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My Hero Academia
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My Hero Academia
Cover of the first volume of My Hero Academia, featuring Izuku Midoriya and All Might
僕のヒーローアカデミア
(Boku no Hīrō Akademia)
Genre
Adventure, comedy[1]
Manga
Written by
Kōhei Horikoshi
Published by
Shueisha
English publisher
AUS
Madman Entertainment
NA
Viz Media
Demographic
Shōnen
Imprint
Jump Comics
Magazine
Weekly Shōnen Jump[2]
English magazine
NA
Weekly Shonen Jump
Original run
July 7, 2014 – present
Volumes
16 (List of volumes)
Manga
My Hero Academia Smash!!
Written by
Kohei Horikoshi
Illustrated by
Hirofumi Neda
Published by
Shueisha
English publisher
NA
Viz Media
Demographic
Shōnen
Magazine
Shōnen Jump +
English magazine
NA
Weekly Shonen Jump
Original run
November 9, 2015 – present
Volumes
2
Anime television series
Directed by
Kenji Nagasaki
Written by
Yōsuke Kuroda
Music by
Yuki Hayashi
Studio
Bones
Licensed by
AUS
Madman Entertainment (former)
Universal/Sony
NA
Funimation
UK
Universal Pictures UK
Original network
JNN (MBS) (Season 1)[3]
NNS (ytv) (Season 2)[4]
English network
SEA
Animax Asia[5]
Original run
April 3, 2016 – present
Episodes
38 (List of episodes)
Game
My Hero Academia: Battle for All
Developer
Dimps
Publisher
Bandai Namco Entertainment
Platform
Nintendo 3DS
Released
JP: May 19, 2016
Manga
Vigilante: My Hero Academia Illegals
Written by
Hiyuki Furuhashi
Illustrated by
Betten Court
Published by
Shueisha
English publisher
NA
Viz Media
Demographic
Shōnen
Magazine
Shōnen Jump GIGA
Shōnen Jump +
Original run
September 2016 – present
Volumes
1
Anime and Manga portal
My Hero Academia (Japanese: 僕のヒーローアカデミア, Hepburn: Boku no Hīrō Akademia) is a comedy adventure manga series written and illustrated by Kōhei Horikoshi. It has been serialized in Weekly Shōnen Jump since July 2014,[6] and 15 volumes have been collected in tankōbon format. The series has been licensed for English-language release by Viz Media, and began serialization in their weekly digital manga anthology Weekly Shonen Jump on February 9, 2015.[7]
The story follows Izuku Midoriya, a boy born without superpowers in a world where they are the norm, but who still dreams of becoming a superhero himself, and is scouted by the world's greatest hero who shares his powers with Izuku after recognizing his value and enrolls him in a high school for heroes in training. The manga was adapted into an anime television series; the first season aired from April 3 to June 26, 2016.[8] The second season aired from April 1 to September 30, 2017. A third season has been announced.[9]
Contents
[hide]
1 Plot
2 Media
2.1 Manga
2.2 Anime
2.3 Video game
3 Reception
4 References
5 External links
Plot[edit]
Main article: List of My Hero Academia characters
On an Earth-like world where people with superpowers known as "Quirks" (個性, Kosei) are the norm, Izuku Midoriya is a regular middle school student who has dreams of one day becoming a Hero despite being bullied by his classmates for not having a Quirk. After being the only one to try and save his childhood bully Katsuki from a Villain, the world's greatest Hero All Might bestows upon him his own quirk "One For All". The story follows Izuku's entrance into U.A. High School (雄英高校, Yūei Kōkō), a school that cultivates the next generation of Super Heroes.
Media[edit]
Manga[edit]
Main article: List of My Hero Academia chapters
My Hero Academia is a Japanese manga series written and illustrated by Kōhei Horikoshi. It began its serialization in the manga magazine Weekly Shōnen Jump in July 2014. As of September 4, 2017 the series been collected into fifteen tankōbon volumes.[10] The series is licensed for English language release in North America by Viz Media, who published the first volume on August 4, 2015. As the series is published in Japan, it is also released simultaneously in English digitally by Viz Media's Weekly Shounen Jump. As of February 7, 2017, 8 volumes have been released.[10]
Anime[edit]
Main article: List of My Hero Academia episodes
On October 29, 2015, the series' official Twitter announced that My Hero Academia would receive an anime adaptation produced by Studio Bones.[11]
With the anime announced, TOHOSHI Group registered the domain name "heroaca.com" as the anime's website.[11] The anime is directed by Kenji Nagasaki, written by Yōsuke Kuroda, and feature character designs by Yoshikiko Umakoshi and music composed by Yuki Hayashi.[12][13] The anime premiered on MBS and other Japan News Network stations in 'Nichigo' time slot at 5pm on Sundays in Japan. The opening theme is "The Day", performed by Porno Graffitti and the ending theme is "Heroes", performed by Brian the Sun. In March 2016, Funimation Entertainment announced they had licensed the series for streaming services, home and broadcast release as well as obtaining the merchandise rights.[14] It has also been licensed in the United Kingdom by Universal Pictures UK.[15]
A second season was announced in the Weekly Shōnen Jump magazine's 30th issue of 2016.[10] It premiered on April 1, 2017 on NTV and YTV, and ended on September 30, 2017, with the staff and cast from the first season returning to reprise their roles.[16]
A third season was announced in the 44th issue of Weekly Shōnen Jump magazine of 2017.[17][9]
Video game[edit]
A video game based on the anime was announced in November 2015.[18] The game is developed by Bandai Namco Studios and published by Bandai Namco Entertainment for the Nintendo 3DS handheld game console, which was released in Japan on May 19, 2016.[19]
Reception[edit]
The manga was nominated for the 8th Manga Taishō in 2015.[20] Before the anime adaptation's premiere, manga author Masashi Kishimoto praised Kōhei Horikoshi's work, believing it would be a success overseas; Horikoshi, meanwhile, has cited Kishimoto's Naruto series as a primary source of inspiration.[21]
Volume 1 reached the 7th place on the weekly Oricon manga chart with 71,575 copies sold.[22] It sold out almost immediately on its first printing.[23] Volume 2 reached the 6th place, with 167,531 copies[24] and, by January 18, 2015, had sold 205,179 copies.[25] As of March 2017, there were over 10 million copies of My Hero Academia in circulation.[26]
The story has been noted to take inspiration from elements in superhero comics, such as the aesthetics of its characters.[27]
Alex Osborn of IGN gave the anime series positive marks, saying "The first season of My Hero Academia delivers thirteen episodes of fantastic action, elevated by a heartfelt story that's wrapped around a core cast of memorable and relatable characters." Osborn went on to state that the villains were underdeveloped.[28]
The manga won the Sugoi Japan Award in 2017.[29] It also won the "Japan Expo Awards" in the same year.[30]
References[edit]
Jump up ^ "Official Website for My Hero Academia". Viz Media. Retrieved October 26, 2017.
Jump up ^ "Official Shonen Jump website". Archived from the original on December 15, 2014. Retrieved December 4, 2014.
Jump up ^ "My Hero Academia Anime to Air in MBS/TBS' 'Nichigo' Timeslot". Anime News Network. January 10, 2016. Archived from the original on January 11, 2016. Retrieved January 10, 2016.
Jump up ^ "My Hero Academia Season 2 Anime to Air on NTV, YTV". Anime News Network. December 22, 2016. Archived from the original on December 23, 2016. Retrieved December 22, 2016.
Jump up ^ "Exclusive: Animax Asia Airs Simulcast of My Hero Academia, Twin Star Exorcists". Anime News Network. March 28, 2016. Archived from the original on April 27, 2016. Retrieved April 6, 2016.
Jump up ^ "Shonen Jump to Launch 4 Manga Series in Next 3 Issues". Anime News Network. June 25, 2014. Archived from the original on December 5, 2014. Retrieved November 30, 2014.
Jump up ^ "Viz's Shonen Jump Adds My Hero Academia". Anime News Network. Archived from the original on January 28, 2015. Retrieved January 26, 2015.
Jump up ^ "My Hero Academia TV Anime Adaptation Confirmed". Anime News Network. October 29, 2015. Archived from the original on November 1, 2015. Retrieved November 2, 2015.
^ Jump up to: a b "My Hero Academia Anime Gets 3rd Season". Anime News Network. September 30, 2017. Archived from the original on October 2, 2017. Retrieved October 2, 2017.
^ Jump up to: a b c "My Hero Academia Anime Gets 2nd Season". Anime News Network. June 23, 2016. Archived from the original on June 23, 2016. Retrieved June 23, 2016.
^ Jump up to: a b "Boku No Hero Academia TV Anime Adaptation Announced". OtakuTale. Archived from the original on October 30, 2015. Retrieved November 5, 2015.
Jump up ^ "My Hero Academia TV Anime's Main Staff Revealed". Anime News Network. Archived from the original on November 6, 2015. Retrieved November 5, 2015.
Jump up ^ "My Hero Academia Anime's 4th Promo Video Previews Animation". Anime News Network. February 28, 2016. Archived from the original on February 29, 2016. Retrieved February 28, 2016.
Jump up ^ "Funimation Licenses My Hero Academia Anime". Anime News Network. March 8, 2016. Archived from the original on March 10, 2016. Retrieved March 8, 2016.
Jump up ^ "BBFC Lists My Hero Academia From Universal". Anime News Network. March 24, 2017. Archived from the original on March 25, 2017. Retrieved March 24, 2017.
Jump up ^ Green, Scott (February 2, 2017). "Latest "My Hero Academia" Anime Cast Addition And Plans Spotted". Crunchyroll. Archived from the original on February 3, 2017. Retrieved February 2, 2017.
Jump up ^ ""My Hero Academia Season 3 Planned"". Crunchyroll. September 29, 2017. Archived from the original on September 30, 2017. Retrieved September 29, 2017.
Jump up ^ Sato (November 18, 2015). "My Hero Academia Game Announced For Nintendo 3DS". Siliconera. Archived from the original on 19 November 2015. Retrieved 18 November 2015.
Jump up ^ "My Hero Academia: Battle for All 3DS Game's Play Videos Preview Characters". Anime News Network. April 4, 2016. Archived from the original on April 5, 2016. Retrieved April 5, 2016.
Jump up ^ "8th Manga Taisho Awards Nominates 14 Titles". Anime News Network. January 18, 2015. Archived from the original on January 19, 2015. Retrieved January 19, 2015.
Jump up ^ "Naruto Cheers on My Hero Academia's Deku". Anime News Network. April 2, 2016. Archived from the original on April 3, 2016. Retrieved April 3, 2016.
Jump up ^ "Japanese Comic Ranking, November 3–9". Anime News Network. November 12, 2014. Archived from the original on December 2, 2014. Retrieved November 30, 2014.
Jump up ^ "Up and Coming Manga Sold Out Immediately". December 1, 2014. Archived from the original on December 3, 2014. Retrieved December 4, 2014.
Jump up ^ 週間 コミックランキング 2015年01月19日付. Oricon Style (in Japanese). Oricon. Archived from the original on January 19, 2015. Retrieved January 20, 2015.
Jump up ^ "Japanese Comic Ranking, January 12–18". Anime News Network. January 21, 2015. Archived from the original on January 22, 2015. Retrieved January 22, 2015.
Jump up ^ "My Hero Academia Has Over 10 Million Copies in Print". Anime News Network. 31 March 2017. Archived from the original on 31 March 2017. Retrieved 31 March 2017.
Jump up ^ ""My Hero Academia" Volume 1 Horikoshi Kohei [daily cartoon guide]". November 19, 2014. Archived from the original on December 10, 2014. Retrieved December 4, 2014.
Jump up ^ Osborn, Alex (June 30, 2016). "My Hero Academia: Season 1 Review". IGN. Archived from the original on July 9, 2016. Retrieved July 16, 2016.
Jump up ^ "Re:ZERO, My Hero Academia Top Sugoi Japan Awards 2017 Results". Anime News Network. March 16, 2017. Archived from the original on August 1, 2017. Retrieved September 13, 2017.
Jump up ^ "Japan Expo AwardsのDaruma賞受賞作品". Japan Expo. March 6, 2017. Archived from the original on September 20, 2017. Retrieved September 13, 2017.
External links[edit]
Official anime website (in Japanese)
Official page at Weekly Shōnen Jump (in Japanese)
My Hero Academia (manga) at Anime News Network's encyclopedia
[show]
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Series currently running in Weekly Shōnen Jump
Black Clover
Boruto: Naruto Next Generations
Food Wars!: Shokugeki no Soma
Gin Tama
Haikyu!!
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2011
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2012
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Cross Manage
Food Wars!: Shokugeki no Soma
2013
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2014
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My Hero Academia
2015
Black Clover
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2016
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2017
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[show]
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Soul Eater (2008–2009)
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Fullmetal Alchemist: Brotherhood (2009–2010)
Tokyo Magnitude 8.0 (2009)
Darker than Black: Gemini of the Meteor (2009)
Heroman (2010)
Star Driver (2010–2011)
Gosick (2011)
No. 6 (2011)
Un-Go (2011)
Eureka Seven: AO (2012)
Blast of Tempest (2012–2013)
Tenkai Knights (2013–2015)
Space Dandy (2014)
Noragami (2014)
Captain Earth (2014)
Soul Eater Not! (2014)
Chaika - The Coffin Princess (2014)
Chaika - The Coffin Princess: Avenging Battle (2014)
Blood Blockade Battlefront (2015)
Show by Rock!! (2015)
Snow White with the Red Hair (2015–2016)
Noragami Aragoto (2015)
Concrete Revolutio (2015)
Concrete Revolutio: The Last Song (2016)
My Hero Academia (2016–present)
Bungo Stray Dogs (2016)
Show by Rock!! Short!! (2016)
Mob Psycho 100 (2016)
Show by Rock!!♯ (2016)
Blood Blockade Battlefront & Beyond (2017)
OVAs/ONAs
RahXephon Interlude: Her and Herself/Thatness and Thereness (2003)
Wolf's Rain (2004)
Fullmetal Alchemist: Premium Collection (2006)
Ayashi Divine Comedy (2007)
Darker than Black: Beneath the Fully Bloomed Cherry Blossoms (2008)
Xam'd: Lost Memories (2008–2009)
Fullmetal Alchemist: Brotherhood (2009–2010)
Halo Legends (animated sequence) (2010)
Darker than Black: Gaiden (2010)
Chaika - The Coffin Princess (2015)
Snow White with the Red Hair (2016)
Blood Blockade Battlefront (2016)
Bungo Stray Dogs (2017)
Films
Escaflowne (2000)
Cowboy Bebop: The Movie (2001)
RahXephon: Pluralitas Concentio (2003)
Fullmetal Alchemist the Movie: Conqueror of Shamballa (2005)
Sword of the Stranger (2007)
Eureka Seven: Pocketful of Rainbows (2009)
Towa no Quon (film series) (2011)
Fullmetal Alchemist: The Sacred Star of Milos (2011)
Un-Go episode:0 Inga chapter (2011)
Star Driver: The Movie (2013)
Eureka Seven: Hi-Evolution (film series) (2017–2019)
Bungo Stray Dogs: Dead Apple (2018)
Video games
Robot Alchemic Drive (2002)
Fullmetal Alchemist and the Broken Angel (2003)
Fullmetal Alchemist 2: Curse of the Crimson Elixir (2004)
Fullmetal Alchemist 3: Kami o Tsugu Shōjo (2005)
Liberation Maiden (2012)
Professor Layton vs. Phoenix Wright: Ace Attorney (2012)
Phoenix Wright: Ace Attorney − Dual Destinies (2013)
Persona 4: Dancing All Night (2015)
Category
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Code Geass: Lelouch of the Rebellion R2
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Sengoku Basara II
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The Heroic Legend of Arslan
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My Hero Academia
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The Seven Deadly Sins: Signs of Holy War
Mobile Suit Gundam: Iron-Blooded Orphans (Season Two)
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text:
Earth's rotation
From Wikipedia, the free encyclopedia
Jump to: navigation, search
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 2.3 milliseconds per century since the 8th century BCE.[2]
Contents
[hide]
1 History
1.1 Empirical tests
2 Rotation period
2.1 True solar day
2.2 Mean solar day
2.3 Stellar and sidereal day
2.4 Angular speed
3 Changes in rotation
3.1 Change in rotational axis
3.2 Change 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.
Rotation period [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: Mean solar day
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 in rotation[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.
Change 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.
Change 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.
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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Clarke Griffin
From Wikipedia, the free encyclopedia
Jump to: navigation, search
Clarke Griffin
The 100 trilogy (novel)
The 100 (television)
character
Eliza Taylor as Clarke Griffin in the television series The 100.
First appearance
Novels
The 100 (Book #1)
September 3, 2013
Television
"Pilot" (1.01)
March 19, 2014
Last appearance
Novels
The 100: Rebellion (Book #4)
December 6, 2016
Created by
Kass Morgan
Jason Rothenberg
Portrayed by
Eliza Taylor
Information
Aliases
Prisoner 319
Television
Wanheda ("Commander of Death")
Klark kom Skaikru ("Clarke of the Skypeople")
Species
Human
Gender
Female
Occupation
Co-leader of The 100
Medical student (formerly)
Family
Novels
Dr. David Griffin (father)
Dr. Mary Griffin (mother)
Television
Jake Griffin (father)
Dr. Abigail "Abby" Griffin (mother)
Significant other(s)
Novels
Wells Jaha
Bellamy Blake
Television
Finn Collins
Lexa
Niylah
Clarke Griffin is a fictional character from the American post apocalyptic young adult science fiction novel series by Kass Morgan, The 100, and television series The 100 on The CW. Clarke is one of the main characters in both the trilogy and the television series, where she is portrayed by Eliza Taylor. She first appears in Morgan's first novel, The 100, and later in the pilot episode of the television series, as a prisoner on a space colony charged with treason. Clarke was one of the original hundred delinquents sent down to Earth to test if it was inhabitable again after a nuclear apocalypse destroyed it a long period prior.
Contents
[hide]
1 Character
1.1 Novels
1.2 Television
1.2.1 Background
1.2.2 Storyline
2 Reception
3 References
Character[edit]
Novels[edit]
Clarke Griffin was born and raised in a space colony above Earth to Dr. David and Mary Griffin. She is a medical student who hopes to follow her parents’ footsteps as a physician, taught by the Council's chief medical adviser Dr. Lahiri. She is also in a relationship with the colony's Chancellor’s son, Wells Jaha. Clarke discovers that her parents are conducting illegal experiments on children under threat of the corrupt Vice Chancellor Rhodes. She confides in Wells, who despite swearing his secrecy, tells his father, hoping to save the Griffins from Rhodes. However, due to the lack of evidence of Rhodes’ involvement, the Griffins are arrested, which also ends Clarke’s relationship with Wells; Clarke assumes that her parents are executed following their arrest, leading her to hate Wells.
Two years later, the Colony decides to send one hundred of its teenage prisoners to investigate whether Earth is habitable. Among the one hundred are Clarke, Wells, Octavia Blake, her older brother Bellamy Blake, and Clarke's friend, Thalia. After arriving on Earth, Clarke and Bellamy become attracted to each other and eventually develop a romantic relationship while co-leading the 100 with Wells.
Eventually, someone sets fires on the camp they are at, ultimately they discover that they are not alone on Earth. The 100 captured an Earth-born girl, Sasha Walgrove, and she reveals there are people from the Colony who arrived before the 100. Clarke eventually meets Sasha’s father, Max, who is a leader of an underground colony underneath the ruins of Mount Weather Emergency Operations Center. Max reveals that he helped Clarke’s parents two years ago, giving her hope that they are still alive. She also discovers that Wells and Bellamy are paternal half-brothers after Wells realizes that Bellamy is his father's secret son from a previous relationship.
After drop ships from the Colony arrive, Vice Chancellor Rhodes attempts to take control over the community Clarke built with Bellamy and Wells on Earth. With Sasha's help, Clarke, Wells and Bellamy escaped, but Sasha is killed when she tries to help Octavia. As Mount Weather’s and Rhodes’ forces battle, Clarke, Bellamy and Wells are captured during the initial exchange, but their allies defeat and capture Rhodes before he can execute the trio.
During Sasha's funeral, Clarke reunites with her parents and reconcile with Wells since her parents are actually alive, but will not resume their past relationship because she is now in love with Bellamy, whom she felt happier to be with than when she was with Wells.
Television[edit]
This section needs an improved plot summary. (January 2016)
Background[edit]
Clarke was born in the year of 2131 and raised on the Ark to Jake and Abigail Griffin. Before her imprisonment, Clarke's father discovered that the Ark space station was running out of oxygen, and had an estimated 6 months worth left. He shared this information with Clarke and planned on going public with the information, only to have Abigail report him to the Chancellor in fears it might scare the public after the Chancellor ordered him not to. He was later 'floated', an act in which he is put in an airlock room and the oxygen is released, thus killing him. Clarke acting as an accomplice was imprisoned for treason instead of being 'floated', because she was under the age of 18. Because of her status of prisoner she was considered to be expendable by the council and was volunteered by her mother to be sent down to Earth to test the air to see if it was livable again with 98 other delinquents. Bellamy Blake acting as a guard, snuck onto the drop ship.
Storyline[edit]
In the first season, Clarke and the other 98 delinquents are sent down in an exodus ship which crash lands after Earth's atmosphere cuts all communication and nearly fries the ship. After the ship lands Clarke soon realizes that they landed in the wrong location. They were originally aimed for the Mount Weather complex, a quarantine zone that had food and supplies, only to find out that they were dropped on the wrong mountain.
In 2015, it was confirmed that Clarke is bisexual, making her the first lead character to be LGBT on The CW and making her the first bisexual lead on network television (in reference to the five major networks, ABC, CBS, NBC, The CW and Fox).[1][2][3]
Reception[edit]
This section needs expansion. You can help by adding to it. (December 2015)
The character of Clarke Griffin has received extremely positive praise with some describing her as the "heart and drive" of the show.[4] Clarke was placed in Buzzfeed's "29 amazingly Badass Female characters of 2015[5] and third on Tell-Tale's 5 "TV Heroes Who Crushed It" in 2015.[6]
References[edit]
Jump up ^ "CW's 'The 100' Reveals LGBT Lead Character". TheWrap. Retrieved December 29, 2015.
Jump up ^ "The 100 2x14 Review: Bodyguard of Lies - The Geekiary". The Geekiary. February 26, 2015. Retrieved June 20, 2016.
Jump up ^ "Will The CW Have Its First Bisexual Lead Hero? –". Pop Insomniacs. February 25, 2015. Retrieved June 20, 2016.
Jump up ^ "The Rise and Reign of Clarke Griffin: The 100 Character Spotlight". SciFi Mafia. Retrieved December 29, 2015.
Jump up ^ "29 Amazingly Badass Female TV Characters". BuzzFeed. Retrieved December 29, 2015.
Jump up ^ "5 TV Heroes That Totally Crushed It in 2015". Tell-Tale TV. Retrieved December 29, 2015.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Clarke_Griffin&oldid=838189376"
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text:
Phoenix Open
From Wikipedia, the free encyclopedia
Jump to: navigation, search
This article needs additional citations for verification. Please help improve this article by adding citations to reliable sources. Unsourced material may be challenged and removed. (April 2009) (Learn how and when to remove this template message)
Phoenix Open
Tournament information
Location
Scottsdale, Arizona
Established
1932, 86 years ago
Course(s)
TPC Scottsdale
Par
71
Length
7,266 yards (6,644 m)
Organized by
The Thunderbirds
Tour(s)
PGA Tour
Format
Stroke play
Prize fund
$6.9 million
Month played
February
Tournament record score
Aggregate
256 Mark Calcavecchia (2001)
256 Phil Mickelson (2013)
To par
−28 Mark Calcavecchia (2001)
−28 Phil Mickelson (2013)
Current champion
Gary Woodland
Scottsdale
Location in the United States
Scottsdale
Location in Arizona
The Phoenix Open (known as the Waste Management Phoenix Open for title sponsorship reasons)[1] is a professional golf tournament on the PGA Tour, held in late January/early February at the Tournament Players Club (TPC) of Scottsdale, Arizona.
The tournament was originally the Arizona Open, but was known for most of its history as the Phoenix Open until the investment bank Friedman Billings Ramsey became the title sponsor in October 2003, and it was known as the FBR Open for the next six editions. Waste Management began its sponsorship in 2010.
The event's relaxed atmosphere, raucous by the standards of professional golf, has earned it the nickname “The Greatest Show on Grass” and made it one of the most popular events on the PGA Tour calendar.
Contents
[hide]
1 History
2 Popularity
3 Conflicts with the Super Bowl
4 Records – scoring and victories
5 Winners
6 Multiple winners
7 References
8 External links
History[edit]
The Phoenix Open began 85 years ago in 1932 but was discontinued after the 1935 tournament. The rebirth of the Phoenix Open came in 1939 when Bob Goldwater, Sr. convinced fellow Thunderbirds to help run the event. The Thunderbirds, a prominent civic organization in Phoenix, were not as enthusiastic about running the event as he was, leaving Goldwater, Sr. to do most of the work in getting a golf open started.
The event was played at the Phoenix Country Club in Phoenix (33°28′55″N 112°03′47″W / 33.482°N 112.063°W / 33.482; -112.063),[2] both in its earlier incarnations and after Goldwater resuscitated it. Beginning in 1955, the Arizona Country Club (also in Phoenix) (33°29′06″N 111°57′32″W / 33.485°N 111.959°W / 33.485; -111.959),[3] alternated as event host with Phoenix Country Club; this arrangement lasted until Phoenix Country Club took The Arizona Country Club's turn in 1975 and became the event's permanent home again.
The tournament moved 31 years ago in 1987 to its current home, the Stadium Course at TPC Scottsdale, northeast of downtown Phoenix. The approximate average elevation of the course is 1,530 feet (465 m) above sea level.
Popularity[edit]
The four-day attendance of the tournament is usually around a half million; the best-attended event in golf. In 2016, it set a PGA Tour and Phoenix Open single day attendance record with 201,003 fans in attendance on Saturday, February 6 and set a tournament week attendance record of 618,365 fans.[4]
The most popular location for spectators is the par-3 16th hole, nicknamed "The Coliseum." (33°38′15″N 111°54′48″W / 33.6375°N 111.9132°W / 33.6375; -111.9132) One of the shortest holes on tour at 162 yards (148 m), it is enclosed by a temporary 20,000-seat grandstand. The hole could be described as "one big party," with many students from the nearby Arizona State University in Tempe in attendance. Poor shots at the 16th hole receive boos, because the hole is very easy by the PGA's standards. Good shots, however, are cheered loudly. Famous moments include Tiger Woods' Saturday hole-in-one in 1997, which caused the gallery to erupt, throwing cups and other objects in celebration,[5] and Justin Leonard giving the finger to the gallery after a poor shot. Jarrod Lyle aced the hole on Saturday in 2011, causing the stands to erupt in excitement. After 2013, the PGA Tour banned the practice of caddies racing the 150 yards (140 m) from the tee box to the green, citing injury concerns.[6]
The most popular tour player at the Phoenix Open is unquestionably Phil Mickelson, an Arizona State alumnus (1992) with three victories at the event. In addition to the golf, there is a concert/party held in the Scottsdale area called the Birds Nest, at which music artists like Huey Lewis and the News play.
The Thunderbirds are still highly active in the organization of the tournament. Portions of the proceeds are used by the Thunderbirds to fund Special Olympics activities in Phoenix.
Conflicts with the Super Bowl[edit]
Since 1973,[7] the Phoenix Open has been played on the weekend of the Super Bowl. In 1996, it was played Wednesday through Saturday, as Super Bowl XXX was held at Sun Devil Stadium in nearby Tempe.[8] In 2009, the tournament overlapped with Super Bowl XLIII in Tampa, Florida, when Kenny Perry and Charley Hoffman went to a playoff. That denied the spectators a chance to watch the beginning of the game on NBC, which featured the local Arizona Cardinals.
Because of the Super Bowl weekend status, the PGA Tour's television contracts with CBS and NBC include an alternating tournament. Usually a CBS tournament, the Phoenix Open airs on NBC when CBS has the Super Bowl, and NBC's Honda Classic airs on CBS in Winter Olympic years.
Records – scoring and victories[edit]
The tournament's lowest 72-hole score was set by Mark Calcavecchia in 2001 with 256 (–28), which was matched by Mickelson in 2013. In the second round Calcavecchia scored a 60 (–11), which equalled the lowest score at the Phoenix Open (by Grant Waite in 1996) and subsequently matched by Mickelson in 2005 and 2013. Calcavecchia had 32 birdies in the tournament, which was also an all-time record.
There have been only two double eagles in the history of the Phoenix Open. Tom Pernice, Jr. made the first one on the 558-yard (510 m) par-5 15th hole in 1990. Andrew Magee scored the second on the 332-yard (304 m) par-4 17th hole in 2001, and was the first-ever ace on a par-4 in PGA Tour history.[9]
Four men have won three times at the Phoenix Open: Arnold Palmer won consecutively (1961, 1962, 1963),[10][11] then Gene Littler (1955, 1959, 1969), Calcavecchia (1989, 1992, 2001), and Mickelson (1996, 2005, 2013).
Winners[edit]
Year
Player
Country
Score
To par
Margin
of victory
Runner(s)-up
Winner's
share ($)
Purse ($)
Waste Management Phoenix Open
2018 Gary Woodland United States 266 −18 Playoff Chez Reavie 1,242,000 6,900,000
2017 Hideki Matsuyama (2) Japan 267 −17 Playoff Webb Simpson 1,206,000 6,700,000
2016 Hideki Matsuyama Japan 270 −14 Playoff Rickie Fowler 1,170,000 6,500,000
2015 Brooks Koepka United States 269 −15 1 stroke Hideki Matsuyama
Ryan Palmer
Bubba Watson 1,134,000 6,300,000
2014 Kevin Stadler United States 268 −16 1 stroke Graham DeLaet
Bubba Watson 1,116,000 6,200,000
2013 Phil Mickelson (3) United States 256 −28 4 strokes Brandt Snedeker 1,116,000 6,200,000
2012 Kyle Stanley United States 269 −15 1 stroke Ben Crane 1,098,000 6,100,000
2011 Mark Wilson United States 266 −18 Playoff Jason Dufner 1,098,000 6,100,000
2010 Hunter Mahan United States 268 −16 1 stroke Rickie Fowler 1,080,000 6,000,000
FBR Open
2009 Kenny Perry United States 270 −14 Playoff Charley Hoffman 1,080,000 6,000,000
2008 J. B. Holmes (2) United States 270 −14 Playoff Phil Mickelson 1,080,000 6,000,000
2007 Aaron Baddeley Australia 263 −21 1 stroke John Rollins 1,080,000 6,000,000
2006 J. B. Holmes United States 263 −21 7 strokes J. J. Henry
Steve Lowery
Ryan Palmer
Scott Verplank
Camilo Villegas 936,000 5,200,000
2005 Phil Mickelson (2) United States 267 −17 5 strokes Scott McCarron
Kevin Na 936,000 5,200,000
2004 Jonathan Kaye United States 266 −18 2 strokes Chris DiMarco 936,000 5,200,000
Phoenix Open
2003 Vijay Singh (2) Fiji 261 −23 3 strokes John Huston 720,000 4,000,000
2002 Chris DiMarco United States 267 −17 1 stroke Kenny Perry
Kaname Yokoo 720,000 4,000,000
2001 Mark Calcavecchia (3) United States 256 −28 8 strokes Rocco Mediate 720,000 4,000,000
2000 Tom Lehman United States 270 −14 1 stroke Robert Allenby
Rocco Mediate 576,000 3,200,000
1999 Rocco Mediate United States 273 −11 2 strokes Justin Leonard 540,000 3,000,000
1998 Jesper Parnevik Sweden 269 −15 3 strokes Tommy Armour III
Brent Geiberger
Steve Pate
Tom Watson 450,000 2,500,000
1997 Steve Jones United States 258 −26 11 strokes Jesper Parnevik 270,000 1,500,000
1996 Phil Mickelson United States 269 −15 Playoff Justin Leonard 234,000 1,300,000
1995 Vijay Singh Fiji 269 −15 Playoff Billy Mayfair 234,000 1,300,000
1994 Bill Glasson United States 268 −16 3 strokes Bob Estes 216,000 1,200,000
1993 Lee Janzen United States 273 −11 2 strokes Andrew Magee 180,000 1,000,000
1992 Mark Calcavecchia (2) United States 264 −20 5 strokes Duffy Waldorf 180,000 1,000,000
1991 Nolan Henke United States 268 −16 1 stroke Gil Morgan
Curtis Strange
Tom Watson 180,000 1,000,000
1990 Tommy Armour III United States 267 −17 5 strokes Jim Thorpe 162,000 900,000
1989 Mark Calcavecchia United States 263 −21 7 strokes Chip Beck 126,000 700,000
1988 Sandy Lyle Scotland 269 −15 Playoff Fred Couples 117,000 650,000
1987 Paul Azinger United States 268 −16 1 stroke Hal Sutton 108,000 600,000
1986 Hal Sutton United States 267 −17 2 strokes Calvin Peete
Tony Sills 90,000 500,000
1985 Calvin Peete United States 270 −14 2 strokes Morris Hatalsky
Doug Tewell 81,000 450,000
1984 Tom Purtzer United States 268 −16 1 stroke Corey Pavin 72,000 400,000
1983 Bob Gilder (2) United States 271 −13 Playoff Rex Caldwell
Johnny Miller
Mark O'Meara 63,000 350,000
1982 Lanny Wadkins United States 263 −21 6 strokes Jerry Pate 54,000 300,000
1981 David Graham Australia 268 −16 1 stroke Lon Hinkle 54,000 300,000
1980 Jeff Mitchell United States 272 −12 4 strokes Rik Massengale 54,000 300,000
1979 Ben Crenshaw United States 199* −14 1 stroke Jay Haas 33,750 250,000
1978 Miller Barber United States 272 −12 1 stroke Jerry Pate
Lee Trevino 40,000 200,000
1977 Jerry Pate United States 277 −7 Playoff Dave Stockton 40,000 200,000
1976 Bob Gilder United States 268 −16 2 strokes Roger Maltbie 40,000 200,000
1975 Johnny Miller (2) United States 260 −24 14 strokes Jerry Heard 30,000 150,000
1974 Johnny Miller United States 271 −13 1 stroke Lanny Wadkins 30,000 150,000
1973 Bruce Crampton Australia 268 −12 1 stroke Steve Melnyk
Lanny Wadkins 30,000 150,000
1972 Homero Blancas United States 273 −11 Playoff Lanny Wadkins 25,000 125,000
Phoenix Open Invitational
1971 Miller Barber United States 261 −23 2 strokes Billy Casper
Dan Sikes 25,000 125,000
1970 Dale Douglass United States 271 −13 1 stroke Howie Johnson
Gene Littler 20,000 100,000
1969 Gene Littler (3) United States 263 −21 2 strokes Miller Barber
Don January
Billy Maxwell 20,000 100,000
1968 George Knudson Canada 272 −12 3 strokes Julius Boros
Sam Carmichael
Jack Montgomery 20,000 100,000
1967 Julius Boros United States 272 −12 1 stroke Ken Still 14,000 70,000
1966 Dudley Wysong United States 278 −6 1 stroke Gardner Dickinson 9,000 60,000
1965 Rod Funseth United States 274 −14 3 strokes Bert Yancey 10,500 65,000
1964 Jack Nicklaus United States 271 −13 3 strokes Bob Brue 7,500 50,000
1963 Arnold Palmer (3) United States 273 −15 1 stroke Gary Player 5,300 35,000
1962 Arnold Palmer (2) United States 269 −15 12 strokes Billy Casper
Don Fairfield
Bob McCallister
Jack Nicklaus 5,300 35,000
1961 Arnold Palmer United States 270 −10 Playoff Doug Sanders 4,300 30,000
1960 Jack Fleck United States 273 −11 Playoff Bill Collins 3,150 22,500
1959 Gene Littler (2) United States 268 −12 1 stroke Art Wall, Jr. 2,400 20,000
1958 Ken Venturi United States 274 −10 1 stroke Walter Burkemo
Jay Hebert 2,000 15,000
1957 Billy Casper United States 271 −9 3 strokes Cary Middlecoff
Mike Souchak 2,000 15,000
Phoenix Open
1956 Cary Middlecoff United States 276 −8 3 strokes Mike Souchak 2,400 15,000
1955 Gene Littler United States 275 −5 1 stroke Billy Maxwell
Johnny Palmer 2,400 15,000
1954 Ed Furgol United States 272 −12 Playoff Cary Middlecoff 2,000 10,000
1953 Lloyd Mangrum (2) United States 272 −12 6 strokes Johnny Bulla
Ted Kroll
Bo Wininger 2,000 10,000
1952 Lloyd Mangrum United States 274 −10 5 strokes E. J. Harrison 2,000 10,000
1951 Lew Worsham United States 272 −12 1 stroke Lawson Little 2,000 10,000
Ben Hogan Open
1950 Jimmy Demaret (2) United States 269 −15 1 stroke Sam Snead 2,000 10,000
Phoenix Open
1949 Jimmy Demaret United States 278 −6 Playoff Ben Hogan 2,000 10,000
1948 Bobby Locke South Africa 268 −16 1 stroke Jimmy Demaret 2,000 10,000
1947 Ben Hogan (2) United States 270 −14 7 strokes Lloyd Mangrum
Ed Oliver 2,000 10,000
1946 Ben Hogan United States 273 −11 Playoff Herman Keiser 1,500 7,500
1945 Byron Nelson (2) United States 274 −10 2 strokes Denny Shute 1,000 5,000
1944 Jug McSpaden United States 273 −11 Playoff Byron Nelson 1,000 5,000
1941–43: No tournament (hosted Western Open in 1941 and 1942)
1940 Ed Oliver United States 205^ −8 1 stroke Ben Hogan 700 3,000
1939 Byron Nelson United States 198^ −15 12 strokes Ben Hogan 700 3,000
1936–38: No tournament
1935 Ky Laffoon United States 281 −3 4 strokes Craig Wood 500 2,500
1934 No tournament
Arizona Open
1933 Harry Cooper United States 281 −3 2 strokes Ray Mangrum
Horton Smith 400 1,500
1932 Ralph Guldahl United States 285 −1 5 strokes John Perelli 600 2,500
*Rain-shortened to 54 holes
^Scheduled 54 holes
Note: Green highlight indicates scoring records.
Sources[12][13][14]
Multiple winners[edit]
Fourteen men have won this tournament more than once.
3 wins
Arnold Palmer: 1961, 1962, 1963 (consecutive)[10][11]
Gene Littler: 1955, 1959, 1969
Mark Calcavecchia: 1989, 1992, 2001
Phil Mickelson: 1996, 2005, 2013
2 wins
Byron Nelson: 1939, 1945
Ben Hogan: 1946, 1947 (consecutive)[15][16]
Jimmy Demaret: 1949, 1950 (consecutive)[17]
Lloyd Mangrum: 1952, 1953
Johnny Miller: 1974, 1975 (consecutive)[18][19]
Miller Barber: 1971, 1978
Bob Gilder: 1976, 1983
Vijay Singh: 1995, 2003
J. B. Holmes: 2006, 2008
Hideki Matsuyama: 2016, 2017 (consecutive)
References[edit]
Jump up ^ "Waste Management to sponsor Phoenix Open". PGA Tour. December 9, 2009. Retrieved March 13, 2013.
Jump up ^ "Golf". Phoenix Country Club. Retrieved February 4, 2017.
Jump up ^ "Golf". Arizona Country Club. Retrieved February 4, 2017.
Jump up ^ "Waste Management Phoenix Open attendance records". AZ Central. February 7, 2016.
Jump up ^ "Jones maintains Phoenix lead; Woods records ace on No. 16". Victoria Advocate. (Texas). January 26, 1997. p. 6B.
Jump up ^ http://www.golfchannel.com/news/golftalkcentral/tour-bans-caddie-races-tpc-scottsdale-colonial/
Jump up ^ "Crampton's birdie nets Phoenix win". Wilmington Morning Star. (North Carolina). Associated Press. January 15, 1973. p. 16.
Jump up ^ "Mickelson grinds out another win". Eugene Register-Guard. (Oregon). Associated Press. January 28, 1996. p. 3F.
Jump up ^ Kelley, Brent. "The Amazing Story of the Only Par-4 Hole-in-One in PGA Tour History". thoughtco.com. Retrieved October 4, 2017.
^ Jump up to: a b "Bee 'helps' Palmer win Phoenix Open". Pittsburgh Press. UPI. February 13, 1963. p. 50.
^ Jump up to: a b "Palmer wins Phoenix Open". Eugene Register-Guard. (Oregon). Associated Press. February 13, 1963. p. 1C.
Jump up ^ 2015 Waste Management Phoenix Open Media Guide – Section 14: Top Finishers 1932–2014 – at wmphoenixopen.com
Jump up ^ Phoenix Open – Winners Archived 2014-06-01 at the Wayback Machine. – at www.pgatour.com
Jump up ^ Phoenix Open – Winners – at golfobserver.com
Jump up ^ "Hogan wins Phoenix Open; trouble looms". Eugene Register-Guard. (Oregon). United Press. January 27, 1947. p. 5.
Jump up ^ "Ben Hogan wins Phoenix tourney". Spokane Daily Chronicle. (Washington). Associated Press. January 27, 1947. p. 13.
Jump up ^ "Demaret winner of Phoenix golf". Spokane Daily Chronicle. (Washington). Associated Press. January 30, 1950. p. 11.
Jump up ^ "Miller shoots 64 for 14-shot edge". Spokesman-Review. (Spokane, Washington). Associated Press. January 13, 1975. p. 13.
Jump up ^ "Miller maybe world's best". Deseret News. (Salt Lake City, Utah). UPI. January 13, 1975. p. 8B.
External links[edit]
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Coordinates: 33°38′N 111°55′W / 33.64°N 111.91°W / 33.64; -111.91
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