History of the center of the Universe
Historically, the center of the Universe had been believed to be a number of locations. Many mythological cosmologies included an axis mundi, the central axis of a flat Earth that connects the Earth, heavens, and other realms together. In the 4th century BCE Greece, the geocentric model was developed based on astronomical observation, proposing that the center of the Universe lies at the center of a spherical, stationary Earth, around which the Sun, Moon, planets, and stars rotate. With the development of the heliocentric model by Nicolaus Copernicus in the 16th century, the Sun was believed to be the center of the Universe, with the planets (including Earth) and stars orbiting it.
In the early 20th century, the discovery of other galaxies and the development of the Big Bang theory led to the development of cosmological models of a homogeneous, isotropic Universe (which lacks a central point) that is expanding at all points.
In religion or mythology, the axis mundi (also cosmic axis, world axis, world pillar, columna cerului, center of the world) is a point described as the center of the world, the connection between it and Heaven, or both.
Mount Hermon was regarded as the axis mundi in Caananite tradition, from where the sons of God are introduced descending in 1 Enoch (1En6:6). The ancient Greeks regarded several sites as places of earth's omphalos (navel) stone, notably the oracle at Delphi, while still maintaining a belief in a cosmic world tree and in Mount Olympus as the abode of the gods. Judaism has the Temple Mount and Mount Sinai, Christianity has the Mount of Olives and Calvary, Islam has Mecca, said to be the place on earth that was created first, and the Temple Mount (Dome of the Rock). In Shinto, the Ise Shrine is the omphalos. In addition to the Kun Lun Mountains, where it is believed the peach tree of immortality is located, the Chinese folk religion recognizes four other specific mountains as pillars of the world.
Sacred places constitute world centers (omphalos) with the altar or place of prayer as the axis. Altars, incense sticks, candles and torches form the axis by sending a column of smoke, and prayer, toward heaven. The architecture of sacred places often reflects this role. "Every temple or palace--and by extension, every sacred city or royal residence--is a Sacred Mountain, thus becoming a Centre." The stupa of Hinduism, and later Buddhism, reflects Mount Meru. Cathedrals are laid out in the form of a cross, with the vertical bar representing the union of Earth and heaven as the horizontal bars represent union of people to one another, with the altar at the intersection. Pagoda structures in Asian temples take the form of a stairway linking earth and heaven. A steeple in a church or a minaret in a mosque also serve as connections of Earth and heaven. Structures such as the maypole, derived from the Saxons' Irminsul, and the totem pole among indigenous peoples of the Americas also represent world axes. The calumet, or sacred pipe, represents a column of smoke (the soul) rising form a world center. A mandala creates a world center within the boundaries of its two-dimensional space analogous to that created in three-dimensional space by a shrine.
In medieval times some Christians thought of Jerusalem as the center of the world (Latin: umbilicus mundi, Greek: Omphalos), and was so represented in the so-called T and O maps. Byzantine hymns speak of the Cross being "planted in the center of the earth."
Center of a flat EarthEdit
The Flat Earth model is a belief that the Earth's shape is a plane or disk covered by a firmament containing heavenly bodies. Most pre-scientific cultures have had conceptions of a Flat Earth, including Greece until the classical period, the Bronze Age and Iron Age civilizations of the Near East until the Hellenistic period, India until the Gupta period (early centuries AD) and China until the 17th century. It was also typically held in the aboriginal cultures of the Americas, and a flat Earth domed by the firmament in the shape of an inverted bowl is common in pre-scientific societies.
"Center" is well-defined in a Flat Earth model. A flat Earth would have a definite geographic center. There would also be a unique point at the exact center of a spherical firmament (or a firmament that was a half-sphere).
Earth as the center of the UniverseEdit
The Flat Earth model gave way to an understanding of a Spherical Earth. Aristotle (384–322 BCE) provided observational arguments supporting the idea of a spherical Earth, namely that different stars are visible in different locations, travelers going south see southern constellations rise higher above the horizon, and the shadow of Earth on the Moon during a lunar eclipse is round, and spheres cast circular shadows while discs generally do not.
This understanding was accompanied by models of the Universe that depicted the Sun, Moon, stars, and naked eye planets circling the spherical Earth, including the noteworthy models of Aristotle (see Aristotelian physics) and Ptolemy. This geocentric model was the dominant model from the 4th century BCE until the 17th century CE.
Sun as center of the UniverseEdit
Heliocentrism, or heliocentricism,[note 1] is the astronomical model in which the Earth and planets revolve around a relatively stationary Sun at the center of our Solar System. The word comes from the Greek (ἥλιος helios "sun" and κέντρον kentron "center").
The notion that the Earth revolves around the Sun had been proposed as early as the 3rd century BCE by Aristarchus of Samos,[note 2] but had received no support from most other ancient astronomers.
Nicolaus Copernicus' major theory of a heliocentric model was published in De revolutionibus orbium coelestium (On the Revolutions of the Celestial Spheres), in 1543, the year of his death, though he had formulated the theory several decades earlier. Copernicus' ideas were not immediately accepted, but they did begin a paradigm shift away from the Ptolemaic geocentric model to a heliocentric model. The Copernican revolution, as this paradigm shift would come to be called, would last until Isaac Newton’s work over a century later.
Johannes Kepler published his first two laws about planetary motion in 1609, having found them by analyzing the astronomical observations of Tycho Brahe. Kepler's third law was published in 1619. The first law was "The orbit of every planet is an ellipse with the Sun at one of the two foci."
On 7 January 1610 Galileo used his telescope, with optics superior to what had been available before. He described "three fixed stars, totally invisible by their smallness", all close to Jupiter, and lying on a straight line through it. Observations on subsequent nights showed that the positions of these "stars" relative to Jupiter were changing in a way that would have been inexplicable if they had really been fixed stars. On 10 January Galileo noted that one of them had disappeared, an observation which he attributed to its being hidden behind Jupiter. Within a few days he concluded that they were orbiting Jupiter: Galileo stated that he had reached this conclusion on 11 January. He had discovered three of Jupiter's four largest satellites (moons). He discovered the fourth on 13 January.
His observations of the satellites of Jupiter created a revolution in astronomy: a planet with smaller planets orbiting it did not conform to the principles of Aristotelian Cosmology, which held that all heavenly bodies should circle the Earth, and many astronomers and philosophers initially refused to believe that Galileo could have discovered such a thing.[clarification needed]
Newton made clear his heliocentric view of the Solar System – developed in a somewhat modern way, because already in the mid-1680s he recognised the "deviation of the Sun" from the centre of gravity of the solar system. For Newton, it was not precisely the centre of the Sun or any other body that could be considered at rest, but rather "the common centre of gravity of the Earth, the Sun and all the Planets is to be esteem'd the Centre of the World", and this centre of gravity "either is at rest or moves uniformly forward in a right line" (Newton adopted the "at rest" alternative in view of common consent that the centre, wherever it was, was at rest).
Milky Way's galactic center as center of the UniverseEdit
Before the 1920s, it was generally believed that there were no galaxies other than our own (see for example The Great Debate). Thus, to astronomers of previous centuries, there was no distinction between a hypothetical center of the galaxy and a hypothetical center of the universe.
In 1750 Thomas Wright, in his work An original theory or new hypothesis of the Universe, correctly speculated that the Milky Way might be a body of a huge number of stars held together by gravitational forces rotating about a Galactic Center, akin to the Solar System but on a much larger scale. The resulting disk of stars can be seen as a band on the sky from our perspective inside the disk. In a treatise in 1755, Immanuel Kant elaborated on Wright's idea about the structure of the Milky Way.
The nonexistence of a center of the UniverseEdit
In 1917, Heber Doust Curtis observed a nova within what then was called the "Andromeda Nebula". Searching the photographic record, 11 more novae were discovered. Curtis noticed that novas in Andromeda were drastically fainter than novas in the Milky Way. Based on this, Curtis was able to estimate that Andromeda was 500,000 light-years away. As a result, Curtis became a proponent of the so-called "island Universes" hypothesis, which held that objects previously believed to be spiral nebulae within the Milky Way were actually independent galaxies.
In 1920, the Great Debate between Harlow Shapley and Curtis took place, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the Universe. To support his claim that the Great Andromeda Nebula (M31) was an external galaxy, Curtis also noted the appearance of dark lanes resembling the dust clouds in our own galaxy, as well as the significant Doppler shift. In 1922 Ernst Öpik presented an elegant and simple astrophysical method to estimate the distance of M31. His result put the Andromeda Nebula far outside our galaxy at a distance of about 450,000 parsec, which is about 1,500,000 ly. Edwin Hubble settled the debate about whether other galaxies exist in 1925 when he identified extragalactic Cepheid variable stars for the first time on astronomical photos of M31. These were made using the 2.5 metre (100 in) Hooker telescope, and they enabled the distance of Great Andromeda Nebula to be determined. His measurement demonstrated conclusively that this feature was not a cluster of stars and gas within our galaxy, but an entirely separate galaxy located a significant distance from our own. This proved the existence of other galaxies.
Hubble also demonstrated that the redshift of other galaxies is approximately proportional to their distance from the Earth (Hubble's law). This raised the appearance of our galaxy being in the center of an expanding Universe, however, Hubble rejected the findings philosophically:
...if we see the nebulae all receding from our position in space, then every other observer, no matter where he may be located, will see the nebulae all receding from his position. However, the assumption is adopted. There must be no favoured location in the Universe, no centre, no boundary; all must see the Universe alike. And, in order to ensure this situation, the cosmologist, postulates spatial isotropy and spatial homogeneity, which is his way of stating that the Universe must be pretty much alike everywhere and in all directions."
The redshift observations of Hubble, in which galaxies appear to be moving away from us at a rate proportional to their distance from us, are now understood to be a result of the metric expansion of space. This is the increase of the distance between two distant parts of the Universe with time, and is an intrinsic expansion whereby the scale of space itself changes. As Hubble theorized, all observers anywhere in the Universe will observe a similar effect.
Copernican and cosmological principlesEdit
The Copernican principle, named after Nicolaus Copernicus, states that the Earth is not in a central, specially favored position. Hermann Bondi named the principle after Copernicus in the mid-20th century, although the principle itself dates back to the 16th-17th century paradigm shift away from the geocentric Ptolemaic system.
The cosmological principle is an extension of the Copernican principle which states that the Universe is homogeneous (the same observational evidence is available to observers at different locations in the Universe) and isotropic (the same observational evidence is available by looking in any direction in the Universe). A homogeneous, isotropic Universe does not have a center.
- Copernican heliocenterism held that the Sun itself was the center of the entire Universe. As it is modernly understood, Heliocenterism refers to the much narrower concept that the Sun is the center of the Solar System, not the center of the entire Universe.
- The work of Aristarchus's in which he proposed his heliocentric system has not survived. We only know of it now from a brief passage in Archimedes's The Sand Reckoner.
- Kelley Coblentz Bautch (25 September 2003). A Study of the Geography of 1 Enoch 17-19: "no One Has Seen what I Have Seen". BRILL. pp. 62–. ISBN 9789004131033. Retrieved 28 June 2011.
- Mircea Eliade (tr. Willard Trask). 'Archetypes and Repetition' in The Myth of the Eternal Return. Princeton, 1971. p.12
- Jean Chevalier and Alain Gheerbrandt. The Penguin Dictionary of Symbols. Editions Robert Lafont S. A. et Editions Jupiter: Paris, 1982. Penguin Books: London, 1996. pp.148-149
- Mircea Eliade (tr. Philip Mairet). 'Symbolism of the Centre' in Images and Symbols. Princeton, 1991. p.52-54
- "Their cosmography as far as we know anything about it was practically of one type up til the time of the white man's arrival upon the scene. That of the Borneo Dayaks may furnish us with some idea of it. 'They consider the Earth to be a flat surface, whilst the heavens are a dome, a kind of glass shade which covers the Earth and comes in contact with it at the horizon.'" Lucien Levy-Bruhl, Primitive Mentality (repr. Boston: Beacon, 1966) 353; "The usual primitive conception of the world's form ... [is] flat and round below and surmounted above by a solid firmament in the shape of an inverted bowl." H. B. Alexander, The Mythology of All Races 10: North American (repr. New York: Cooper Square, 1964) 249.
- Lawson, Russell M. (2004). Science in the ancient world: an encyclopedia. ABC-CLIO. pp. 29–30. ISBN 978-1851095346. Retrieved 2 October 2009.
- Teaching about Evolution and the Nature of Science (National Academy of Sciences, 1998), p.27; also, Don O' Leary, Roman Catholicism and Modern Science: A History (Continuum Books, 2006), p.5.
- Dreyer, J.L.E. (1906). History of the planetary systems from Thales to Kepler. Cambridge University Press. pp. 135–48.
- Linton, C.M. (2004). From Eudoxus to Einstein: A History of Mathematical Astronomy. E-Libro. Cambridge University Press. p. 38,205. ISBN 9781139453790.
- Holton, Gerald James; Brush, Stephen G. (2001). Physics, the Human Adventure: From Copernicus to Einstein and Beyond (3rd paperback ed.). Piscataway, NJ: Rutgers University Press. pp. 40–41. ISBN 978-0-8135-2908-0. Retrieved December 27, 2009.
- i.e., invisible to the naked eye.
- Drake, Stillman (1978). Galileo at Work: His Scientific Biography. University of Chicago Press. pp. 146, 152, 157–163.
- In Sidereus Nuncius,1892, 3:81 (in Latin)
- Linton, C.M. (2004). From Eudoxus to Einstein: A History of Mathematical Astronomy. E-Libro. Cambridge University Press. p. 38. ISBN 9781139453790.
- See Curtis Wilson, "The Newtonian achievement in astronomy", pages 233–274 in R Taton & C Wilson (eds) (1989) The General History of Astronomy, Volume, 2A', at page 233.
- Text quotations are from 1729 translation of Newton's Principia, Book 3 (1729 vol.2) at pages 232–233.
- Evans, J. C. (1995). "Our Galaxy". Retrieved 25 April 2012.
- Curtis, H. D. (1988). "Novae in Spiral Nebulae and the Island Universe Theory". Publications of the Astronomical Society of the Pacific. 100: 6. Bibcode:1988PASP..100....6C. doi:10.1086/132128.
- Öpik, E. (1922). "An estimate of the distance of the Andromeda Nebula". Astrophysical Journal. 55: 406–410. Bibcode:1922ApJ....55..406O. doi:10.1086/142680.
- Hubble, E. P. (1929). "A spiral nebula as a stellar system, Messier 31". Astrophysical Journal. 69: 103–158. Bibcode:1929ApJ....69..103H. doi:10.1086/143167.
- Hubble, E. P. (1937). The observational approach to cosmology. Oxford University Press.
- H. Bondi (1952). Cosmology. Cambridge University Press. p. 13.
- Livio, Mario (2001). The Accelerating Universe: Infinite Expansion, the Cosmological Constant, and the Beauty of the Cosmos. John Wiley and Sons. p. 53. ISBN 9780471437147. Retrieved 31 March 2012.