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Earth's rotation
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For the duration of daylight and night, see Daytime and Night.
An animation of Earth's rotation around the planet's axis
This long-exposure photo of the northern night sky over the Nepali Himalayas shows the apparent paths of the stars as Earth rotates.
Earth's rotation is the rotation of Planet Earth around its own axis. Earth rotates eastward, in prograde motion. As viewed from the north pole star Polaris, Earth turns counter clockwise.
The North Pole, also known as the Geographic North Pole or Terrestrial North Pole, is the point in the Northern Hemisphere where Earth's axis of rotation meets its surface. This point is distinct from Earth's North Magnetic Pole. The South Pole is the other point where Earth's axis of rotation intersects its surface, in Antarctica.
Earth rotates once in about 24 hours with respect to the Sun, but once every 23 hours, 56 minutes, and 4 seconds with respect to the stars (see below). Earth's rotation is slowing slightly with time; thus, a day was shorter in the past. This is due to the tidal effects the Moon has on Earth's rotation. Atomic clocks show that a modern day is longer by about 1.7 milliseconds than a century ago,[1] slowly increasing the rate at which UTC is adjusted by leap seconds. Analysis of historical astronomical records shows a slowing trend of about 2.3 milliseconds per century since the 8th century BCE.[2]
Contents
1 History
1.1 Empirical tests
2 Periods
2.1 True solar day
2.2 Mean solar day
2.3 Stellar and sidereal day
2.4 Angular speed
3 Changes
3.1 In rotational axis
3.2 In rotational velocity
3.2.1 Tidal interactions
3.2.2 Resonant stabilization
3.2.3 Global events
3.3 Measurement
3.4 Ancient observations
4 Origin
5 See also
6 Notes
7 References
8 External links
History[edit]
Among the ancient Greeks, several of the Pythagorean school believed in the rotation of the earth rather than the apparent diurnal rotation of the heavens. Perhaps the first was Philolaus (470–385 BCE), though his system was complicated, including a counter-earth rotating daily about a central fire.[3]
A more conventional picture was that supported by Hicetas, Heraclides and Ecphantus in the fourth century BCE who assumed that the earth rotated but did not suggest that the earth revolved about the sun. In the third century BCE, Aristarchus of Samos suggested the sun's central place.
However, Aristotle in the fourth century BCE criticized the ideas of Philolaus as being based on theory rather than observation. He established the idea of a sphere of fixed stars that rotated about the earth.[4] This was accepted by most of those who came after, in particular Claudius Ptolemy (2nd century CE), who thought the earth would be devastated by gales if it rotated.[5]
In 499 CE, the Indian astronomer Aryabhata wrote that the spherical earth rotates about its axis daily, and that the apparent movement of the stars is a relative motion caused by the rotation of the Earth. He provided the following analogy: "Just as a man in a boat going in one direction sees the stationary things on the bank as moving in the opposite direction, in the same way to a man at Lanka the fixed stars appear to be going westward."[6][7]
In the 10th century, some Muslim astronomers accepted that the Earth rotates around its axis.[8] According to al-Biruni, Abu Sa'id al-Sijzi (d. circa 1020) invented an astrolabe called al-zūraqī based on the idea believed by some of his contemporaries "that the motion we see is due to the Earth's movement and not to that of the sky."[9][10] The prevalence of this view is further confirmed by a reference from the 13th century which states: "According to the geometers [or engineers] (muhandisīn), the earth is in constant circular motion, and what appears to be the motion of the heavens is actually due to the motion of the earth and not the stars."[9] Treatises were written to discuss its possibility, either as refutations or expressing doubts about Ptolemy's arguments against it.[11] At the Maragha and Samarkand observatories, the Earth's rotation was discussed by Tusi (b. 1201) and Qushji (b. 1403); the arguments and evidence they used resemble those used by Copernicus.[12]
In medieval Europe, Thomas Aquinas accepted Aristotle's view[13] and so, reluctantly, did John Buridan[14] and Nicole Oresme[15] in the fourteenth century. Not until Nicolaus Copernicus in 1543 adopted a heliocentric world system did the contemporary understanding of earth's rotation begin to be established. Copernicus pointed out that if the movement of the earth is violent, then the movement of the stars must be very much more so. He acknowledged the contribution of the Pythagoreans and pointed to examples of relative motion. For Copernicus this was the first step in establishing the simpler pattern of planets circling a central sun.[16]
Tycho Brahe, who produced accurate observations on which Kepler based his laws, used Copernicus's work as the basis of a system assuming a stationary earth. In 1600, William Gilbert strongly supported the earth's rotation in his treatise on the earth's magnetism[17] and thereby influenced many of his contemporaries.[18] Those like Gilbert who did not openly support or reject the motion of the earth about the sun are often called "semi-Copernicans".[19] A century after Copernicus, Riccioli disputed the model of a rotating earth due to the lack of then-observable eastward deflections in falling bodies;[20] such deflections would later be called the Coriolis effect. However, the contributions of Kepler, Galileo and Newton gathered support for the theory of the rotation of the Earth.
Empirical tests[edit]
The earth's rotation implies that the equator bulges and the poles are flattened. In his Principia, Newton predicted this flattening would occur in the ratio of 1:230, and pointed to the 1673 pendulum measurements by Richer as corroboration of the change in gravity,[21] but initial measurements of meridian lengths by Picard and Cassini at the end of the 17th century suggested the opposite. However measurements by Maupertuis and the French Geodesic Mission in the 1730s established the flattening, thus confirming both Newton and the Copernican position.[22]
In the Earth's rotating frame of reference, a freely moving body follows an apparent path that deviates from the one it would follow in a fixed frame of reference. Because of the Coriolis effect, falling bodies veer slightly eastward from the vertical plumb line below their point of release, and projectiles veer right in the northern hemisphere (and left in the southern) from the direction in which they are shot. The Coriolis effect is mainly observable at a meteorological scale, where it is responsible for the differing rotation direction of cyclones in the northern and southern hemispheres.
Hooke, following a 1679 suggestion from Newton, tried unsuccessfully to verify the predicted eastward deviation of a body dropped from a height of 8.2 meters, but definitive results were only obtained later, in the late 18th and early 19th century, by Giovanni Battista Guglielmini in Bologna, Johann Friedrich Benzenberg in Hamburg and Ferdinand Reich in Freiberg, using taller towers and carefully released weights.[n 1] A ball dropped from a height of 158.5 m (520 ft) departed by 27.4 mm (1.08 in) from the vertical compared with a calculated value of 28.1 mm (1.11 in).
The most celebrated test of Earth's rotation is the Foucault pendulum first built by physicist Léon Foucault in 1851, which consisted of a lead-filled brass sphere suspended 67 m from the top of the Panthéon in Paris. Because of the Earth's rotation under the swinging pendulum, the pendulum's plane of oscillation appears to rotate at a rate depending on latitude. At the latitude of Paris the predicted and observed shift was about 11 degrees clockwise per hour. Foucault pendulums now swing in museums around the world.
Periods [edit]
Starry circles arc around the south celestial pole, seen overhead at ESO's La Silla Observatory.[23]
True solar day[edit]
Main article: Solar time
Earth's rotation period relative to the Sun (solar noon to solar noon) is its true solar day or apparent solar day. It depends on the Earth's orbital motion and is thus affected by changes in the eccentricity and inclination of Earth's orbit. Both vary over thousands of years, so the annual variation of the true solar day also varies. Generally, it is longer than the mean solar day during two periods of the year and shorter during another two.[n 2] The true solar day tends to be longer near perihelion when the Sun apparently moves along the ecliptic through a greater angle than usual, taking about 10 seconds longer to do so. Conversely, it is about 10 seconds shorter near aphelion. It is about 20 seconds longer near a solstice when the projection of the Sun's apparent motion along the ecliptic onto the celestial equator causes the Sun to move through a greater angle than usual. Conversely, near an equinox the projection onto the equator is shorter by about 20 seconds. Currently, the perihelion and solstice effects combine to lengthen the true solar day near 22 December by 30 mean solar seconds, but the solstice effect is partially cancelled by the aphelion effect near 19 June when it is only 13 seconds longer. The effects of the equinoxes shorten it near 26 March and 16 September by 18 seconds and 21 seconds, respectively.[24][25][26]
Mean solar day[edit]
Main article: Solar time § Mean solar time
The average of the true solar day during the course of an entire year is the mean solar day, which contains 86,400 mean solar seconds. Currently, each of these seconds is slightly longer than an SI second because Earth's mean solar day is now slightly longer than it was during the 19th century due to tidal friction. The average length of the mean solar day since the introduction of the leap second in 1972 has been about 0 to 2 ms longer than 86,400 SI seconds.[27][28][29] Random fluctuations due to core-mantle coupling have an amplitude of about 5 ms.[30][31] The mean solar second between 1750 and 1892 was chosen in 1895 by Simon Newcomb as the independent unit of time in his Tables of the Sun. These tables were used to calculate the world's ephemerides between 1900 and 1983, so this second became known as the ephemeris second. In 1967 the SI second was made equal to the ephemeris second.[32]
The apparent solar time is a measure of the Earth's rotation and the difference between it and the mean solar time is known as the equation of time.
Stellar and sidereal day[edit]
On a prograde planet like the Earth, the stellar day is shorter than the solar day. At time 1, the Sun and a certain distant star are both overhead. At time 2, the planet has rotated 360° and the distant star is overhead again but the Sun is not (1→2 = one stellar day). It is not until a little later, at time 3, that the Sun is overhead again (1→3 = one solar day).
Earth's rotation period relative to the fixed stars, called its stellar day by the International Earth Rotation and Reference Systems Service (IERS), is 86,164.098 903 691 seconds of mean solar time (UT1) (23h 56m 4.098 903 691s, 0.997 269 663 237 16 mean solar days).[33][n 3] Earth's rotation period relative to the precessing or moving mean vernal equinox, named sidereal day, is 86,164.090 530 832 88 seconds of mean solar time (UT1) (23h 56m 4.090 530 832 88s, 0.997 269 566 329 08 mean solar days).[33] Thus the sidereal day is shorter than the stellar day by about 8.4 ms.[35]
Both the stellar day and the sidereal day are shorter than the mean solar day by about 3 minutes 56 seconds. The mean solar day in SI seconds is available from the IERS for the periods 1623–2005[36] and 1962–2005.[37]
Recently (1999–2010) the average annual length of the mean solar day in excess of 86,400 SI seconds has varied between 0.25 ms and 1 ms, which must be added to both the stellar and sidereal days given in mean solar time above to obtain their lengths in SI seconds (see Fluctuations in the length of day).
Angular speed[edit]
Plot of latitude vs tangential speed. The dashed line shows that the Kennedy Space Center example. The dot-dash line denotes typical airliner cruise speed.
The angular speed of Earth's rotation in inertial space is (7.2921150 ± 0.0000001) ×10−5 radians per SI second (mean solar second).[33] Multiplying by (180°/π radians)×(86,400 seconds/mean solar day) yields 360.9856°/mean solar day, indicating that Earth rotates more than 360° relative to the fixed stars in one solar day. Earth's movement along its nearly circular orbit while it is rotating once around its axis requires that Earth rotate slightly more than once relative to the fixed stars before the mean Sun can pass overhead again, even though it rotates only once (360°) relative to the mean Sun.[n 4] Multiplying the value in rad/s by Earth's equatorial radius of 6,378,137 m (WGS84 ellipsoid) (factors of 2π radians needed by both cancel) yields an equatorial speed of 465.1 m/s (1,526 ft/s), or 1,674.4 km/h (1,040.4 mph).[38] Some sources state that Earth's equatorial speed is slightly less, or 1,669.8 km/h.[39] This is obtained by dividing Earth's equatorial circumference by 24 hours. However, the use of only one circumference unwittingly implies only one rotation in inertial space, so the corresponding time unit must be a sidereal hour. This is confirmed by multiplying by the number of sidereal days in one mean solar day, 1.002 737 909 350 795,[33] which yields the equatorial speed in mean solar hours given above of 1,674.4 km/h.
The tangential speed of Earth's rotation at a point on Earth can be approximated by multiplying the speed at the equator by the cosine of the latitude.[40] For example, the Kennedy Space Center is located at latitude 28.59° N, which yields a speed of: cos 28.59° × 1,674.4 km/h (1,040.4 mph; 465.1 m/s) = 1,470.23 km/h (913.56 mph; 408.40 m/s)
Changes[edit]
Main articles: Fluctuations in the length of day and ΔT
Earth's axial tilt is about 23.4°. It oscillates between 22.1° and 24.5° on a 41,000-year cycle and is currently decreasing.
In rotational axis[edit]
The Earth's rotation axis moves with respect to the fixed stars (inertial space); the components of this motion are precession and nutation. It also moves with respect to the Earth's crust; this is called polar motion.
Precession is a rotation of the Earth's rotation axis, caused primarily by external torques from the gravity of the Sun, Moon and other bodies. The polar motion is primarily due to free core nutation and the Chandler wobble.
In rotational velocity[edit]
Tidal interactions[edit]
Over millions of years, the Earth's rotation slowed significantly by tidal acceleration through gravitational interactions with the Moon. In this process, angular momentum is slowly transferred to the Moon at a rate proportional to r − 6 {\displaystyle r^{-6}} , where r {\displaystyle r} is the orbital radius of the Moon. This process gradually increased the length of day to its current value and resulted in the Moon being tidally locked with the Earth.
This gradual rotational deceleration is empirically documented with estimates of day lengths obtained from observations of tidal rhythmites and stromatolites; a compilation of these measurements[41] found the length of day to increase steadily from about 21 hours at 600Myr ago[42] to the current 24 hour value. By counting the microscopic lamina that form at higher tides, tidal frequencies (and thus day lengths) can be estimated, much like counting tree rings, though these estimates can be increasingly unreliable at older ages.[43]
Resonant stabilization[edit]
The current rate of tidal deceleration is anomalously high, implying the Earth's rotational velocity must have decreased more slowly in the past. Empirical data[41] tentatively shows a sharp increase in rotational deceleration about 600Myr ago. Some models suggest that the Earth maintained a constant day length of 21 hours throughout much of the Precambrian.[42] This day length corresponds to the semidiurnal resonant period of the thermally-driven atmospheric tide; at this day length, the decelerative lunar torque could have been canceled by an accelerative torque from the atmospheric tide, resulting in no net torque and a constant rotational period. This stabilizing effect could have been broken by a sudden change in global temperature. Recent computational simulations support this hypothesis and suggest the Marinoan or Sturtian glaciations broke this stable configuration about 600Myr ago, citing the resemblance of simulated results and existing paleorotational data.[44]
Deviation of day length from SI based day
Global events[edit]
Additionally, some large-scale events, such as the 2004 Indian Ocean earthquake, have caused the length of a day to shorten by 3 microseconds by affecting the Earth's moment of inertia.[45] Post-glacial rebound, ongoing since the last Ice age, is also changing the distribution of the Earth's mass thus affecting the moment of inertia of the Earth and, by the conservation of angular momentum, the Earth's rotation period.[46]
Measurement[edit]
The primary monitoring of the Earth's rotation is performed with very-long-baseline interferometry coordinated with the Global Positioning System, satellite laser ranging, and other satellite techniques. This provides an absolute reference for the determination of universal time, precession, and nutation.[47]
Ancient observations[edit]
There are recorded observations of solar and lunar eclipses by Babylonian and Chinese astronomers beginning in the 8th century BCE, as well as from the medieval Islamic world and elsewhere. These observations can be used to determine changes in the Earth's rotation over the last 27 centuries, since the length of the day is a critical parameter in the calculation of the place and time of eclipses. A change in day length of milliseconds per century shows up as a change of hours and thousands of kilometers in eclipse observations. The ancient data is consistent with a shorter day, meaning the Earth was turning faster throughout the past.[48][49]
Origin[edit]
An artist's rendering of the protoplanetary disk.
The Earth's original rotation was a vestige of the original angular momentum of the cloud of dust, rocks, and gas that coalesced to form the Solar System. This primordial cloud was composed of hydrogen and helium produced in the Big Bang, as well as heavier elements ejected by supernovas. As this interstellar dust is heterogeneous, any asymmetry during gravitational accretion resulted in the angular momentum of the eventual planet.[50]
However, if the giant-impact hypothesis for the origin of the Moon is correct, this primordial rotation rate would have been reset by the Theia impact 4.5 billion years ago. Regardless of the speed and tilt of the Earth's rotation before the impact, it would have experienced a day some five hours long after the impact.[51] Tidal effects would then have slowed this rate to its modern value.
See also[edit]
Allais effect
Axial precession
Diurnal cycle
Earth's orbit
Formation and evolution of the Solar System
Geodesic (in mathematics)
Geodesics in general relativity
Geodesy
Giant-impact hypothesis
History of Earth
History of geodesy, Space techniques
List of important publications in geology
Newcomb's Tables of the Sun
Nychthemeron
Spherical Earth
World Geodetic System
Notes[edit]
Jump up ^ See Fallexperimente zum Nachweis der Erdrotation (German Wikipedia article).
Jump up ^ When Earth's eccentricity exceeds 0.047 and perihelion is at an appropriate equinox or solstice, only one period with one peak balances another period that has two peaks.[24]
Jump up ^ Aoki, the ultimate source of these figures, uses the term "seconds of UT1" instead of "seconds of mean solar time".[34]
Jump up ^ In astronomy, unlike geometry, 360° means returning to the same point in some cyclical time scale, either one mean solar day or one sidereal day for rotation on Earth's axis, or one sidereal year or one mean tropical year or even one mean Julian year containing exactly 365.25 days for revolution around the Sun.
References[edit]
Jump up ^ Dennis D. McCarthy; Kenneth P. Seidelmann (18 September 2009). Time: From Earth Rotation to Atomic Physics. John Wiley & Sons. p. 232. ISBN 978-3-527-62795-0.
Jump up ^ Stephenson, F. Richard (2003). "Historical eclipses and Earth's rotation". Astronomy & Geophysics. 44 (2). pp. 2.22–2.27. Bibcode:2003A&G....44b..22S. doi:10.1046/j.1468-4004.2003.44222.x.
Jump up ^ Burch, George Bosworth (1954). "The Counter-Earth". Osiris. 11: 267–294. doi:10.1086/368583. JSTOR 301675.
Jump up ^ Aristotle. Of the Heavens. Book II, Ch 13. 1.
Jump up ^ Ptolemy. Almagest Book I, Chapter 8.
Jump up ^ http://www.new1.dli.ernet.in/data1/upload/insa/INSA_1/20005b61_51.pdf
Jump up ^ Kim Plofker (2009). Mathematics in India. Princeton University Press. p. 71. ISBN 0-691-12067-6.
Jump up ^ Alessandro Bausani (1973). "Cosmology and Religion in Islam". Scientia/Rivista di Scienza. 108 (67): 762.
^ Jump up to: a b Young, M. J. L., ed. (2 November 2006). Religion, Learning and Science in the 'Abbasid Period. Cambridge University Press. p. 413. ISBN 9780521028875.
Jump up ^ Nasr, Seyyed Hossein (1 January 1993). An Introduction to Islamic Cosmological Doctrines. SUNY Press. p. 135. ISBN 9781438414195.
Jump up ^ Ragep, Sally P. (2007). "Ibn Sīnā: Abū ʿAlī al‐Ḥusayn ibn ʿAbdallāh ibn Sīnā". In Thomas Hockey; et al. The Biographical Encyclopedia of Astronomers. New York: Springer. pp. 570–2. ISBN 978-0-387-31022-0. (PDF version)
Jump up ^ Ragep, F. Jamil (2001a), "Tusi and Copernicus: The Earth's Motion in Context", Science in Context, Cambridge University Press, 14 (1–2): 145–163, doi:10.1017/s0269889701000060
Jump up ^ Aquinas, Thomas. Commentaria in libros Aristotelis De caelo et Mundo. Lib II, cap XIV. trans in Grant, Edward, ed. (1974). A Source Book in Medieval Science. Harvard University Press. pages 496–500
Jump up ^ Buridan, John (1942). Quaestiones super libris quattuo De Caelo et mundo. pp. 226–232. in Grant 1974, pp. 500–503
Jump up ^ Oresme, Nicole. Le livre du ciel et du monde. pp. 519–539. in Grant 1974, pp. 503–510
Jump up ^ Copernicus, Nicolas. On the Revolutions of the Heavenly Spheres. Book I, Chap 5–8.
Jump up ^ Gilbert, William. De Magnete, On the Magnet and Magnetic Bodies, and on the Great Magnet the Earth. pp. 313–347.
Jump up ^ Russell, John L. "Copernican System in Great Britain". In J. Dobrzycki. The Reception of Copernicus' Heliocentric Theory. p. 208.
Jump up ^ J. Dobrzycki 1972, p. 221
Jump up ^ Almagestum novum, chapter nine, cited in Graney, Christopher M. (2012). "126 arguments concerning the motion of the earth. GIOVANNI BATTISTA RICCIOLI in his 1651 ALMAGESTUM NOVUM" (PDF). Journal for the History of Astronomy. volume 43, pages 215–226.
Jump up ^ Newton, Isaac (1846). Newton's Principia. Translated by A. Motte. p. 412.
Jump up ^ Shank, J. B. (2008). The Newton Wars and the Beginning of the French Enlightenment. U of Chicago Press. pp. 324, 355.
Jump up ^ "Starry Spin-up". Retrieved 24 August 2015.
^ Jump up to: a b Jean Meeus; J. M. A. Danby (January 1997). Mathematical Astronomy Morsels. Willmann-Bell. pp. 345–346. ISBN 978-0-943396-51-4.
Jump up ^ Equation of time in red and true solar day in blue
Jump up ^ The duration of the true solar day
Jump up ^ http://hpiers.obspm.fr/eoppc/eop/eopc04_05/eopc04.62-now
Jump up ^ Physical basis of leap seconds
Jump up ^ Leap seconds Archived 12 March 2015 at the Wayback Machine.
Jump up ^ Prediction of Universal Time and LOD Variations
Jump up ^ R. Hide et al., "Topographic core-mantle coupling and fluctuations in the Earth's rotation" 1993.
Jump up ^ Leap seconds by USNO Archived 12 March 2015 at the Wayback Machine.
^ Jump up to: a b c d IERS EOP Useful constants
Jump up ^ Aoki, et al., "The new definition of Universal Time", Astronomy and Astrophysics 105 (1982) 359–361.
Jump up ^ Explanatory Supplement to the Astronomical Almanac, ed. P. Kenneth Seidelmann, Mill Valley, Cal., University Science Books, 1992, p.48, ISBN 0-935702-68-7.
Jump up ^ IERS Excess of the duration of the day to 86,400s … since 1623 Archived 3 October 2008 at the Wayback Machine. Graph at end.
Jump up ^ IERS Variations in the duration of the day 1962–2005
Jump up ^ Arthur N. Cox, ed., Allen's Astrophysical Quantities p.244.
Jump up ^ Michael E. Bakich, The Cambridge planetary handbook, p.50.
Jump up ^ Butterworth & Palmer. "Speed of the turning of the Earth". Ask an Astrophysicist. NASA Goddard Spaceflight Center.
^ Jump up to: a b Williams, George E. (1 February 2000). "Geological constraints on the Precambrian history of Earth's rotation and the Moon's orbit". Reviews of Geophysics. 38 (1): 37–59. Bibcode:2000RvGeo..38...37W. doi:10.1029/1999RG900016. ISSN 1944-9208.
^ Jump up to: a b Zahnle, K.; Walker, J. C. (1 January 1987). "A constant daylength during the Precambrian era?". Precambrian Research. 37: 95–105. Bibcode:1987PreR...37...95Z. doi:10.1016/0301-9268(87)90073-8. ISSN 0301-9268. PMID 11542096.
Jump up ^ Scrutton, C. T. (1 January 1978). Brosche, Professor Dr Peter; Sündermann, Professor Dr Jürgen, eds. Periodic Growth Features in Fossil Organisms and the Length of the Day and Month. Springer Berlin Heidelberg. pp. 154–196. doi:10.1007/978-3-642-67097-8_12. ISBN 9783540090465.
Jump up ^ Bartlett, Benjamin C.; Stevenson, David J. (1 January 2016). "Analysis of a Precambrian resonance-stabilized day length". Geophysical Research Letters: 2016GL068912. arXiv:1502.01421  . Bibcode:2016GeoRL..43.5716B. doi:10.1002/2016GL068912. ISSN 1944-8007.
Jump up ^ Sumatran earthquake sped up Earth's rotation, Nature, 30 December 2004.
Jump up ^ Wu, P.; W.R.Peltier (1984). "Pleistocene deglaciation and the earth's rotation: a new analysis". Geophysical Journal of the Royal Astronomical Society. 76 (3): 753–792. Bibcode:1984GeoJ...76..753W. doi:10.1111/j.1365-246X.1984.tb01920.x.
Jump up ^ Permanent monitoring
Jump up ^ Sid Perkins (6 December 2016). "Ancient eclipses show Earth's rotation is slowing". Science. doi:10.1126/science.aa10469.
Jump up ^ FR Stephenson; LV Morrison; CY Hohonkerk (7 December 2016). "Measurement of the Earth's rotation: 720 BC to AD 2015". Proceedings of the Royal Society A. 472 (2196). Bibcode:2016RSPSA.47260404S. doi:10.1098/rspa.2016.0404. PMC 5247521  .
Jump up ^ "Why do planets rotate?". Ask an Astronomer.
Jump up ^ Stevenson, D. J. (1987). "Origin of the moon–The collision hypothesis". Annual Review of Earth and Planetary Sciences. 15 (1): 271–315. Bibcode:1987AREPS..15..271S. doi:10.1146/annurev.ea.15.050187.001415.
External links[edit]
USNO Earth Orientation new site, being populated
USNO IERS old site, to be abandoned
IERS Earth Orientation Center: Earth rotation data and interactive analysis
International Earth Rotation and Reference Systems Service (IERS)
If the Earth's rotation period is less than 24 hours, why don't our clocks fall out of sync with the Sun?
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The Hanged Man (Tarot card)
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The Hanged Man (XII)
The Hanged Man (XII) is the twelfth trump or Major Arcana card in most traditional Tarot decks. It is used in game playing as well as in divination.
It depicts a pittura infamante (pronounced [pitˈtuːra iɱfaˈmante]), an image of a man being hung upside-down by one ankle. This method of hanging was a common punishment at the time for traitors in Italy. However, the solemn expression on his face traditionally suggests that he is there by his own accord, and the card is meant to represent self-sacrifice more so than it does corporal punishment or criminality.
In other interpretations, The Hanged Man is a depiction of the Norse god Odin, who suspended himself from a tree in order to gain knowledge. There is also a Christian interpretation that portrays Judas, and include the bags of silver in his hands.

Description[edit]
A 1393 decree for Milan and Lombardy of the punishment for traitors: “Let him be drug [dragged] on a [wooden] plank at a horse’s tail to the place of execution, and there be suspended by one foot to the gallows, and be left there until he is dead. As long as he lives let him be given food and drink.”[1]
The Cross of St. Peter is shown in this French stained glass window. Saint Peter is conventionally shown as having been crucified upside-down.
Modern versions of the tarot deck depict a man hanging upside-down by one foot. The figure is most often suspended from a wooden beam (as in a cross or gallows) or a tree. Ambiguity results from the fact that the card itself may be viewed inverted.
In his book The Pictorial Key to the Tarot, A. E. Waite, the designer of the Rider-Waite tarot deck, wrote of the symbol:
The gallows from which he is suspended forms a Tau cross, while the figure—from the position of the legs—forms a fylfot cross. There is a nimbus about the head of the seeming martyr. It should be noted (1) that the tree of sacrifice is living wood, with leaves thereon; (2) that the face expresses deep entrancement, not suffering; (3) that the figure, as a whole, suggests life in suspension, but life and not death. [...] It has been called falsely a card of martyrdom, a card of prudence, a card of the Great Work, a card of duty [...] I will say very simply on my own part that it expresses the relation, in one of its aspects, between the Divine and the Universe.[2]
There is a halo burning brightly around the hanged man's head, signifying a higher learning or an enlightenment.[3]
References[edit]
Jump up ^ A Modern Catholic Looks at the Tarot, Pre-Gebelin Tarot History
Jump up ^ Waite, A. E. The Pictorial Key to the Tarot, ill. by Pamela Colman Smith [1911], at sacred-texts.com
Jump up ^ Gray, Eden. "Complete Guide to the Tarot." 1970. Crown Publishers, New York, NY.
Further reading[edit]
Wikimedia Commons has media related to Hanged Man (Major Arcana).
A. E. Waite's 1910 Pictorial Key to the Tarot
Hajo Banzhaf, Tarot and the Journey of the Hero (2000)
Wood, Juliette. (1998) "The Celtic Tarot and the Secret Tradition: A Study in Modern Legend Making". Folklore 109: 15–24
Francesca Lia Block, The Hanged Man (1999)
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Bernina International
From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
Bernina International AG
Type
Aktiengesellschaft
Industry
Sewing and embroidery systems
Founded
1893; 125 years ago (1893)
Founder
Fritz Gegauf
Headquarters
Steckborn, Switzerland
Area served
Worldwide
Key people
Hanspeter Ueltschi
(Owner and Chairman of the Board of Directors)[1]
Claude Dreyer (CEO)
Products
Bernina sewing machines
Textile machines
Software
Revenue
CHF 186 million (Consolidated net turnover 2016, of which 67% USA, 25% Europe, 8% other countries)
Owner
Hanspeter Ueltschi
Number of employees
1038 (Annual average for 2016, of which approx. 270 in Steckborn)
Website
www.bernina.com
Bernina International AG is a privately owned international manufacturer of sewing and embroidery systems. The company was founded in 1893 in Steckborn, Switzerland, by a Swiss inventor Fritz Gegauf. The company develops, manufactures, and sells goods and services for the textile market, primarily household sewing-related products in the fields of embroidery, quilting, home textiles, garment sewing, and crafting.[2] The origins of the company lie in the invention of the hemstitch sewing machine, invented in 1893 by a Swiss inventor and entrepreneur Karl Friedrich Gegauf. Currently, the company's products include sewing machines, embroidery machines, serger/overlocker machines, and computer software for embroidery design.
Contents
1 History
1.1 1890–1926: Karl Friedrich Gegauf and the invention of the hemstitch sewing machine
1.2 1926–1947: Fritz Gegauf and the development of the first Bernina household sewing machine
1.3 1959–1988: Odette Gegauf-Ueltschi and the fully automatic sewing machine
1.4 1988–2009: Hanspeter Ueltschi and the first sewing computer, expansion of markets and production
1.5 Present
2 Models
2.1 Timeline
2.2 Model ranges
3 Embroidery software
4 See also
5 References
6 Further reading
7 External links
History[edit]
Company founder Karl Friedrich Gegauf and his sons
Fritz Gegauf introduced the Bernina brand name in 1932.
Odette Ueltschi took charge of the company in 1965.
Hanspeter Ueltschi (right) and CEO Claude Dreyer launched the B830 model in 2008.
1890–1926: Karl Friedrich Gegauf and the invention of the hemstitch sewing machine[edit]
The present-day Bernina International AG was founded by Karl Friedrich Gegauf in 1893, when he decided to pursue an apprenticeship as a mechanic instead of studying medicine. After completing his apprenticeship, he worked in the Baum embroidery machine factory in Rorschach. In 1890, Karl Friedrich Gegauf set up his own business in Steckborn, Switzerland, opening an embroidery and mechanical workshop for the manufacture of his own invention, a monogram embroidery machine. Together with his brother Georg, a salesman, Karl Friedrich ran the Gebrüder Gegauf (Bros. Gegauf) company. Through his involvement in the textile industry, he noticed how laborious it was to produce hemstitching, which until then could only be done manually. Consequently, in 1893, Karl Friedrich Gegauf invented the world’s first hemstitch sewing machine, capable of sewing 100 stitches per minute.[3] In 1895, the Bros. Gegauf workshop was completely destroyed by fire, except for the prototype of the hemstitch sewing machine, which was the only thing that could be rescued. Karl Friedrich built a new workshop in an old barn, where the focus was no longer on embroidery, but on the construction of the hemstitch sewing machine. About 70 people were employed in the serial production of the hemstitch sewing machine. The mechanical production of hemstitching, whether as embellishment for handkerchiefs, tablecloths, or bedspreads, was commonly referred to as "gegaufing", because the name Gegauf became famous in the industry.[4]
1926–1947: Fritz Gegauf and the development of the first Bernina household sewing machine[edit]
In 1919, Fritz Gegauf, one of Karl’s sons, together with his father, filed a patent application for the "Wotan" hemstich sewing machine, which became another international success for the company, which changed its name to "Fritz Gegauf". After being in Paris selling the company’s tin openers, which had no market in Switzerland, he returned to his home town. His brother Gustav and he took control of the factory after their father’s death in 1926.[5] During the Great Depression, Fritz Gegauf joined forces with the embroidery factory, Brütsch & Sohn in St. Gallen, which was also operating in the red. By the end of 1932, they had developed the company's first household sewing machine, which they named Bernina. The Bernina was soon being produced as furniture-cum-sewing-machine, which required the building of a new, attached furniture factory in Steckborn. As of October 26, 1937, a total of 20,000 machines had left the factory in Steckborn. In 1937, he introduced the first Bernina zigzag machine and in 1945 the world’s first portable zigzag machine on the market. In 1947, Gustav Gegauf left the company. By mid-1963, one million Bernina zigzag sewing machines had been manufactured in Steckborn. Since then, the company has commonly been called Bernina, although, since 1947, its official name has been "Fritz Gegauf Aktiengesellschaft, Bernina Nähmaschinenfabrik".
1959–1988: Odette Gegauf-Ueltschi and the fully automatic sewing machine[edit]
Since 1959, Odette Ueltschi, Fritz Gegauf's daughter, took the lead role at Bernina.[6] She took over the management after the death of her brother in 1965. In 1963, the first Bernina sewing machine with a patented knee-activated presser foot lifter, the 730, appeared on the market. From 1963 onwards, the subsequent model, the 730, was produced, and in the same year, the millionth Bernina sewing machine was manufactured. The top-seller of all the models was the 830 class, which came into production in 1971 and continued until 1981. In 1981, the company took a further step in the development of household sewing machines. The 930 model was the first machine with a stretch-stitch function. It was followed by the 1130, the first fully automated sewing machine, the 1130, launched in 1986. The enduring mark which Odette Gegauf-Ueltschi left on the company is reflected in the name of the bernette sewing machine line, formed by a combination of the first half of the brand name and the second half of her given name.[7]
1988–2009: Hanspeter Ueltschi and the first sewing computer, expansion of markets and production[edit]
Hanspeter Ueltschi took over the management of Fritz Gegauf AG in 1988 from his mother Odette Gegauf-Ueltschi, and currently runs the company as owner and chairman of the board of directors. After studying business administration at the University of St. Gallen, Ueltschi spent seven years gaining professional experience in the USA before getting into the leadership of the family company in Switzerland. Ueltschi further expanded the leading position of the company in the sewing machine technology sector, brought down manufacturing costs, and promoted product innovations and marketing. He ushered the computer age into the business with the artista 180, Bernina’s first sewing computer, and ensured the continuous development and optimization of computer technology in the sewing sphere, as shown by the successive models of the artista, as well as the aurora series. In doing so, he made strides toward his declared goal of making sewing more appealing and more popular worldwide. Under the chairmanship of Hanspeter Ueltschi, a manufacturing outlet was set up in Thailand, in addition to the parent factory in Steckborn. He is also largely responsible for establishing the US as a key market and expansion to the new markets in Eastern Europe, Russia, South America, and India, as well as in the Middle East. He renamed "Fritz Gegauf AG" to "Bernina International AG" to accommodate the trend toward globalization and the success of the company brand and at the same time, Ueltschi incorporated the flag of Switzerland into the company logo as a sign of patriotism. Linking to the 830, the most successful Bernina model from the 1970s, the new B830, in 2008 and its sister model, the B820, in 2009, were introduced as the most advanced sewing machines of the brand to date, with a total of 15 patents filed for the new B830.
Present[edit]
The Bernina Textile Group is a globally active group of 15 companies doing business in 80 countries. The company operates in the product categories such as household sewing and embroidery machines, household overlocker machines, longarm quilting machines, multineedle embroidery machines, accessories (presser foot, embroidery hoops and other accessories for sewing, quilting and overlocking), and computer software for embroidery design.
Subsidiaries are established in Australia, Austria, Belgium, Germany, Japan, the Netherlands, New Zealand, Switzerland, and the USA. The subsidiary Benartex, headquartered in the United States[8], sells printed textiles and quilting fabrics in particular. OESD, another subsidiary, develops and sells embroidery designs. Brewer, engaging in the sewing supplies market, offers sewing and crafting notions, patterns, books etc. The company supplies 80 markets worldwide via business-to-business connections.
The latest model, B 880, is the company’s current flagship model, while the 7 series models are Bernina’s most advanced products, equipped with the Bernina hook system for 9 mm stitch width at up to 1,000 stitches per minutes.
Models[edit]
Timeline[edit]
Year 1932 1938 1945 1954 1963 1971 1982 1986 1989 1993 1998 2001 2002 2004 2006 2007 2008 2009 2010
Models Model 105
Model 117
Model 125
Model 530
Model 730
Model 830
Model 930
Model 1130
Model 1230/1260
Model 1630
artista 180
activa 145
artista 200
QE
artista 640
aurora 440 QE
artista 730
Model B830
Model B820
Model ranges[edit]
Construction Series Note Image
1932–1945 Model 105 First household sewing machine bearing the Bernina brand name
Manual sewing machine manufactured by Fritz Gegauf
1938–1945 Model 117 First BERNINA zigzag sewing machine.
1945–1963 Model 125 First electric Bernina free-arm zigzag sewing machine
1954–1963 Model 530 First Bernina with patented snap-on presser foot and semi-automatic buttonhole-sewing function
1963–1982 Model 730 The 730 model, with patented knee-activated presser-foot lifter
1971–1982 Model 830 First Bernina with electronic foot control—the top-of-the-range model for 11 years
1982–1989 Model 930 First Bernina with stretch-stitch function and an especially powerful motor
1986–1989 Model 1130 First computerized Bernina with fully automatic one-step buttonholes and stitch memory
1989–1998 Model 1230 Model with expanded memory capacity and fully automatic one-step buttonholes, including eyelet buttonholes
1993–1998 Model 1630 Top model: 9mm stitch width, over 400 stitch patterns, monograms, five alphabets, sewing in 16 directions possible
1998–2002 artista 180 Top model with Customized Pattern Selection software for customer-specific settings, optional embroidery module, conversion of scanned templates to embroidery designs
2001–2002 activa 145 Simple compact sewing machine: Computerized; individually adjustable memory for stitch patterns, buttonhole repeat, stitch library, patchwork presser foot
2002–2006 artista 200 World’s first sewing and embroidery computer: Microsoft Windows operating system, CD-ROM drive, LCD display, more than 850 stitches, programmable function key, memory function for stitch combinations and embroidery designs
2004–2006 440QE World’s first sewing computer with Bernina Stitch Regulator system for consistent stitch lengths at variable sewing speeds, especially for quilters[9]
2004 artista 640 Advanced sewing computer: Extensive utility and decorative stitch programs, optional embroidery module with built-in embroidery software and optional BSR system
2006 artista 730 High-end sewing and embroidery system: Utility and decorative stitches, embroidery designs, many automatic settings such as thread cutter, touchscreen, BSR system, CFL light. Optional embroidery module
2008 Model B830 World’s biggest and fastest sewing and embroidery system for home users: 1100 sewing stitches/min, 1000 embroidery stitches/min, extra-large bobbin (40% more capacity than before), fully automatic needle threader, 360° multidirectional sewing, 7-inch TFT screen, especially bright working area (30 LED lamps), more than 1000 stitch patterns, 150 pre-installed embroidery motifs by international designers
2009 Model B820 Similar to the B830, but without embroidery functionality (not upgradable) or sideways feed (multidirectional sewing), and with a smaller screen and fewer stitch patterns
2011 Model 580 Sewing and embroidery machine, top model of the Bernina 5 series: 227 stitches, of which 186 decorative stitches, optional embroidery module, large TFT touch screen, memory function, embroidery function integrated and 100 embroidery motifs
2012 Model 780 Sewing and embroidery machine with Bernina dual transport, Bernina 9 gripper, large embroidery module, BSR, 1306 stitches, 130 integrated embroidery patterns, including sewing consultant and tutorial, top model of the Bernina-7 series
2014 Model Q 24 First Bernina long-arm quilting machine with 24-inch free arm, stitch regulation via integrated BSR sensors, 2.200 stitches per minute, designed for use on a quil frame of 3,55x1,2 m (length x width), installation at the parent plant in Steckborn, until now, Bernina has only been producing household sewing machines with the Q 24 model and the smaller Q 20 to a new, semiprofessional customer segment, the so-called prosumer. For the long-arm quilting machines, a new assembly line was set up in the Steckborn headquarters.
2015 Model 790 Further development of the B 780 with new gripper (in the sister model B 720 for the first time also available with 5.5mm stitch width), adaptive thread tension, embroidery module, embroidery designer and BERNINA stitch regulator.[10]
Embroidery software[edit]
Bernina developed embroidery design editing and full digitizing software branded under its own name and written by industrial digitizing software manufacturer Wilcom International Pty Ltd.[11]
See also[edit]
List of sewing machine brands
Sewing machine
Machine embroidery
References[edit]
Jump up ^ "Sewing hotshot Hanspeter Ueltschi pays a visit to Portland's Modern Domestic". OregonLive.com. 2014-04-24. Retrieved 2017-07-20.
Jump up ^ Enders, Gudrun (2015-04-15). "Nähmaschine kommt von Herzen" (in German). Thurgauer Zeitung. Retrieved 2017-07-19.
Jump up ^ Harris, Jessica. "Sewing Machine Companies & Brands". Retrieved 2017-07-20.
Jump up ^ Wright, Ericka (2014-07-31). "Bernina: Sewing Machine Royalty Bearing Gifts". Retrieved 2017-07-20.
Jump up ^ "History of the Sewing Machine". Bernina International. p. 23. Retrieved 2017-07-21.
Jump up ^ "Der Erfinder Karl Friedrich Gegauf" (in German). Bernina International. p. 22. Retrieved 2017-07-21.
Jump up ^ "Bernina history". Bernina. Retrieved 2017-07-21.
Jump up ^ "Bernina of America to Exhibit at Runways & Gallery at Austin Fashion Week May 18 - 21 in Austin Texas". 2017-05-16. Retrieved 2017-07-21.
Jump up ^ Switzerland Released EP1738007 B1, King, Michael; Zrsch, Wolfgang & Durville, Gérard, "Method and device for controlling the needle movement in a sewing machine"
Jump up ^ Switzerland Released EP2623658 B1, Brunner, Severin; Wacker, Niklaus & Janouschek, Georg et al., "Gripper arrangement for a sewing machine"
Jump up ^ Bernina (2009), "Product Brochure", p. 4
Further reading[edit]
Daniela Dujmic-Erbe: Bernina - Der rote Faden in der Welt des Nähens, 2006, ISBN 978-3-033-01045-1
Fredy Meyer: Der Erfinder Karl Friedrich Gegauf, 2010, Medien Konstanz GmbH, ISBN 978-3-942058-00-1
Verein für wirtschaftshistorische Studien: Schweizer Pioniere der Wirtschaft und Technik, 1969, Zürich, Band 21
External links[edit]
Wikimedia Commons has media related to Bernina (company).
Official website
Bernina Canada
Bernina Australia
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text:
The End of the Affair
From Wikipedia, the free encyclopedia
Jump to: navigation, search
For other uses, see The End of the Affair (disambiguation).
The End of the Affair
First edition
(with Daily Mail Book of the Month wrapper)
Author
Graham Greene
Country
United Kingdom
Language
English
Set in
London, 1942–46
Publisher
Heinemann
Publication date
1951
Media type
Hardcover (first edition)
Pages
237 p. (first edition)
OCLC
492087111
Dewey Decimal
823.912
Preceded by
The Third Man (1949)
Followed by
The Quiet American (1955)
The End of the Affair (1951) is a novel by British author Graham Greene, as well as the title of two feature films (released in 1955 and 1999) that were adapted from the novel.
Set in London during and just after the Second World War, the novel examines the obsessions, jealousy and discernments within the relationships between three central characters: writer Maurice Bendrix; Sarah Miles; and her husband, civil servant Henry Miles.
Graham Greene's own affair with Lady Catherine Walston played into the basis for The End of the Affair. The British edition of the novel is dedicated to "C" while the American version is made out to "Catherine." Greene's own house at 14 Clapham Common Northside was bombed during the Blitz.[1]
Contents
[hide]
1 Synopsis
2 Criticism
3 Adaptations
4 References
5 External links
Synopsis[edit]
The novel focuses on Maurice Bendrix, a rising writer during the Second World War in London, and Sarah Miles, the wife of an impotent civil servant. Bendrix is based on Greene himself, and he reflects often on the act of writing a novel. Sarah is based on Greene's lover at the time, Catherine Walston, to whom the book is dedicated.
Bendrix and Sarah fall in love quickly, but he soon realises that the affair will end as quickly as it began. The relationship suffers from his overt and admitted jealousy. He is frustrated by her refusal to divorce Henry, her amiable but boring husband. When a bomb blasts Bendrix's flat as he is with Sarah, he is nearly killed. After this, Sarah breaks off the affair with no apparent explanation.
Later, Bendrix is still wracked with jealousy when he sees Henry crossing the Common that separates their flats. Henry has finally started to suspect something, and Bendrix decides to go to a private detective to discover Sarah's new lover. Through her diary, he learns that, when she thought he was dead after the bombing, she made a promise to God not to see Bendrix again if He allowed him to live again. Greene describes Sarah's struggles. After her sudden death from a lung infection brought to a climax by walking on the Common in the rain, several miraculous events occur, advocating for some kind of meaningfulness to Sarah's faith. By the last page of the novel, Bendrix may have come to believe in a God as well, though not to love Him.
The End of the Affair is the fourth and last of Greene's explicitly Catholic novels.
Criticism[edit]
Though often considered as among Greene's best novels, and having been chosen by Robert McCrum for his list of the '100 Greatest Novels in English', the author Jonathan Franzen said that he considered E. M. Forster and Graham Greene, in particular highlighting The End of the Affair. However, he did also comment that he believed that part of the reason for this was him being American, as he said that many authors' brilliance is lost when it crosses the Atlantic. He said that he believed that the effect may have occurred with David Foster Wallace.
Adaptations[edit]
Main articles: The End of the Affair (1955 film), The End of the Affair (1999 film), and The End of the Affair (opera)
In 1955, the book was made into a film, directed by Edward Dmytryk, with the screenplay adaptation by Lenore J. Coffee. David Lewis was the producer and David E. Rose executive producer. It starred Deborah Kerr as Sarah Miles, Van Johnson as Maurice Bendrix, John Mills as Albert Parkis, and Peter Cushing as Henry Miles.
In 1999, the novel was made into another film (The End of the Affair), directed by Neil Jordan. Jordan also wrote the screenplay and produced the film with Stephen Woolley. It starred American actress Julianne Moore as Sarah Miles, English actor Ralph Fiennes as Maurice Bendrix, and Irish actor Stephen Rea as Henry Miles. Julianne Moore was nominated for an Academy Award for Best Actress for her performance.
In 2004, Jake Heggie composed an opera based on the novel. It premiered at the Houston Grand Opera in March of that year, and was subsequently revised into its final form.
In 2011, the novel was adapted into a play by Karla Boos and had its world premiere at Quantum Theatre.[2]
In 2012, an audio edition performed by Colin Firth and produced by Audible.com was released; the recording was recognized as Audiobook of the Year at the Audies Gala in May 2013.[3]
Various websites have suggested that the 2012 Bollywood film Jab Tak Hai Jaan might have drawn inspiration from the novel.[4][5]
The Italian band Daisy Chains has released an album titled A Story Has No Beginning or End, which is the first line of the novel by G. Greene, and whose own second track is titled "The End of the Affair".[6]
References[edit]
Jump up ^ Graham Greene, uneasy Catholic – TLS Highlights – Times Online
Jump up ^ "Quantum looks to have an 'Affair' in Polish Hill" (25 Aug 2011) Pittsburgh Post-Gazette
Jump up ^ "Colin Firth Wins Audiobook of the Year for 'The End of the Affair'" (31 May 2013) Galleycat
Jump up ^ "'Jab Tak Hai Jaan': Inspired by Graham Greene's novel 'The End of the Affair'?" (17 November 2012) IBNLive
Jump up ^ "Is JAB TAK HAI JAAN inspired by THE END OF THE AFFAIR?" (17 November 2012) Glamsham
Jump up ^ "Italian Daisy Chains"
External links[edit]
The End of the Affair (1955) on IMDb
The End of the Affair (1999) on IMDb
Nicolas Tredell's London Fictions article on The End of the Affair https://www.londonfictions.com/graham-greene-the-end-of-the-affair.html
[hide]
v
t
e
Works by Graham Greene
Novels
The Man Within (1929)
The Name of Action (1930)
Rumour at Nightfall (1932)
Stamboul Train (1932)
It's a Battlefield (1934)
England Made Me (1935)
The Bear Fell Free (1935)
A Gun for Sale (1936)
Brighton Rock (1938)
The Confidential Agent (1939)
The Power and the Glory (1940)
The Ministry of Fear (1943)
The Heart of the Matter (1948)
The Third Man (novella; 1949)
The End of the Affair (1951)
The Quiet American (1955)
Loser Takes All (1955)
Our Man in Havana (1958)
A Burnt-Out Case (1960)
The Comedians (1966)
Travels with My Aunt (1969)
The Honorary Consul (1973)
The Human Factor (1978)
Doctor Fischer of Geneva (1980)
Monsignor Quixote (1982)
The Tenth Man (1985)
The Captain and the Enemy (1988)
No Man's Land (2005)
Travel books
Journey Without Maps (1936)
The Lawless Roads (1939)
In Search of a Character: Two African Journals (1961)
Autobiography
A Sort of Life (1971)
Ways of Escape (1980)
Getting to Know the General: The Story of an Involvement (1984)
A World of My Own: A Dream Diary (1992)
Plays
The Living Room (1953)
The Potting Shed (1957)
The Complaisant Lover (1959)
Carving a Statue (1964)
The Return of A. J. Raffles (1975)
The Great Jowett (1981)
Yes and No (1983)
For Whom the Bell Chimes (1983)
Films
The Future's in the Air (1937)
The New Britain (1940)
21 Days (1940)
Brighton Rock (1947)
The Fallen Idol (1948)
The Third Man (1949)
The Heart of the Matter (1953)
Loser Takes All (1956)
Saint Joan (1957)
The Quiet American (1958)
Our Man in Havana (1959)
The Comedians (1967)
Story collections
Twenty-One Stories (1954)
A Sense of Reality (1963)
May We Borrow Your Husband? (1967)
The Last Word and Other Stories (1990)
Short stories
"The End of the Party" (1929)
"Proof Positive" (1930)
"The Basement Room" (1936)
"Across the Bridge" (1938)
"Alas, Poor Maling" (1940)
"The Blue Film" (1954)
"The Destructors" (1954)
"A Shocking Accident"
"The Invisible Japanese Gentlemen"
"The Last Word"
Authority control
WorldCat Identities
GND: 4594462-3
VIAF: 175555776
Retrieved from "https://en.wikipedia.org/w/index.php?title=The_End_of_the_Affair&oldid=839960742"
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