text stringlengths 4 7.07k | text_hash stringlengths 32 32 | __index_level_0__ int64 1 1.81M |
|---|---|---|
= = = = Binary stars = = = =
| 4cf4468db9160561bacb4f0e14145547 | 36,162 |
The post β main @-@ sequence evolution of binary stars may be significantly different from the evolution of single stars of the same mass . If stars in a binary system are sufficiently close , when one of the stars expands to become a red giant it may overflow its Roche lobe , the region around a star where material i... | 56ab9062f89f4e128dead819c72b4d42 | 36,164 |
= = Distribution = =
| 008ab98ccbb39f1d44d6090122c744d7 | 36,166 |
In addition to isolated stars , a multi @-@ star system can consist of two or more gravitationally bound stars that orbit each other . The simplest and most common multi @-@ star system is a binary star , but systems of three or more stars are also found . For reasons of orbital stability , such multi @-@ star systems... | 5f46030775ccc097d82f39ce6224a560 | 36,168 |
It has been a long @-@ held assumption that the majority of stars occur in gravitationally bound , multiple @-@ star systems . This is particularly true for very massive O and B class stars , where 80 % of the stars are believed to be part of multiple @-@ star systems . The proportion of single star systems increases ... | 3ae84cc51e868172f435fa749342dea8 | 36,169 |
Stars are not spread uniformly across the universe , but are normally grouped into galaxies along with interstellar gas and dust . A typical galaxy contains hundreds of billions of stars , and there are more than 100 billion ( 1011 ) galaxies in the observable universe . In 2010 , one estimate of the number of stars i... | d52699ee71f41cd081e21d013f4ecf71 | 36,170 |
The nearest star to the Earth , apart from the Sun , is Proxima Centauri , which is 39 @.@ 9 trillion kilometres , or 4 @.@ 2 light @-@ years . Travelling at the orbital speed of the Space Shuttle ( 8 kilometres per second β almost 30 @,@ 000 kilometres per hour ) , it would take about 150 @,@ 000 years to arrive . Th... | d48a75c92226e1df3e2b5dfb1e77abd0 | 36,171 |
Due to the relatively vast distances between stars outside the galactic nucleus , collisions between stars are thought to be rare . In denser regions such as the core of globular clusters or the galactic center , collisions can be more common . Such collisions can produce what are known as blue stragglers . These abno... | da2eb2eeb379118a00472faddc501fb9 | 36,172 |
= = Characteristics = =
| 7578e00b1806474d133aedda48bbb013 | 36,174 |
Almost everything about a star is determined by its initial mass , including such characteristics as luminosity , size , evolution , lifespan , and its eventual fate .
| 68569f11d197fa2f8f9b040c3e4b9b7a | 36,176 |
= = = Age = = =
| 4a95f9d1c7525ddf0f304a48f13c89c7 | 36,178 |
Most stars are between 1 billion and 10 billion years old . Some stars may even be close to 13 @.@ 8 billion years old β the observed age of the universe . The oldest star yet discovered , HD 140283 , nicknamed Methuselah star , is an estimated 14 @.@ 46 Β± 0 @.@ 8 billion years old . ( Due to the uncertainty in the va... | 654eb0c27353a1ce7c61861f96829f27 | 36,180 |
The more massive the star , the shorter its lifespan , primarily because massive stars have greater pressure on their cores , causing them to burn hydrogen more rapidly . The most massive stars last an average of a few million years , while stars of minimum mass ( red dwarfs ) burn their fuel very slowly and can last ... | d0666e4ad0fc112efa80a99c16344104 | 36,181 |
= = = Chemical composition = = =
| ae97336f4d5ae55a487d7acdc9a468e1 | 36,183 |
When stars form in the present Milky Way galaxy they are composed of about 71 % hydrogen and 27 % helium , as measured by mass , with a small fraction of heavier elements . Typically the portion of heavy elements is measured in terms of the iron content of the stellar atmosphere , as iron is a common element and its a... | 53877c1607e1aae8cbe45d956f8b0f93 | 36,185 |
The star with the lowest iron content ever measured is the dwarf HE1327 @-@ 2326 , with only 1 / 200,000th the iron content of the Sun . By contrast , the super @-@ metal @-@ rich star ΞΌ Leonis has nearly double the abundance of iron as the Sun , while the planet @-@ bearing star 14 Herculis has nearly triple the iron... | c48210a648222f300884c81d25f8835e | 36,186 |
= = = Diameter = = =
| c4a070d7bfa1821d1f1e609dc8f3eeeb | 36,188 |
Due to their great distance from the Earth , all stars except the Sun appear to the unaided eye as shining points in the night sky that twinkle because of the effect of the Earth 's atmosphere . The Sun is also a star , but it is close enough to the Earth to appear as a disk instead , and to provide daylight . Other t... | 1a0fddcef51f579ee100288cced2e48c | 36,190 |
The disks of most stars are much too small in angular size to be observed with current ground @-@ based optical telescopes , and so interferometer telescopes are required to produce images of these objects . Another technique for measuring the angular size of stars is through occultation . By precisely measuring the d... | 1cf853bc8c9188ed78077936024f16b0 | 36,191 |
Stars range in size from neutron stars , which vary anywhere from 20 to 40 km ( 25 mi ) in diameter , to supergiants like Betelgeuse in the Orion constellation , which has a diameter approximately 1 @,@ 070 times that of the Sun β about 1 @,@ 490 @,@ 171 @,@ 880 km ( 925 @,@ 949 @,@ 878 mi ) . Betelgeuse , however , h... | e4a6293052a6373a43b0b145780c9d83 | 36,192 |
= = = Kinematics = = =
| d2a132eac895997d5fa0a6c2c3db68ab | 36,194 |
The motion of a star relative to the Sun can provide useful information about the origin and age of a star , as well as the structure and evolution of the surrounding galaxy . The components of motion of a star consist of the radial velocity toward or away from the Sun , and the traverse angular movement , which is ca... | 023a8c11d0564d4507fc19d4c7d8d78c | 36,196 |
Radial velocity is measured by the doppler shift of the star 's spectral lines , and is given in units of km / s . The proper motion of a star , its parallax , is determined by precise astrometric measurements in units of milli @-@ arc seconds ( mas ) per year . With knowledge of the star 's parallax and its distance ... | 574a59b550b2176b853085864638541a | 36,197 |
When both rates of movement are known , the space velocity of the star relative to the Sun or the galaxy can be computed . Among nearby stars , it has been found that younger population I stars have generally lower velocities than older , population II stars . The latter have elliptical orbits that are inclined to the... | 2184c10779e67d5d84a6a4b44ccc02af | 36,198 |
= = = Magnetic field = = =
| 281399724c4f9260f1116ab1ae1f7b02 | 36,200 |
The magnetic field of a star is generated within regions of the interior where convective circulation occurs . This movement of conductive plasma functions like a dynamo , wherein the movement of elecrical charges induce magnetic fields , as does a mechanical dynamo . Those magnetic fields have a great range that exte... | 21bb778d3db787a6ba7c7ed0fe87ea7f | 36,202 |
Young , rapidly rotating stars tend to have high levels of surface activity because of their magnetic field . The magnetic field can act upon a star 's stellar wind , functioning as a brake to gradually slow the rate of rotation with time . Thus , older stars such as the Sun have a much slower rate of rotation and a l... | 894ca5e414c025f9a07a09756cefc2dd | 36,203 |
= = = Mass = = =
| c281ed249493569059ec4a5fc7e05e5b | 36,205 |
One of the most massive stars known is Eta Carinae , which , with 100 β 150 times as much mass as the Sun , will have a lifespan of only several million years . Studies of the most massive open clusters suggests 150 M β as an upper limit for stars in the current era of the universe . This represents an empirical value... | c890b8d0b3f6f07665fb545c9d2968a3 | 36,207 |
The first stars to form after the Big Bang may have been larger , up to 300 M β , due to the complete absence of elements heavier than lithium in their composition . This generation of supermassive population III stars is likely to have existed in the very early universe ( i.e. , they are observed to have a high redsh... | 6eccf97b62f0874623e5dcae19203658 | 36,208 |
With a mass only 80 times that of Jupiter ( MJ ) , 2MASS J0523 @-@ 1403 is the smallest known star undergoing nuclear fusion in its core . For stars with metallicity similar to the Sun , the theoretical minimum mass the star can have and still undergo fusion at the core , is estimated to be about 75 MJ . When the meta... | d8559c14f6cdb66876360366c73fd966 | 36,209 |
The combination of the radius and the mass of a star determines its surface gravity . Giant stars have a much lower surface gravity than do main sequence stars , while the opposite is the case for degenerate , compact stars such as white dwarfs . The surface gravity can influence the appearance of a star 's spectrum ,... | 33ee9fb11d55d28d1d96075b311dd443 | 36,210 |
= = = Rotation = = =
| 86ff79bd0c7d2ee7e5de097a52124a5e | 36,212 |
The rotation rate of stars can be determined through spectroscopic measurement , or more exactly determined by tracking their starspots . Young stars can have a rotation greater than 100 km / s at the equator . The B @-@ class star Achernar , for example , has an equatorial velocity of about 225 km / s or greater , ca... | dd909a327b610f766d5a8ab277cf2377 | 36,214 |
Degenerate stars have contracted into a compact mass , resulting in a rapid rate of rotation . However they have relatively low rates of rotation compared to what would be expected by conservation of angular momentum β the tendency of a rotating body to compensate for a contraction in size by increasing its rate of sp... | 2c4e6f4773ec2790ee66aee338b9689a | 36,215 |
= = = Temperature = = =
| 9eee63a38eee53880d5cd6ab99cc3413 | 36,217 |
The surface temperature of a main sequence star is determined by the rate of energy production of its core and by its radius , and is often estimated from the star 's color index . The temperature is normally given in terms of an effective temperature , which is the temperature of an idealized black body that radiates... | 954577f6ae09cefed721b7d533fbae26 | 36,219 |
The stellar temperature will determine the rate of ionization of various elements , resulting in characteristic absorption lines in the spectrum . The surface temperature of a star , along with its visual absolute magnitude and absorption features , is used to classify a star ( see classification below ) .
| 45fd16500dc157adbcd7727b912ab147 | 36,220 |
Massive main sequence stars can have surface temperatures of 50 @,@ 000 K. Smaller stars such as the Sun have surface temperatures of a few thousand K. Red giants have relatively low surface temperatures of about 3 @,@ 600 K ; but they also have a high luminosity due to their large exterior surface area .
| 4f82b16e78a1e46f54472afb92e5aee9 | 36,221 |
= = Radiation = =
| 57e7bfad29f2a344eb239e3fb74e27c9 | 36,223 |
The energy produced by stars , a product of nuclear fusion , radiates to space as both electromagnetic radiation and particle radiation . The particle radiation emitted by a star is manifested as the stellar wind , which streams from the outer layers as electrically charged protons and alpha and beta particles . Altho... | e498206057c4932e02213d3f4f258c87 | 36,225 |
The production of energy at the core is the reason stars shine so brightly : every time two or more atomic nuclei fuse together to form a single atomic nucleus of a new heavier element , gamma ray photons are released from the nuclear fusion product . This energy is converted to other forms of electromagnetic energy o... | 3a1665a905ad057e18d904ca1044f6d8 | 36,226 |
The color of a star , as determined by the most intense frequency of the visible light , depends on the temperature of the star 's outer layers , including its photosphere . Besides visible light , stars also emit forms of electromagnetic radiation that are invisible to the human eye . In fact , stellar electromagneti... | 12112756f86195b5eb5396dc264b1e69 | 36,227 |
Using the stellar spectrum , astronomers can also determine the surface temperature , surface gravity , metallicity and rotational velocity of a star . If the distance of the star is found , such as by measuring the parallax , then the luminosity of the star can be derived . The mass , radius , surface gravity , and r... | a6e3a19fd0d4fde86e7aa73303a112bb | 36,228 |
= = = Luminosity = = =
| bad0ab405597a39831627180ce8614d6 | 36,230 |
The luminosity of a star is the amount of light and other forms of radiant energy it radiates per unit of time . It has units of power . The luminosity of a star is determined by its radius and surface temperature . Many stars do not radiate uniformly across their entire surface . The rapidly rotating star Vega , for ... | 984e153b04e295336c89fcd309943982 | 36,232 |
Patches of the star 's surface with a lower temperature and luminosity than average are known as starspots . Small , dwarf stars such as our Sun generally have essentially featureless disks with only small starspots . Giant stars have much larger , more obvious starspots , and they also exhibit strong stellar limb dar... | c897061f568b3e069c18b5e7ab654ae1 | 36,233 |
= = = Magnitude = = =
| d12d504f79ac056ea772871a8b561868 | 36,235 |
The apparent brightness of a star is expressed in terms of its apparent magnitude . It is a function of the star 's luminosity , its distance from Earth , and the altering of the star 's light as it passes through Earth 's atmosphere . Intrinsic or absolute magnitude is directly related to a star 's luminosity , and i... | fbf1eb081d4004c6f54eab8cc9cfd3c1 | 36,237 |
Both the apparent and absolute magnitude scales are logarithmic units : one whole number difference in magnitude is equal to a brightness variation of about 2 @.@ 5 times ( the 5th root of 100 or approximately 2 @.@ 512 ) . This means that a first magnitude star ( + 1 @.@ 00 ) is about 2 @.@ 5 times brighter than a se... | a49df4b019183a904c40434b011ec98e | 36,238 |
On both apparent and absolute magnitude scales , the smaller the magnitude number , the brighter the star ; the larger the magnitude number , the fainter the star . The brightest stars , on either scale , have negative magnitude numbers . The variation in brightness ( ΞL ) between two stars is calculated by subtractin... | 1300163e48113cb8c02545d1c25a04ba | 36,239 |
<formula>
| 79c2f3e78aa986c8331905878dada39f | 36,240 |
<formula>
| 79c2f3e78aa986c8331905878dada39f | 36,241 |
Relative to both luminosity and distance from Earth , a star 's absolute magnitude ( M ) and apparent magnitude ( m ) are not equivalent ; for example , the bright star Sirius has an apparent magnitude of β 1 @.@ 44 , but it has an absolute magnitude of + 1 @.@ 41 .
| a1daabaae3146fd92e477c7ea4fa277e | 36,242 |
The Sun has an apparent magnitude of β 26 @.@ 7 , but its absolute magnitude is only + 4 @.@ 83 . Sirius , the brightest star in the night sky as seen from Earth , is approximately 23 times more luminous than the Sun , while Canopus , the second brightest star in the night sky with an absolute magnitude of β 5 @.@ 53 ... | 1eede66c5065664ce39963e152c76922 | 36,243 |
As of 2006 , the star with the highest known absolute magnitude is LBV 1806 @-@ 20 , with a magnitude of β 14 @.@ 2 . This star is at least 5 @,@ 000 @,@ 000 times more luminous than the Sun . The least luminous stars that are currently known are located in the NGC 6397 cluster . The faintest red dwarfs in the cluster... | 52688d230da8f3098129e042bb1bf7e3 | 36,244 |
= = Classification = =
| 1fa799726c451f719162ca39992e2485 | 36,246 |
The current stellar classification system originated in the early 20th century , when stars were classified from A to Q based on the strength of the hydrogen line . It thought that the hydrogen line strength was a simple linear function of temperature . Rather , it was more complicated ; it strengthened with increasin... | 7c79e7cf8b933ee7508d96b808827ef5 | 36,248 |
Stars are given a single @-@ letter classification according to their spectra , ranging from type O , which are very hot , to M , which are so cool that molecules may form in their atmospheres . The main classifications in order of decreasing surface temperature are : O , B , A , F , G , K , and M. A variety of rare s... | 21ce65d13c8a451f7b7c58b3d5f87dbe | 36,249 |
In addition , stars may be classified by the luminosity effects found in their spectral lines , which correspond to their spatial size and is determined by their surface gravity . These range from 0 ( hypergiants ) through III ( giants ) to V ( main sequence dwarfs ) ; some authors add VII ( white dwarfs ) . Most star... | 933654e505974c27947e94b5c737e6b9 | 36,250 |
Additional nomenclature , in the form of lower @-@ case letters added to the end of the spectral type to indicate peculiar features of the spectrum . For example , an " e " can indicate the presence of emission lines ; " m " represents unusually strong levels of metals , and " var " can mean variations in the spectral... | cba175661a8a40c98182d7a2078b47f8 | 36,251 |
White dwarf stars have their own class that begins with the letter D. This is further sub @-@ divided into the classes DA , DB , DC , DO , DZ , and DQ , depending on the types of prominent lines found in the spectrum . This is followed by a numerical value that indicates the temperature .
| 900ecb17e69a951b482080a09fff98d7 | 36,252 |
= = Variable stars = =
| 1415046443fb84f44460389e41aa7dec | 36,254 |
Variable stars have periodic or random changes in luminosity because of intrinsic or extrinsic properties . Of the intrinsically variable stars , the primary types can be subdivided into three principal groups .
| 74e4d10c302b43144d46efc44af11e0c | 36,256 |
During their stellar evolution , some stars pass through phases where they can become pulsating variables . Pulsating variable stars vary in radius and luminosity over time , expanding and contracting with periods ranging from minutes to years , depending on the size of the star . This category includes Cepheid and Ce... | bb659556afb36802b60c66eb048e7f75 | 36,257 |
Eruptive variables are stars that experience sudden increases in luminosity because of flares or mass ejection events . This group includes protostars , Wolf @-@ Rayet stars , and flare stars , as well as giant and supergiant stars .
| e4fda1ad35ba46a08a99cc258456f631 | 36,258 |
Cataclysmic or explosive variable stars are those that undergo a dramatic change in their properties . This group includes novae and supernovae . A binary star system that includes a nearby white dwarf can produce certain types of these spectacular stellar explosions , including the nova and a Type 1a supernova . The ... | 8e239fa0f1c13b7dee3d31d2cd041034 | 36,259 |
Stars can also vary in luminosity because of extrinsic factors , such as eclipsing binaries , as well as rotating stars that produce extreme starspots . A notable example of an eclipsing binary is Algol , which regularly varies in magnitude from 2 @.@ 3 to 3 @.@ 5 over a period of 2 @.@ 87 days .
| 134da28a4c451736b7e81f5ae8a3372a | 36,260 |
= = Structure = =
| e86941bee721ef15e6abd6a93e41179a | 36,262 |
The interior of a stable star is in a state of hydrostatic equilibrium : the forces on any small volume almost exactly counterbalance each other . The balanced forces are inward gravitational force and an outward force due to the pressure gradient within the star . The pressure gradient is established by the temperatu... | c51b85a7fce33afabb1595e0c22e5566 | 36,264 |
As atomic nuclei are fused in the core , they emit energy in the form of gamma rays . These photons interact with the surrounding plasma , adding to the thermal energy at the core . Stars on the main sequence convert hydrogen into helium , creating a slowly but steadily increasing proportion of helium in the core . Ev... | 6af06554db2a9f3901b13dc3d0d2b888 | 36,265 |
In addition to hydrostatic equilibrium , the interior of a stable star will also maintain an energy balance of thermal equilibrium . There is a radial temperature gradient throughout the interior that results in a flux of energy flowing toward the exterior . The outgoing flux of energy leaving any layer within the sta... | 2e6d95f5e3b4a6a36ac6de4d737cf7c6 | 36,266 |
The radiation zone is the region of the stellar interior where the flux of energy outward is dependent on radiative heat transfer , since convective heat transfer is inefficient in that zone . In this region the plasma will not be perturbed , and any mass motions will die out . If this is not the case , however , then... | fe252582e99d4208ea01d38872300f38 | 36,267 |
The occurrence of convection in the outer envelope of a main sequence star depends on the star 's mass . Stars with several times the mass of the Sun have a convection zone deep within the interior and a radiative zone in the outer layers . Smaller stars such as the Sun are just the opposite , with the convective zone... | 8e48e94100c05bf260c505c7b7102030 | 36,268 |
The photosphere is that portion of a star that is visible to an observer . This is the layer at which the plasma of the star becomes transparent to photons of light . From here , the energy generated at the core becomes free to propagate into space . It is within the photosphere that sun spots , regions of lower than ... | 728f3d4215481d5d9e21bf0d1a16cd0b | 36,269 |
Above the level of the photosphere is the stellar atmosphere . In a main sequence star such as the Sun , the lowest level of the atmosphere , just above the photosphere , is the thin chromosphere region , where spicules appear and stellar flares begin . Above this is the transition region , where the temperature rapid... | 0c837bbce15c01a4662994bb1e21e9c6 | 36,270 |
From the corona , a stellar wind of plasma particles expands outward from the star , until it interacts with the interstellar medium . For the Sun , the influence of its solar wind extends throughout a bubble @-@ shaped region called the heliosphere .
| 36b9f42d99d02b7be278f580fb1003ab | 36,271 |
= = Nuclear fusion reaction pathways = =
| 70fd3b3805cffab936934a5e09a99ff2 | 36,273 |
A variety of nuclear fusion reactions take place in the cores of stars , that depend upon their mass and composition . When nuclei fuse , the mass of the fused product is less than the mass of the original parts . This lost mass is converted to electromagnetic energy , according to the mass @-@ energy equivalence rela... | ee22a23f94ee6b2bef67cc1dead830b9 | 36,275 |
The hydrogen fusion process is temperature @-@ sensitive , so a moderate increase in the core temperature will result in a significant increase in the fusion rate . As a result , the core temperature of main sequence stars only varies from 4 million kelvin for a small M @-@ class star to 40 million kelvin for a massiv... | da092ca8fc34b7cbbddf2adf26ee5f6b | 36,276 |
In the Sun , with a 10 @-@ million @-@ kelvin core , hydrogen fuses to form helium in the proton @-@ proton chain reaction :
| 9890450a3a8ace78c91012592d82c011 | 36,277 |
41H β 22H + 2e + + 2Ξ½e ( 2 x 0 @.@ 4 MeV )
| 554effd767aa7e477f8d5ed014626c47 | 36,278 |
2e + + 2e- β 2Ξ³ ( 2 x 1 @.@ 0 MeV )
| 8b67cfbb3f78799359cd8acd942749f8 | 36,279 |
21H + 22H β 23He + 2Ξ³ ( 2 x 5 @.@ 5 MeV )
| 402418c4bb303354b735265d63a2b587 | 36,280 |
23He β 4He + 21H ( 12 @.@ 9 MeV )
| 4ebb1d28ee9c9eb8c9b22468f9d8b67c | 36,281 |
These reactions result in the overall reaction :
| e212ede7fb9e47a453461ca8fc9cb00c | 36,282 |
41H β 4He + 2e + + 2Ξ³ + 2Ξ½e ( 26 @.@ 7 MeV )
| 7ed50b4430b7e1886cf4b46a65d933c5 | 36,283 |
where e + is a positron , Ξ³ is a gamma ray photon , Ξ½e is a neutrino , and H and He are isotopes of hydrogen and helium , respectively . The energy released by this reaction is in millions of electron volts , which is actually only a tiny amount of energy . However enormous numbers of these reactions occur constantly ... | ad84b3825427829957c519743fe49af4 | 36,284 |
In more massive stars , helium is produced in a cycle of reactions catalyzed by carbon called the carbon @-@ nitrogen @-@ oxygen cycle .
| 945ea45b75dcb8e00765cafd9f788bbf | 36,285 |
In evolved stars with cores at 100 million kelvin and masses between 0 @.@ 5 and 10 M β , helium can be transformed into carbon in the triple @-@ alpha process that uses the intermediate element beryllium :
| 51d77c391fc32709cf6955920eb15b03 | 36,286 |
4He + 4He + 92 keV β 8 * Be
| 5a9f951a59122551e46a654ad6018e3a | 36,287 |
4He + 8 * Be + 67 keV β 12 * C
| afc757b86b079fb9990a0f2ee8a69b5c | 36,288 |
12 * C β 12C + Ξ³ + 7 @.@ 4 MeV
| 9525cf3cf5247eb085776a51c4fe7809 | 36,289 |
For an overall reaction of :
| d03f481384f52bef9c07824690da7d85 | 36,290 |
34He β 12C + Ξ³ + 7 @.@ 2 MeV
| 456008954fa5c176dc4a416206d02b0a | 36,291 |
In massive stars , heavier elements can also be burned in a contracting core through the neon burning process and oxygen burning process . The final stage in the stellar nucleosynthesis process is the silicon burning process that results in the production of the stable isotope iron @-@ 56 , an endothermic process that... | d9c72c90b73d1681fc6620484d1bd374 | 36,292 |
The example below shows the amount of time required for a star of 20 M β to consume all of its nuclear fuel . As an O @-@ class main sequence star , it would be 8 times the solar radius and 62 @,@ 000 times the Sun 's luminosity .
| d9a09e4ab927380acdbce4591a051519 | 36,293 |
= Perry the Platypus =
| 069ced6d8299ad0e44ee265de700ff92 | 36,296 |
Perry the Platypus , also known as Agent P or simply Perry , is an anthropomorphic platypus from the animated series Phineas and Ferb . Perry was created by the series ' co @-@ founders , Dan Povenmire and Jeff " Swampy " Marsh . He first appeared along with the majority of the main cast in the pilot episode " Rollerc... | 56998233c2d99f5f512263dacd7b5316 | 36,298 |
Perry is the pet platypus of the Flynn @-@ Fletcher family , and is perceived as mindless and domesticated . In secret , however , he lives a double life as a member of an all @-@ animal espionage organization referred to as O.W.C.A. ( The Organization Without a Cool Acronym ) . Many secret entrances to his undergroun... | 5b6197334fd28ce65df757637a447785 | 36,299 |
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