomes insignificant when compared to radiation pressure from the Sun and the dynamic pressure of the solar wind. The thermosphere in this range has large gradients of pressure, temperature and composition, and varies greatly due to space weather.
On the Earth, temperature is defined in terms of the kinetic activity of the surrounding atmosphere. However the temperature of the vacuum cannot be measured in this way. Instead, the temperature is determined by measurement of the radiation. All of the observable Universe is filled with photons that were created during the Big Bang, which is known as the cosmic microwave background radiation (CMB). (There is quite likely a correspondingly large number of neutrinos called the cosmic neutrino background.) The current black body temperature of the background radiation is about 3 K (−270 °C; −454 °F). Some regions of outer space can contain highly energetic particles that have a much higher temperature than the CMB, such as the corona of the Sun where temperatures can range over 1.2–2.6 MK.
Outside of a protective atmosphere and magnetic field, there are few obstacles to the passage through space of energetic subatomic particles known as cosmic rays. These particles have energies ranging from about 106 eV up to an extreme 1020 eV of ultra-high-energy cosmic rays. The peak flux of cosmic rays occurs at energies of about 109 eV, with approximately 87% protons, 12% helium nuclei and 1% heavier nuclei. In the high energy range, the flux of electrons is only about 1% of that of protons. Cosmic rays can damage electronic components and pose a health threat to space travelers.
Despite the harsh environment, several life forms have been found that can withstand extreme space conditions for extended periods. Species of lichen carried on the ESA BIOPAN facility survived exposure for ten days in 2007. Seeds of arabidopsis thaliana and nicotiana tabacum germinated after being exposed to space for 1.5 years. A strain of bacillus subtilis has survived 559 days when exposed to low-Earth orbit or a simulated martian environment. The lithopanspermia hypothesis suggests that rocks ejected into outer space from life-harboring planets may successfully transport life forms to another habitable world. A conjecture is that just such a scenario occurred early in the history of the Solar System, with potentially microorganism-bearing rocks being exchanged between Venus, Earth, and Mars.
Effect on human bodies
Sudden exposure to very low pressure, such as during a rapid decompression, can cause pulmonary barotrauma—a rupture of the lungs, due to the large pressure differential between inside and outside of the chest. Even if the victim's airway is fully open, the flow of air through the windpipe may be too slow to prevent the rupture. Rapid decompression can rupture eardrums and sinuses, bruising and blood seep can occur in soft tissues, and shock can cause an increase in oxygen consumption that leads to hypoxia.
As a consequence of rapid decompression, any oxygen dissolved in the blood will empty into the lungs to try to equalize the partial pressure gradient. Once the deoxygenated blood arrives at the brain, humans and animals will lose consciousness after a few seconds and die of hypoxia within minutes. Blood and other body fluids boil when the pressure drops below 6.3 kPa, and this condition is called ebullism. The steam may bloat the body to twice its normal size and slow circulation, but tissues are elastic and porous enough to prevent rupture. Ebullism is slowed by the pressure containment of blood vessels, so some blood remains liquid. Swelling and ebullism can be reduced by containment in a flight suit. Shuttle astronauts wear a fitted elastic garment called the Crew Altitude Protection Suit (CAPS) which prevents ebullism at pressures as low as 2 kPa. Space suits are needed at 8 km (5.0 mi) to provide enough oxygen for breathing and to prevent water loss, while above 20 km (12 mi) they are essential to prevent ebullism. Most space suits use around 30–39 kPa of pure oxygen, about the same as on the Earth's surface. This pressure is high enough to prevent ebullism, but evaporation of blood could still cause decompression sickness and gas embolisms if not managed.
Because humans are optimized for life in Earth gravity, exposure to weightlessness has been shown to have deleterious effects on the health of the human body. Initially, more than 50% of astronauts experience space motion sickness. This can cause nausea and vomiting, vertigo, headaches, lethargy, and overall malaise. The duration of space sickness varies, but it typically lasts for 1–3 days, after which the body adjusts to the new environment. Longer term exposure to weightlessness results in muscle atrophy and deterioration of the skeleton, or spaceflight osteopenia. These effects can be minimized through a regimen of exercise. Other effects include fluid redistribution, slowing of the cardiovascular system, decreased production of red blood cells, balance disorders, and a weakening of the immune system. Lesser symptoms include loss of body mass, nasal congestion, sleep disturbance, and puffiness of the face.
For long duration space travel, radiation can pose an acute health hazard. Exposure to radiation sources such as high-energy, ionizing cosmic rays can result in fatigue, nausea, vomiting, as well as damage to the immune system and changes to the white blood cell count. Over longer durations, symptoms include an increase in the risk of cancer, plus damage to the eyes, nervous system, lungs and the gastrointestinal tract. On a round-trip Mars mission lasting three years, nearly the entire body would be traversed by high energy nuclei, each of which can cause ionization damage to cells. Fortunately, most such particles are significantly attenuated by the shielding provided by the aluminum walls of a spacecraft, and can be further diminished by water containers and other barriers. However, the impact of the cosmic rays upon the shielding produces additional radiation that can affect the crew. Further research will be needed to assess the radiation hazards and determine suitable countermeasures.
There is no clear boundary between Earth's atmosphere and space, as the density of the atmosphere gradually decreases as the altitude increases. There are several standard boundary designations, namely:
- The Fédération Aéronautique Internationale has established the Kármán line at an altitude of 100 km (62 mi) as a working definition for the boundary between aeronautics and astronautics. This is used because at an altitude of about 100 km (62 mi), as Theodore von Kármán calculated, a vehicle would have to travel faster than orbital velocity in order to derive sufficient aerodynamic lift from the atmosphere to support itself.
- The United States designates people who travel above an altitude of 50 miles (80 km) as astronauts.
- NASA's mission control uses 76 mi (122 km) as their re-entry altitude (termed the Entry Interface), which roughly marks the boundary where atmospheric drag becomes noticeable (depending on the ballistic coefficient of the vehicle), thus leading shuttles to switch from steering with thrusters to maneuvering with air surfaces.
In 2009, scientists at the University of Calgary reported detailed measurements with a Supra-Thermal Ion Imager (an instrument that measures the direction and speed of ions), which allowed them to establish a boundary at 118 km (73 mi) above Earth. The boundary represents the midpoint of a gradual transition over tens of kilometers from the relatively gentle winds of the Earth's atmosphere to the more violent flows of charged particles in space, which can reach speeds well over 268 m/s (600 mph).
The altitude where the atmospheric pressure matches the vapor pressure of water at the temperature of the human body is called the Armstrong line, named after American physician Harry G. Armstrong. Located at an altitude of around 19.14 km (11.89 mi), this is the height at which water in the blood stream changes phase from liquid to gas; in other words, the blood begins to boil. Hence, at this altitude the human body requires a pressure suit, or a pressurized capsule, to survive. The region between the Armstrong line and the Karman line is sometimes termed near space.
The Outer Space Treaty provides the basic framework for international space law. It covers the legal use of outer space by nation states, and includes in its definition of outer space the Moon and other celestial bodies. The treaty states that outer space is free for all nation states to explore and is not subject to claims of national sovereignty. It also prohibits the deployment of nuclear weapons in outer space. The treaty was passed by the United Nations General Assembly in 1963 and signed in 1967 by the USSR, the United States of America and the United Kingdom. As of January 1, 2008 the treaty has been ratified by 98 states and signed by an additional 27 states.
Beginning in 1958, outer space has been the subject of multiple resolutions by the United Nations General Assembly. Of these, more than 50 have been concerning the international co-operation in the peaceful uses of outer space and preventing an arms race in space. Four additional space law treaties have been negotiated and drafted by the UN's Committee on the Peaceful Uses of Outer Space. Still, there remains no legal prohibition against deploying conventional weapons in space, and anti-satellite weapons have been successfully tested by the US, USSR and China. The 1979 Moon Treaty turned the jurisdiction of all heavenly bodies (including the orbits around such bodies) over to the international community. However, this treaty has not been ratified by any nation that currently practices manned spaceflight.
In 1976 eight equatorial states (Ecuador, Colombia, Brazil, Congo, Zaire, Uganda, Kenya, and Indonesia) met in Bogotá, Colombia. They made the "Declaration of the First Meeting of Equatorial Countries," also known as "the Bogotá Declaration", where they made a claim to control the segment of the geosynchronous orbital path corresponding to each country. These claims are not internationally accepted.
A spacecraft enters orbit when it has enough horizontal velocity for its centripetal acceleration due to gravity to be less than or equal to the centrifugal acceleration due to the horizontal component of its velocity. For a low Earth orbit, this velocity is about 7,800 m/s (28,100 km/h; 17,400 mph); by contrast, the fastest manned airplane speed ever achieved (excluding speeds achieved by deorbiting spacecraft) was 2,200 m/s (7,900 km/h; 4,900 mph) in 1967 by the North American X-15.
To achieve an orbit, a spacecraft must travel faster than a sub-orbital spaceflight. The energy required to reach Earth orbital velocity at an altitude of 600 km (370 mi) is about 36 MJ/kg, which is six times the energy needed merely to climb to the corresponding altitude. Spacecraft with a perigee below about 2,000 km (1,200 mi) are subject to drag from the Earth's atmosphere, which will cause the orbital altitude to decrease. The rate of orbital decay depends on the satellite's cross-sectional area and mass, as well as variations in the air density of the upper atmosphere. Below about 300 km (190 mi), decay becomes more rapid with lifetimes measured in days. Once a satellite descends to 180 km (110 mi), it will start to burn up in the atmosphere. The escape velocity required to pull free of Earth's gravitational field altogether and move into interplanetary space is about 11,200 m/s (40,300 km/h; 25,100 mph).
Earth's gravity reaches out far past the Van Allen radiation belt and keeps the Moon in orbit at an average distance of 384,403 km (238,857 mi). The region of space where the gravity of a planet tends to dominate the motion of objects in the presence of other perturbing bodies (such as another planet) is known as the Hill sphere. For Earth, this sphere has a radius of about 1,500,000 km (930,000 mi).
Space is a partial vacuum: its different regions are defined by the various atmospheres and "winds" that dominate within them, and extend to the point at which those winds give way to those beyond. Geospace extends from Earth's atmosphere to the outer reaches of Earth's magnetic field, whereupon it gives way to the solar wind of interplanetary space. Interplanetary space extends to the heliopause, whereupon the solar wind gives way to the winds of the interstellar medium. Interstellar space then continues to the edges of the galaxy, where it fades into the intergalactic void.
Geospace is the region of outer space near the Earth. Geospace includes the upper region of the atmosphere and the magnetosphere. The Van Allen radiation belt lies within the geospace. The outer boundary of geospace is the magnetopause, which forms an interface between the planet's magnetosphere and the solar wind. The inner boundary is the ionosphere. As the physical properties and behavior of near Earth space is affected by the behavior of the Sun and space weather, the field of geospace is interlinked with heliophysics; the study of the Sun and its impact on the Solar System planets.
The volume of geospace defined by the magnetopause is compacted in the direction of the Sun by the pressure of the solar wind, giving it a typical subsolar distance of 10 Earth radii from the center of the planet. However, the tail can extend outward to more than 100–200 Earth radii. The Moon passes through the geospace tail during roughly four days each month, during which time the surface is shielded from the solar wind.
Geospace is populated by electrically charged particles at very low densities, the motions of which are controlled by the Earth's magnetic field. These plasmas form a medium from which storm-like disturbances powered by the solar wind can drive electrical currents into the Earth’s upper atmosphere. During geomagnetic storms two regions of geospace, the radiation belts and the ionosphere, can become strongly disturbed. These storms increase fluxes of energetic electrons that can permanently damage satellite electronics, disrupting telecommunications and GPS technologies, and can also be a hazard to astronauts, even in low Earth orbit. They also create aurorae seen near the magnetic poles.
Although it meets the definition of outer space, the atmospheric density within the first few hundred kilometers above the Kármán line is still sufficient to produce significant drag on satellites. This region contains material left over from previous manned and unmanned launches that are a potential hazard to spacecraft. Some of this debris re-enters Earth's atmosphere periodically.
Interplanetary space, the space around the Sun and planets of the Solar System, is the region dominated by the interplanetary medium, which extends out to the heliopause where the influence of the galactic environment starts to dominate over the magnetic field and particle flux from the Sun. Interplanetary space is defined by the solar wind, a continuous stream of charged particles emanating from the Sun that creates a very tenuous atmosphere (the heliosphere) for billions of miles into space. This wind has a particle density of 5–10 protons/cm3 and is moving at a velocity of 350–400 km/s (780,000–890,000 mph). The distance and strength of the heliopause varies depending on the activity level of the solar wind. The discovery since 1995 of extrasolar planets means that other stars must possess their own interplanetary media.
The volume of interplanetary space is a nearly total vacuum, with a mean free path of about one astronomical unit at the orbital distance of the Earth. However, this space is not completely empty, and is sparsely filled with cosmic rays, which include ionized atomic nuclei and various subatomic particles. There is also gas, plasma and dust, small meteors, and several dozen types of organic molecules discovered to date by microwave spectroscopy.
Interplanetary space contains the magnetic field generated by the Sun. There are also magnetospheres generated by planets such as Jupiter, Saturn, Mercury and the Earth that have their own magnetic fields. These are shaped by the influence of the solar wind into the approximation of a teardrop shape, with the long tail extending outward behind the planet. These magnetic fields can trap particles from the solar wind and other sources, creating belts of magnetic particles such as the Van Allen radiation belt. Planets without magnetic fields, such as Mars, have their atmospheres gradually eroded by the solar wind.
Interstellar space is the physical space within a galaxy not occupied by stars or their planetary systems. The contents of interstellar space are called the interstellar medium. The average density of matter in this region is about 106 particles per m3, but this varies from a low of about 104 – 105 in regions of sparse matter up to about 108 – 1010 in dark nebula. Regions of star formation may reach 1012 – 1014 particles per m3 (as a comparison, Earth's atmospheric density at sea level is on the order of 1025 particles per m3). Nearly 70% of the mass of the interstellar medium consists of lone hydrogen atoms. This is enriched with helium atoms as well as trace amounts of heavier atoms formed through stellar nucleosynthesis. These atoms can be ejected into the interstellar medium by stellar winds, or when evolved stars begin to shed their outer envelopes such as during the formation of a planetary nebula. The cataclysmic explosion of a supernova will generate an expanding shock wave consisting of ejected materials.
A number of molecules exist in interstellar space, as can tiny, 0.1 μm dust particles. The tally of molecules discovered through radio astronomy is steadily increasing at the rate of about four new species per year. Large regions of higher density matter known as molecular clouds allow chemical reactions to occur, including the formation of organic polyatomic species. Much of this chemistry is driven by collisions. Energetic cosmic rays penetrate the cold, dense clouds and ionize hydrogen and helium, resulting, for example, in the trihydrogen cation. An ionized helium atom can then split relatively abundant carbon monoxide to produce ionized carbon, which in turn can lead to organic chemical reactions.
The local interstellar medium is a region of space within 100 parsecs (pc) of the Sun, which is of interest both for its proximity and for its interaction with the Solar System. This volume nearly coincides with a region of space known as the Local Bubble, which is characterized by a lack of dense, cold clouds. It forms a cavity in the Orion Arm of the Milky Way galaxy, with dense molecular clouds lying along the borders, such as those in the constellations of Ophiuchus and Taurus. (The actual distance to the border of this cavity varies from 60 to 250 pc or more.) This volume contains about 104–105 stars and the local interstellar gas counterbalances the astrospheres that surround these stars, with the volume of each sphere varying depending on the local density of the interstellar medium. The Local Bubble contains dozens of warm interstellar clouds with temperatures of up to 7,000 K and radii of 0.5–5 pc.
When stars are moving at a sufficiently high peculiar velocity, their astrosphere can generate a bow shock as it collides with the interstellar medium. For decades it was assumed that the Sun had a bow shock. In 2012, data from Interstellar Boundary Explorer (IBEX) and Voyagers showed that the Sun's bow shock does not exist. Instead, these authors argue that a subsonic bow wave defines the transition from the solar wind flow to the interstellar medium. A bow shock is the third boundary of an astrosphere after the termination shock and the astropause (called the heliopause in the Solar System).
Intergalactic space is the physical space between galaxies. The huge spaces between galaxy clusters are called the voids. Surrounding and stretching between galaxies, there is a rarefied plasma that is organized in a galactic filamentary structure. This material is called the intergalactic medium (IGM). The density of the IGM is 5-200 times the average density of the Universe. It consists mostly of ionized hydrogen; i.e. a plasma consisting of equal numbers of electrons and protons. As gas falls into the intergalactic medium from the voids, it heats up to temperatures of 105 K to 107 K, which is high enough so that collisions between atoms have enough energy to cause the bound electrons to escape from the hydrogen nuclei; this is why the IGM is ionized. At these temperatures, it is called the warm–hot intergalactic medium (WHIM). (Although the gas is very hot by terrestrial standards, 105 K is often called "warm" in astrophysics.) Computer simulations and observations indicate that up to half of the atomic matter in the Universe might exist in this warm-hot, rarefied state. When gas falls from the filamentary structures of the WHIM into the galaxy clusters at the intersections of the cosmic filaments, it can heat up even more, reaching temperatures of 108 K and above in the so-called intracluster medium.
Exploration and applications
For the majority of human history, space was explored by remote observation; initially with the unaided eye and then with the telescope. Prior to the advent of reliable rocket technology, the closest that humans had come to reaching outer space was through the use of balloon flights. In 1935, the U.S. Explorer II manned balloon flight had reached an altitude of 22 km (14 mi). This was greatly exceeded in 1942 when the third launch of the German A-4 rocket climbed to an altitude of about 80 km (50 mi). In 1957, the unmanned satellite Sputnik 1 was launched by a Russian R-7 rocket, achieving Earth orbit at an altitude of 215–939 kilometres (134–583 mi). This was followed by the first human spaceflight in 1961, when Yuri Gagarin was sent into orbit on Vostok 1. The first humans to escape Earth orbit were Frank Borman, Jim Lovell and William Anders in 1968 on board the U.S. Apollo 8, which achieved lunar orbit and reached a maximum distance of 377,349 km (234,474 mi) from the Earth.
The first spacecraft to reach escape velocity was the Soviet Luna 1, which performed a fly-by of the Moon in 1959. In 1961, Venera 1 became the first planetary probe. It revealed the presence of the solar wind and performed the first fly-by of the planet Venus, although contact was lost before reaching Venus. The first successful planetary mission was the Mariner 2 fly-by of Venus in 1962. The first spacecraft to perform a fly-by of Mars was Mariner 4, which reached the planet in 1964. Since that time, unmanned spacecraft have successfully examined each of the Solar System's planets, as well their moons and many minor planets and comets. They remain a fundamental tool for the exploration of outer space, as well as observation of the Earth. In August 2012, Voyager 1 became the first man-made object to leave the Solar System and enter interstellar space.
The absence of air makes outer space (and the surface of the Moon) ideal locations for astronomy at all wavelengths of the electromagnetic spectrum, as evidenced by the spectacular pictures sent back by the Hubble Space Telescope, allowing light from about 13.8 billion years ago—almost to the time of the Big Bang—to be observed. However, not every location in space is ideal for a telescope. The interplanetary zodiacal dust emits a diffuse near-infrared radiation that can mask the emission of faint sources such as extrasolar planets. Moving an infrared telescope out past the dust will increase the effectiveness of the instrument. Likewise, a site like the Daedalus crater on the far side of the Moon could shield a radio telescope from the radio frequency interference that hampers Earth-based observations.
Unmanned spacecraft in Earth orbit have become an essential technology of modern civilization. They allow direct monitoring of weather conditions, relay long-range communications including telephone calls and television signals, provide a means of precise navigation, and allow remote sensing of the Earth. The latter role serves a wide variety of purposes, including tracking soil moisture for agriculture, prediction of water outflow from seasonal snow packs, detection of diseases in plants and trees, and surveillance of military activities.
The deep vacuum of space could make it an attractive environment for certain industrial processes, such as those that require ultraclean surfaces. However, like asteroid mining, space manufacturing requires a significant investment with little prospect of an immediate return.
- Earth's location in the universe
- Human outpost
- Interplanetary Internet
- Space Agency
- Space and survival
- Space science
- Space station
- Space technology
- Timeline of knowledge about the interstellar and intergalactic medium
- Timeline of Solar System exploration
- Timeline of spaceflight
- List of topics in space
- Dainton 2001, pp. 132–133.
- Chuss, David T. (June 26, 2008), Cosmic Background Explorer, NASA Goddard Space Flight Center, retrieved 2013-04-27.
- Freedman & Kaufmann 2005, pp. 573, 599-601.
- Trimble, V. (1987). "Existence and nature of dark matter in the universe". Annual Review of Astronomy and Astrophysics 25: 425–472. Bibcode:1987ARA&A..25..425T. doi:10.1146/annurev.aa.25.090187.002233.
- "Dark Energy, Dark Matter". NASA Science. Retrieved May 31, 2013. "It turns out that roughly 68% of the Universe is dark energy. Dark matter makes up about 27%."
- Freedman & Kaufmann 2005, pp. 650-653.
- O'Leary 2009, p. 84.
- Grant 1981, p. 10.
- Porter, Park & Daston 2006, p. 27.
- Eckert 2006, p. 5.
- Needham & Ronan 1985, pp. 82–87.
- Holton & Brush 2001, pp. 267–268.
- Cajori 1917, pp. 64–66.
- Genz 2001, pp. 127–128.
- Tassoul & Tassoul 2004, p. 22.
- Gatti 2002, pp. 99–104.
- Kelly 1965, pp. 97–107.
- Olenick, Apostol & Goodstein 1986, p. 356.
- Hariharan 2003, p. 2.
- Olenick, Apostol & Goodstein 1986, pp. 357–365.
- Thagard 1992, pp. 206–209.
- Maor 1991, p. 195.
- Webb 1999, pp. 71–73.
- Cepheid Variable Stars & Distance Determination, CSIRO Australia, October 25, 2004, retrieved 2011-09-12.
- Tyson & Goldsmith 2004, pp. 114–115.
- Assis, A. K. T.; Paulo, São; Neves, M. C. D. (July 1995), "History of the 2.7 K Temperature Prior to Penzias and Wilson", Apeiron 2 (3): 79–87, doi:10.1.1.1.2453.
- Lemaître, G. (May 1931), "The Beginning of the World from the Point of View of Quantum Theory", Nature 127 (3210): 706, Bibcode:1931Natur.127..706L, doi:10.1038/127706b0.
- Stuart Wortley 1841, p. 410.
- Von Humboldt 1845, p. 39.
- Harper, Douglas, "Outer", Online Etymology Dictionary, retrieved 2008-03-24.
- Harper, Douglas (November 2001), Space, The Online Etymology Dictionary, retrieved 2009-06-19.
- Turner, Michael S. (September 2009), "Origin of the Universe", Scientific American 301 (3): 36–43, Bibcode:2009SciAm.301c..36T, doi:10.1038/scientificamerican0909-36.
- Silk 2000, pp. 105–308.
- "WMAP — Shape of the universe". NASA. December 21, 2012. Retrieved June 4, 2013.
- Sparke & Gallagher 2007, pp. 329-330.
- Wollack, Edward J. (June 24, 2011), What is the Universe Made Of?, NASA, retrieved 2011-10-14.
- Krumm, N.; Brosch, N. (October 1984), "Neutral hydrogen in cosmic voids", Astronomical Journal 89: 1461–1463, Bibcode:1984AJ.....89.1461K, doi:10.1086/113647.
- Peebles, P.; Ratra, B. (2003). "The cosmological constant and dark energy". Reviews of Modern Physics 75 (2): 559. arXiv:astro-ph/0207347. Bibcode:2003RvMP...75..559P. doi:10.1103/RevModPhys.75.559.
- Tadokoro, M. (1968), "A Study of the Local Group by Use of the Virial Theorem", Publications of the Astronomical Society of Japan 20: 230, Bibcode:1968PASJ...20..230T This source estimates a density of 7 × 10−29 g/cm3 for the Local Group. An atomic mass unit is 1.66 × 10−24 g, for roughly 40 atoms per cubic meter.
- Borowitz & Beiser 1971.
- Davies 1977, p. 93.
- Fitzpatrick, E. L. (May 2004), "Interstellar Extinction in the Milky Way Galaxy", in Witt, Adolf N.; Clayton, Geoffrey C.; Draine, Bruce T., Astrophysics of Dust, ASP Conference Series 309, p. 33, arXiv:astro-ph/0401344, Bibcode:2004ASPC..309...33F.
- Chamberlain 1978, p. 2.
- Squire, Tom (September 27, 2000), "U.S. Standard Atmosphere, 1976", Thermal Protection Systems Expert and Material Properties Database (NASA), retrieved 2011-10-23.
- Forbes, Jeffrey M. (2007), "Dynamics of the thermosphere", Journal of the Meteorological Society of Japan, Series II 85B: 193–213, retrieved 2012-03-25.
- Fixsen, D. J. (December 2009), "The Temperature of the Cosmic Microwave Background", The Astrophysical Journal 707 (2): 916–920, arXiv:0911.1955, Bibcode:2009ApJ...707..916F, doi:10.1088/0004-637X/707/2/916.
- Withbroe, George L. (February 1988), "The temperature structure, mass, and energy flow in the corona and inner solar wind", Astrophysical Journal, Part 1 325: 442–467, Bibcode:1988ApJ...325..442W, doi:10.1086/166015.
- Letessier-Selvon, Antoine; Stanev, Todor (July 2011), "Ultrahigh energy cosmic rays", Reviews of Modern Physics 83 (3): 907–942, arXiv:1103.0031, Bibcode:2011RvMP...83..907L, doi:10.1103/RevModPhys.83.907.
- Lang 1999, p. 462.
- Lide 1993, p. 11-217.
- Raggio, J. et al. (May 2011), "Whole Lichen Thalli Survive Exposure to Space Conditions: Results of Lithopanspermia Experiment with Aspicilia fruticulosa", Astrobiology 11 (4): 281–292, Bibcode:2011AsBio..11..281R, doi:10.1089/ast.2010.0588.
- Tepfer, David et al. (May 2012), "Survival of Plant Seeds, Their UV Screens, and nptII DNA for 18 Months Outside the International Space Station", Astrobiology 12 (5): 517–528, Bibcode:2012AsBio..12..517T, doi:10.1089/ast.2011.0744, retrieved 2013-05-19.
- Wassmann, Marko et al. (May 2012), "Survival of Spores of the UV-ResistantBacillus subtilis Strain MW01 After Exposure to Low-Earth Orbit and Simulated Martian Conditions: Data from the Space Experiment ADAPT on EXPOSE-E", Astrobiology 12 (5): 498–507, Bibcode:2012AsBio..12..498W, doi:10.1089/ast.2011.0772.
- Nicholson, W. L. (April 2010), "Towards a General Theory of Lithopanspermia", Astrobiology Science Conference 2010: 5272–528, Bibcode:2010LPICo1538.5272N.
- Bolonkin, Alexander (2009), "Man in Outer Space Without a Special Space Suit", American Journal of Engineering and Applied Sciences 2 (4): 573–579, retrieved 2011-12-15.
- Krebs, Matthew B.; Pilmanis, Andrew A. (November 1996), Human pulmonary tolerance to dynamic over-pressure, United States Air Force Armstrong Laboratory, retrieved 2011-12-23.
- Harding, R. M.; Mills, F. J. (April 30, 1983), "Aviation medicine. Problems of altitude I: hypoxia and hyperventilation", British Medical Journal 286 (6375): 1408–1410, doi:10.1136/bmj.286.6375.1408.
- Hodkinson, P. D. (March 2011), "Acute exposure to altitude", Journal of the Royal Army Medical Corps 157 (1): 85–91, PMID 21465917, retrieved 2011-12-16.
- Billings 1973, pp. 1–34.
- Landis, Geoffrey A. (August 7, 2007), Human Exposure to Vacuum, www.geoffreylandis.com, retrieved 2009-06-19.
- Webb, P. (1968), "The Space Activity Suit: An Elastic Leotard for Extravehicular Activity", Aerospace Medicine 39 (4): 376–383, PMID 4872696.
- Ellery 2000, p. 68.
- Davis, Johnson & Stepanek 2008, pp. 270-271.
- Kanas, Nick; Manzey, Dietrich (2008), "Basic Issues of Human Adaptation to Space Flight", Space Psychology and Psychiatry, Space Technology Library 22: 15–48, doi:10.1007/978-1-4020-6770-9_2.
- Williams, David et al. (June 23, 2009), "Acclimation during space flight: effects on human physiology", Canadian Medical Association Journal 180 (13): 1317–1323, doi:10.1503/cmaj.090628.
- Kennedy, Ann R., Radiation Effects, National Space Biological Research Institute, retrieved 2011-12-16.
- Setlow, Richard B. (November 2003), "The hazards of space travel", Science and Society 4 (11): 1013–1016, doi:10.1038/sj.embor.7400016.
- Wong & Fergusson 2010, p. 16.
- Petty, John Ira (February 13, 2003), "Entry", Human Spaceflight (NASA), retrieved 2011-12-16.
- Thompson, Andrea (April 9, 2009), Edge of Space Found, space.com, retrieved 2009-06-19.
- Sangalli, L. et al. (2009), "Rocket-based measurements of ion velocity, neutral wind, and electric field in the collisional transition region of the auroral ionosphere", Journal of Geophysical Research (American Geophysical Union) 114: A04306, Bibcode:2009JGRA..11404306S, doi:10.1029/2008JA013757.
- Piantadosi 2003, pp. 188-189.
- Treaty on Principles Governing the Activities of States in the Exploration and Use of Outer Space, including the Moon and Other Celestial Bodies, United Nations Office for Outer Space Affairs, January 1, 2008, retrieved 2009-12-30.
- Index of Online General Assembly Resolutions Relating to Outer Space, United Nations Office for Outer Space Affairs, 2011, retrieved 2009-12-30.
- Wong & Fergusson 2010, p. 4.
- Columbus launch puts space law to the test, European Science Foundation, November 5, 2007, retrieved 2009-12-30.
- Representatives of the States traversed by the Equator (December 3, 1976), "Declaration of the first meeting of equatorial countries", Space Law (Bogota, Republic of Colombia: JAXA), retrieved 2011-10-14.
- Gangale, Thomas (2006), "Who Owns the Geostationary Orbit?", Annals of Air and Space Law 31, retrieved 2011-10-14.
- Hill, James V. H. (April 1999), "Getting to Low Earth Orbit", Space Future, retrieved 2012-03-18.
- Shiner, Linda (November 1, 2007), X-15 Walkaround, Air & Space Magazine, retrieved 2009-06-19.
- Dimotakis, P. et al. (October 1999), 100 lbs to Low Earth Orbit (LEO): Small-Payload Launch Options, The Mitre Corporation, pp. 1–39, retrieved 2012-01-21.
- Kennewell, John; McDonald, Andrew (2011), Satellite Lifetimes and Solar Activity, Commonwealth of Australia Bureau of Weather, Space Weather Branch, retrieved 2011-12-31.
- Williams, David R. (November 17, 2010), "Earth Fact Sheet", Lunar & Planetary Science (NASA), retrieved 2012-05-10.
- Yoder, Charles F., "Astrometric and Geodetic Properties of Earth and the Solar System" (PDF), in Ahrens, Thomas J., Global earth physics a handbook of physical constants, AGU reference shelf Series 1, Washington, DC: American Geophysical Union, p. 1, Bibcode:1995geph.conf....1Y, ISBN 0-87590-851-9, retrieved 2011-12-31.. This work lists a Hill sphere radius of 234.9 times the mean radius of Earth, or 234.9 × 6,371 km = 1.5 million km.
- Schrijver & Siscoe 2010, p. 363.
- Kintner, Paul; GMDT Committee and Staff (September 2002), Report of the Living With a Star Geospace Mission Definition Team (PDF), NASA, retrieved 2012-04-15.
- Fichtner & Liu 2011, pp. 341–345.
- Koskinen 2010, pp. 32, 42.
- Mendillo 2000, p. 275.
- "Geomagnetic Storms", OECD/IFP Futures Project on "Future Global Shocks" (CENTRA Technology, Inc.), January 14, 2011: 1–69, retrieved 2012-04-07.
- Portree, David; Loftus, Joseph (1999), Orbital Debris: A Chronology, NASA, p. 13, retrieved 2012-05-05.
- "The cislunar gateway with no gate". The Space Review.
- Papagiannis 1972, pp. 12–149.
- Phillips, Tony (2009-09-29), Cosmic Rays Hit Space Age High, NASA, retrieved 2009-10-20.
- Frisch et al. 2002, pp. 21–34.
- Flynn, G. J. et al. (2003), "The Origin of Organic Matter in the Solar System: Evidence from the Interplanetary Dust Particles", in Norris, R.; Stootman, F., Bioastronomy 2002: Life Among the Stars, Proceedings of IAU Symposium #213, San Francisco: Astronomical Society of the Pacific, Bibcode:2004IAUS..213..275F.
- Johnson, R. E. (August 1994), "Plasma-Induced Sputtering of an Atmosphere", Space Science Reviews 69 (3-4): 215–253, Bibcode:1994SSRv...69..215J, doi:10.1007/BF02101697.
- Tyson, Patrick (January 2012). "The Kinetic Atmosphere: Molecular Numbers". Retrieved 13 September 2013.
- Rauchfuss 2008, pp. 72–81.
- Klemperer, William (August 15, 2006), "Interstellar chemistry", Proceedings of the National Academy of Sciences of the United States of America 103 (33): 12232–12234, Bibcode:2006PNAS..10312232K, doi:10.1073/pnas.0605352103, PMC 1567863.
- Redfield, S. (September 2006), "The Local Interstellar Medium", New Horizons in Astronomy; Proceedings of the Conference Held 16–18 October 2005 at The University of Texas, Austin, Texas, USA, Frank N. Bash Symposium ASP Conference Series 352, p. 79, arXiv:astro-ph/0601117, Bibcode:2006ASPC..352...79R.
- McComas, D. J. et al. (2012), "The Heliosphere's Interstellar Interaction: No Bow Shock", Science, Bibcode:2012Sci...336.1291M, doi:10.1126/science.1221054.
- Fox, Karen C. (May 10, 2012), NASA - IBEX Reveals a Missing Boundary At the Edge Of the Solar System, NASA, retrieved 2012-05-14.
- Jafelice, Luiz C.; Opher, Reuven (July 1992), "The origin of intergalactic magnetic fields due to extragalactic jets", Monthly Notices of the Royal Astronomical Society (Royal Astronomical Society) 257 (1): 135–151, Bibcode:1992MNRAS.257..135J.
- Wadsley, James W. et al. (August 20, 2002), "The Universe in Hot Gas", Astronomy Picture of the Day (NASA), retrieved 2009-06-19.
- Fang, T. et al. (2010), "Confirmation of X-Ray Absorption by Warm-Hot Intergalactic Medium in the Sculptor Wall", The Astrophysical Journal 714 (2): 1715, arXiv:1001.3692, Bibcode:2010ApJ...714.1715F, doi:10.1088/0004-637X/714/2/1715.
- Gupta, Anjali; Galeazzi, M.; Ursino, E. (May 2010), "Detection and Characterization of the Warm-Hot Intergalactic Medium", Bulletin of the American Astronomical Society 41: 908, Bibcode:2010AAS...21631808G.
- Bykov, A. M.; Paerels, F. B. S.; Petrosian, V. (February 2008), "Equilibration Processes in the Warm-Hot Intergalactic Medium", Space Science Reviews 134 (1–4): 141–153, arXiv:0801.1008, Bibcode:2008SSRv..134..141B, doi:10.1007/s11214-008-9309-4.
- Wakker, B. P.; Savage, B. D. (2009), "The Relationship Between Intergalactic H I/O VI and Nearby (z<0.017) Galaxies", The Astrophysical Journal Supplement Series 182: 378, arXiv:0903.2259, Bibcode:2009ApJS..182..378W, doi:10.1088/0067-0049/182/1/378.
- Mathiesen, B. F.; Evrard, A. E. (2001), "Four Measures of the Intracluster Medium Temperature and Their Relation to a Cluster's Dynamical State", The Astrophysical Journal 546: 100, arXiv:astro-ph/0004309, Bibcode:2001ApJ...546..100M, doi:10.1086/318249.
- Pfotzer, G. (June 1972), "History of the Use of Balloons in Scientific Experiments", Space Science Reviews 13 (2): 199–242, Bibcode:1972SSRv...13..199P, doi:10.1007/BF00175313.
- O'Leary 2009, pp. 209–224.
- Harrison 2002, pp. 60–63.
- Orloff 2001.
- Hardesty, Eisman & Krushchev 2008, pp. 89–90.
- Collins 2007, p. 86.
- Harris 2008, pp. 7, 68–69.
- Wall, Mike. "Voyager 1 Has Left Solar System". Web. Space.com. Retrieved 13 September 2013.
- Landgraf, M. et al. (February 2001), "IRSI/Darwin: peering through the interplanetary dust cloud", ESA Bulletin (105): 60–63, arXiv:astro-ph/0103288, Bibcode:2001ESABu.105...60L.
- Maccone, Claudio (August 2001), "Searching for bioastronomical signals from the farside of the Moon", in Ehrenfreund, P.; Angerer, O.; Battrick, B., Exo-/astro-biology. Proceedings of the First European Workshop, Noordwijk: ESA Publications Division, pp. 277–280, Bibcode:2001ESASP.496..277M, ISBN 92-9092-806-9.
- Razani 2012, pp. 97–99.
- Chapmann, Glenn (May 22–27, 1991), "Space: the Ideal Place to Manufacture Microchips" (PDF), in Blackledge, R.; Radfield, C.; Seida, S., Proceedings of the 10th International Space Development Conference, San Antonio, Texas, pp. 25–33, retrieved 2010-01-12.
- Forgan, Duncan H.; Elvis, Martin (October 2011), "Extrasolar asteroid mining as forensic evidence for extraterrestrial intelligence", International Journal of Astrobiology 10: 307–313, arXiv:1103.5369, Bibcode:2011IJAsB..10..307F, doi:10.1017/S1473550411000127.
- Billings, Charles E. (1973), "Barometric Pressure", in Parker, James F.; West, Vita R., Bioastronautics Data Book (2nd ed.), NASA, Bibcode:1973NASSP3006.....P, NASA SP-3006
- Borowitz, Sidney; Beiser, Arthur (1971), Essentials of physics: a text for students of science and engineering, Addison-Wesley series in physics (2nd ed.), Addison-Wesley Publishing Company Note: this source gives a value of 2.7 × 1025 molecules per cubic meter.
- Cajori, Florian (1917), A history of physics in its elementary branches: including the evolution of physical laboratories, New York: The Macmillan Company
- Chamberlain, Joseph Wyan (1978), Theory of planetary atmospheres: an introduction to their physics and chemistry, International geophysics series 22, Academic Press, ISBN 0-12-167250-6
- Collins, Martin J. (2007), "Mariner 2 Mock-up", After Sputnik: 50 years of the Space Age, HarperCollins, ISBN 0-06-089781-3
- Dainton, Barry (2001), "Conceptions of Void", Time and space, McGill-Queen's Press, ISBN 0-7735-2306-5
- Davis, Jeffrey R.; Johnson, Robert; Stepanek, Jan (2008), Fundamentals of Aerospace Medicine (4th ed.), Lippincott Williams & Wilkins, ISBN 0-7817-7466-7
- Davies, P. C. W. (1977), The physics of time asymmetry, University of California Press, ISBN 0-520-03247-0 Note: a light year is about 1013 km.
- Eckert, Michael (2006), The dawn of fluid dynamics: a discipline between science and technology, Wiley-VCH, ISBN 3-527-40513-5
- Ellery, Alex (2000), An introduction to space robotics, Springer-Praxis books in astronomy and space sciences, Springer, ISBN 1-85233-164-X
- Freedman, Roger A.; Kaufmann, William J. (2005), Universe (seventh ed.), New York: W. H. Freeman and Company, ISBN 0-7167-8694-X
- Fichtner, Horst; Liu, W. William (2011), "Advances in Coordinated Sun-Earth System Science Through Interdisciplinary Initiatives and International Programs", written at Sopron, Hungary, in Miralles, M.P.; Almeida, J. Sánchez, The Sun, the Solar Wind, and the Heliosphere, IAGA Special Sopron Book Series 4, Berlin: Springer, Bibcode:2011sswh.book..341F, doi:10.1007/978-90-481-9787-3_24, ISBN 978-90-481-9786-6
- Frisch, Priscilla C.; Müller, Hans R.; Zank, Gary P.; Lopate, C. (May 6–9, 2002), "Galactic environment of the Sun and stars: interstellar and interplanetary material", in Livio, Mario; Reid, I. Neill; Sparks, William B., Astrophysics of life. Proceedings of the Space Telescope Science Institute Symposium, Space Telescope Science Institute symposium series 16, Baltimore, MD, USA: Cambridge University Press, Bibcode:2005asli.symp...21F, ISBN 0-521-82490-7
- Gatti, Hilary (2002), Giordano Bruno and Renaissance science, Cornell University Press, ISBN 0-8014-8785-4
- Genz, Henning (2001), Nothingness: the science of empty space, Da Capo Press, ISBN 0-7382-0610-5
- Grant, Edward (1981), Much ado about nothing: theories of space and vacuum from the Middle Ages to the scientific revolution, The Cambridge history of science series, Cambridge University Press, ISBN 0-521-22983-9
- Hardesty, Von; Eisman, Gene; Krushchev, Sergei (2008), Epic Rivalry: The Inside Story of the Soviet and American Space Race, National Geographic Books, pp. 89–90, ISBN 1-4262-0321-7
- Hariharan, P. (2003), Optical interferometry (2nd ed.), Academic Press, ISBN 0-12-311630-9
- Harris, Philip Robert (2008), Space enterprise: living and working offworld in the 21st century, Springer Praxis Books / Space Exploration Series, Springer, ISBN 0-387-77639-7
- Harrison, Albert A. (2002), Spacefaring: The Human Dimension, University of California Press, ISBN 0-520-23677-7
- Holton, Gerald James; Brush, Stephen G. (2001), Physics, the human adventure: from Copernicus to Einstein and beyond (3rd ed.), Rutgers University Press, ISBN 0-8135-2908-5
- Kelly, Suzanne (1965), The de muno of William Gilbert, Amsterdam: Menno Hertzberger & Co.
- Koskinen, Hannu (2010), Physics of Space Storms: From the Surface of the Sun to the Earth, Environmental Sciences Series, Springer, ISBN 3-642-00310-9
- Lang, Kenneth R. (1999), Astrophysical formulae: Radiation, gas processes, and high energy astrophysics, Astronomy and astrophysics library (3rd ed.), Birkhäuser, ISBN 3-540-29692-1
- Lide, David R. (1993), CRC handbook of chemistry and physics (74th ed.), CRC Press, ISBN 0-8493-0595-0
- Maor, Eli (1991), To infinity and beyond: a cultural history of the infinite, Princeton paperbacks, ISBN 0-691-02511-8
- Mendillo, Michael (November 8–10, 2000), "The atmosphere of the moon", in Barbieri, Cesare; Rampazzi, Francesca, Earth-Moon Relationships, Padova, Italy at the Accademia Galileiana Di Scienze Lettere Ed Arti: Springer, p. 275, ISBN 0-7923-7089-9
- Needham, Joseph; Ronan, Colin (1985), The Shorter Science and Civilisation in China, Shorter Science and Civilisation in China 2, Cambridge University Press, ISBN 0-521-31536-0
- O'Leary, Beth Laura (2009), Darrin, Ann Garrison, ed., Handbook of space engineering, archaeology, and heritage, Advances in engineering, CRC Press, ISBN 1-4200-8431-3
- Olenick, Richard P.; Apostol, Tom M.; Goodstein, David L. (1986), Beyond the mechanical universe: from electricity to modern physics, Cambridge University Press, ISBN 0-521-30430-X
- Orloff, Richard W. (2001), Apollo by the Numbers: A Statistical Reference, NASA, ISBN 0-16-050631-X, retrieved 2008-01-28
- Papagiannis, Michael D. (1972), Space Physics and Space Astronomy, Taylor & Francis, ISBN 0-677-04000-8
- Piantadosi, Claude A. (2003), The Biology of Human Survival: Life and Death in Extreme Environments, Oxford University Press, ISBN 0199748071
- Porter, Roy; Park, Katharine; Daston, Lorraine (2006), "The Cambridge History of Science: Early modern science", Early Modern Science (Cambridge University Press) 3: 27, ISBN 0-521-57244-4
- Razani, Mohammad (2012), Information Communication and Space Technology, CRC Press, ISBN 1439841632
- Rauchfuss, Horst (2008), Chemical Evolution and the Origin of Life, Translated by T. N. Mitchell, Springer, ISBN 3-540-78822-0
- Schrijver, Carolus J.; Siscoe, George L. (2010), Heliophysics: Evolving Solar Activity and the Climates of Space and Earth, Cambridge University Press, ISBN 0-521-11294-X
- Silk, Joseph (2000), The Big Bang (3rd ed.), Macmillan, ISBN 0-8050-7256-X
- Sparke, Linda S.; Gallagher, John S. (2007), Galaxies in the Universe: An Introduction (2nd ed.), Cambridge University Press, ISBN 978-0-521-85593-8
- Stuart Wortley, Emmeline Charlotte E. (1841), The maiden of Moscow, a poem, How and Parsons, Canto X, section XIV, lines 14-15, "All Earth in madness moved,—o'erthrown, / To outer space—driven—racked—undone!"
- Thagard, Paul (1992), Conceptual revolutions, Princeton University Press, ISBN 0-691-02490-1
- Tassoul, Jean Louis; Tassoul, Monique (2004), A concise history of solar and stellar physics, Princeton University Press, ISBN 0-691-11711-X
- Tyson, Neil deGrasse; Goldsmith, Donald (2004), Origins: fourteen billion years of cosmic evolution, W. W. Norton & Company, pp. 114–115, ISBN 0-393-05992-8
- Von Humboldt, Alexander (1845), Cosmos: a survey of the general physical history of the Universe, New York: Harper & Brothers Publishers
- Webb, Stephen (1999), Measuring the universe: the cosmological distance ladder, Springer, ISBN 1-85233-106-2
- Wong, Wilson; Fergusson, James Gordon (2010), Military space power: a guide to the issues, Contemporary military, strategic, and security issues, ABC-CLIO, ISBN 0-313-35680-7
|Find more about Space at Wikipedia's sister projects|
|Definitions and translations from Wiktionary|
|Media from Commons|
|Learning resources from Wikiversity|
|Quotations from Wikiquote|
|Source texts from Wikisource|
|Textbooks from Wikibooks|