This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
The full set of rings, imaged as Saturn eclipsed the Sun from the vantage of the Cassini orbiter, 1.2 million km (¾ million miles) distant, on 19 July 2013 (brightness is exaggerated). Earth appears as a dot at 4 o'clock, between the G and E rings.
The rings of Saturn are the most extensive and complex ring system of any planet in the Solar System. They consist of countless small particles, ranging in size from micrometers to meters,[1] that orbit around Saturn. The ring particles are made almost entirely of water ice, with a trace component of rocky material. There is still no consensus as to their mechanism of formation. Although theoretical models indicated that the rings were likely to have formed early in the Solar System's history,[2] newer data from Cassini suggested they formed relatively late.[3]
Although reflection from the rings increases Saturn's brightness, they are not visible from Earth with unaided vision. In 1610, the year after Galileo Galilei turned a telescope to the sky, he became the first person to observe Saturn's rings, though he could not see them well enough to discern their true nature. In 1655, Christiaan Huygens was the first person to describe them as a disk surrounding Saturn.[4] The concept that Saturn's rings are made up of a series of tiny ringlets can be traced to Pierre-Simon Laplace,[4] although true gaps are few – it is more correct to think of the rings as an annular disk with concentric local maxima and minima in density and brightness.[2] On the scale of the clumps within the rings there is much empty space.
The rings have numerous gaps where particle density drops sharply: two opened by known moons embedded within them, and many others at locations of known destabilizing orbital resonances with the moons of Saturn. Other gaps remain unexplained. Stabilizing resonances, on the other hand, are responsible for the longevity of several rings, such as the Titan Ringlet and the G Ring.
Well beyond the main rings is the Phoebe ring, which is presumed to originate from Phoebe and thus share its retrograde orbital motion. It is aligned with the plane of Saturn's orbit. Saturn has an axial tilt of 27 degrees, so this ring is tilted at an angle of 27 degrees to the more visible rings orbiting above Saturn's equator.
Voyager 2 view of Saturn casting a shadow across its rings. Four satellites, two of their shadows, and ring spokes are visible.
In September 2023, astronomers reported studies suggesting that the rings of Saturn may have resulted from the collision of two moons "a few hundred million years ago".[5][6]
Detail of Galileo's drawing of Saturn in a letter to Belisario Vinta (1610)
Galileo Galilei was the first to observe the rings of Saturn in 1610 using his telescope, but was unable to identify them as such. He wrote to the Duke of Tuscany that "The planet Saturn is not alone, but is composed of three, which almost touch one another and never move nor change with respect to one another. They are arranged in a line parallel to the zodiac, and the middle one (Saturn itself) is about three times the size of the lateral ones."[7] He also described the rings as Saturn's "ears". In 1612 the Earth passed through the plane of the rings and they became invisible. Mystified, Galileo remarked "I do not know what to say in a case so surprising, so unlooked for and so novel."[4] He mused, "Has Saturn swallowed his children?" — referring to the myth of the TitanSaturn devouring his offspring to forestall the prophecy of them overthrowing him.[7][8] He was further confused when the rings again became visible in 1613.[4]
Early astronomers used anagrams as a form of commitment scheme to lay claim to new discoveries before their results were ready for publication. Galileo used the anagram "smaismrmilmepoetaleumibunenugttauiras" for Altissimum planetam tergeminum observavi ("I have observed the most distant planet to have a triple form") for discovering the rings of Saturn.[9][10][11]
In 1657 Christopher Wren became Professor of Astronomy at Gresham College, London. He had been making observations of the planet Saturn from around 1652 with the aim of explaining its appearance. His hypothesis was written up in De corpore saturni, in which he came close to suggesting the planet had a ring. However, Wren was unsure whether the ring was independent of the planet, or physically attached to it. Before Wren's hypothesis was published Christiaan Huygens presented his hypothesis of the rings of Saturn. Immediately Wren recognised this as a better hypothesis than his own and De corpore saturni was never published. Robert Hooke was another early observer of the rings of Saturn, and noted the casting of shadows on the rings.[12]
Huygens' ring hypothesis and later developments[edit]
Huygens' ring hypothesis in Systema Saturnium (1659)
Huygens began grinding lenses with his father Constantijn in 1655 and was able to observe Saturn with greater detail using a 43× power refracting telescope that he designed himself. He was the first to suggest that Saturn was surrounded by a ring detached from the planet, and famously published the anagram: "aaaaaaacccccdeeeeeghiiiiiiillllmmnnnnnnnnnooooppqrrstttttuuuuu".[13] Three years later, he revealed it to mean Annulo cingitur, tenui, plano, nusquam coherente, ad eclipticam inclinato ("[Saturn] is surrounded by a thin, flat, ring, nowhere touching [the body of the planet], inclined to the ecliptic").[14][4][15] He published his ring hypothesis in Systema Saturnium (1659) which also included his discovery of Saturn's moon, Titan, as well as the first clear outline of the dimensions of the Solar System.[16]
In 1675, Giovanni Domenico Cassini determined that Saturn's ring was composed of multiple smaller rings with gaps between them;[17] the largest of these gaps was later named the Cassini Division. This division is a 4,800-kilometre-wide (3,000 mi) region between the A ring and B Ring.[18]
In 1787, Pierre-Simon Laplace proved that a uniform solid ring would be unstable and suggested that the rings were composed of a large number of solid ringlets.[19][4][20]
In 1859, James Clerk Maxwell demonstrated that a nonuniform solid ring, solid ringlets or a continuous fluid ring would also not be stable, indicating that the ring must be composed of numerous small particles, all independently orbiting Saturn.[21][20] Later, Sofia Kovalevskaya also found that Saturn's rings cannot be liquid ring-shaped bodies.[22][23] Spectroscopic studies of the rings which were carried out independently in 1895 by James Keeler of the Allegheny Observatory and by Aristarkh Belopolsky of the Pulkovo Observatory showed that Maxwell's analysis was correct.[24][25]
Four robotic spacecraft have observed Saturn's rings from the vicinity of the planet. Pioneer 11's closest approach to Saturn occurred in September 1979 at a distance of 20,900 km (13,000 mi).[26]Pioneer 11 was responsible for the discovery of the F ring.[26]Voyager 1's closest approach occurred in November 1980 at a distance of 64,200 km (39,900 mi).[27] A failed photopolarimeter prevented Voyager 1 from observing Saturn's rings at the planned resolution; nevertheless, images from the spacecraft provided unprecedented detail of the ring system and revealed the existence of the G ring.[28]Voyager 2's closest approach occurred in August 1981 at a distance of 41,000 km (25,000 mi).[27]Voyager 2's working photopolarimeter allowed it to observe the ring system at higher resolution than Voyager 1, and to thereby discover many previously unseen ringlets.[29]Cassini spacecraft entered into orbit around Saturn in July 2004.[30]Cassini's images of the rings are the most detailed to-date, and are responsible for the discovery of yet more ringlets.[31]
The rings are named alphabetically in the order they were discovered[32] (A and B in 1675 by Giovanni Domenico Cassini, C in 1850 by William Cranch Bond and his son George Phillips Bond, D in 1933 by Nikolai P. Barabachov and B. Semejkin, E in 1967 by Walter A. Feibelman, F in 1979 by Pioneer 11, and G in 1980 by Voyager 1). The main rings are, working outward from the planet, C, B and A, with the Cassini Division, the largest gap, separating Rings B and A. Several fainter rings were discovered more recently. The D Ring is exceedingly faint and closest to the planet. The narrow F Ring is just outside the A Ring. Beyond that are two far fainter rings named G and E. The rings show a tremendous amount of structure on all scales, some related to perturbations by Saturn's moons, but much unexplained.[32]
In September 2023, astronomers reported studies suggesting that the rings of Saturn may have resulted from the collision of two moons "a few hundred million years ago".[5][6]
Simulated appearance of Saturn as seen from Earth over the course of one Saturn year
Saturn's axial tilt is 26.7°, meaning that widely varying views of the rings, of which the visible ones occupy its equatorial plane, are obtained from Earth at different times.[33] Earth makes passes through the ring plane every 13 to 15 years, about every half Saturn year, and there are about equal chances of either a single or three crossings occurring in each such occasion. The most recent ring plane crossings were on 22 May 1995, 10 August 1995, 11 February 1996 and 4 September 2009; upcoming events will occur on 23 March 2025, 15 October 2038, 1 April 2039 and 9 July 2039. Favorable ring plane crossing viewing opportunities (with Saturn not close to the Sun) only come during triple crossings.[34][35][36]
Saturn's equinoxes, when the Sun passes through the ring plane, are not evenly spaced. The sun passes south to north through the ring plane when Saturn's heliocentric longitude is 173.6 degrees (e.g. 11 August 2009), about the time Saturn crosses from Leo to Virgo. 15.7 years later Saturn's longitude reaches 353.6 degrees and the sun passes to the south side of the ring plane. On each orbit the Sun is north of the ring plane for 15.7 Earth years, then south of the plane for 13.7 years.[a] Dates for north-to-south crossings include 19 November 1995 and 6 May 2025, with south-to-north crossings on 11 August 2009 and 23 January 2039.[38] During the period around an equinox the illumination of most of the rings is greatly reduced, making possible unique observations highlighting features that depart from the ring plane.[39]
Simulated image using color to present radio-occultation-derived particle size data. The attenuation of 0.94-, 3.6-, and 13-cm signals sent by Cassini through the rings to Earth shows abundance of particles of sizes similar to or larger than those wavelengths. Purple (B, inner A Ring) means few particles are < 5 cm (all signals similarly attenuated). Green and blue (C, outer A Ring) mean particles < 5 cm and < 1 cm, respectively, are common. White areas (B Ring) are too dense to transmit adequate signal. Other evidence shows rings A to C have a broad range of particle sizes, up to m across.The dark Cassini Division separates the wide inner B Ring and outer A ring in this image from the HST's ACS (March 22, 2004). The less prominent C Ring is just inside the B Ring.Cassini mosaic of Saturn's rings on August 12, 2009, a day after equinox. With the rings pointed at the Sun, illumination is by light reflected off Saturn, except on thicker or out-of-plane sections, like the F Ring.Cassini space probe view of the unilluminated side of Saturn's rings (May 9, 2007).
The dense main rings extend from 7,000 km (4,300 mi) to 80,000 km (50,000 mi) away from Saturn's equator, whose radius is 60,300 km (37,500 mi) (see Major subdivisions). With an estimated local thickness of as little as 10 metres (32' 10")[40] and as much as 1 km (1093 yards),[41] they are composed of 99.9% pure water ice with a smattering of impurities that may include tholins or silicates.[42] The main rings are primarily composed of particles smaller than 10 m.[43]
Cassini directly measured the mass of the ring system via their gravitational effect during its final set of orbits that passed between the rings and the cloud tops, yielding a value of 1.54 (± 0.49) × 1019 kg, or 0.41 ± 0.13 Mimas masses.[3] This is around two-thirds the mass of the Earth's entire Antarctic ice sheet, spread across a surface area 80 times larger than that of Earth.[44][45] The estimate is close to the value of 0.40 Mimas masses derived from Cassini observations of density waves in the A, B and C rings.[3] It is a small fraction of the total mass of Saturn (about 0.25 ppb). Earlier Voyager observations of density waves in the A and B rings and an optical depth profile had yielded a mass of about 0.75 Mimas masses,[46] with later observations and computer modeling suggesting that was an underestimate.[47]
Although the largest gaps in the rings, such as the Cassini Division and Encke Gap, can be seen from Earth, the Voyager spacecraft discovered that the rings have an intricate structure of thousands of thin gaps and ringlets. This structure is thought to arise, in several different ways, from the gravitational pull of Saturn's many moons. Some gaps are cleared out by the passage of tiny moonlets such as Pan,[48] many more of which may yet be discovered, and some ringlets seem to be maintained by the gravitational effects of small shepherd satellites (similar to Prometheus and Pandora's maintenance of the F ring). Other gaps arise from resonances between the orbital period of particles in the gap and that of a more massive moon further out; Mimas maintains the Cassini Division in this manner.[49] Still more structure in the rings consists of spiral waves raised by the inner moons' periodic gravitational perturbations at less disruptive resonances.[citation needed]
Data from the Cassini space probe indicate that the rings of Saturn possess their own atmosphere, independent of that of the planet itself. The atmosphere is composed of molecular oxygen gas (O2) produced when ultraviolet light from the Sun interacts with water ice in the rings. Chemical reactions between water molecule fragments and further ultraviolet stimulation create and eject, among other things, O2. According to models of this atmosphere, H2 is also present. The O2 and H2 atmospheres are so sparse that if the entire atmosphere were somehow condensed onto the rings, it would be about one atom thick.[50] The rings also have a similarly sparse OH (hydroxide) atmosphere. Like the O2, this atmosphere is produced by the disintegration of water molecules, though in this case the disintegration is done by energetic ions that bombard water molecules ejected by Saturn's moon Enceladus. This atmosphere, despite being extremely sparse, was detected from Earth by the Hubble Space Telescope.[51]
Saturn shows complex patterns in its brightness.[52] Most of the variability is due to the changing aspect of the rings,[53][54] and this goes through two cycles every orbit. However, superimposed on this is variability due to the eccentricity of the planet's orbit that causes the planet to display brighter oppositions in the northern hemisphere than it does in the southern.[55]
In 1980, Voyager 1 made a fly-by of Saturn that showed the F ring to be composed of three narrow rings that appeared to be braided in a complex structure; it is now known that the outer two rings consist of knobs, kinks and lumps that give the illusion of braiding, with the less bright third ring lying inside them.[citation needed]
New images of the rings taken around the 11 August 2009 equinox of Saturn by NASA's Cassini spacecraft have shown that the rings extend significantly out of the nominal ring plane in a few places. This displacement reaches as much as 4 km (2.5 mi) at the border of the Keeler Gap, due to the out-of-plane orbit of Daphnis, the moon that creates the gap.[56]
Estimates of the age of Saturn's rings vary widely, depending on the approach used. They have been considered to possibly be very old, dating to the formation of Saturn itself. However, data from Cassini suggest they are much younger, having most likely formed within the last 100 million years, and may thus be between 10 million and 100 million years old.[3][57] This recent origin scenario is based on a new, low mass estimate, modeling of the rings' dynamical evolution, and measurements of the flux of interplanetary dust, which feed into an estimate of the rate of ring darkening over time.[3] Since the rings are continually losing material, they would have been more massive in the past than at present.[3] The mass estimate alone is not very diagnostic, since high mass rings that formed early in the Solar System's history would have evolved by now to a mass close to that measured.[3] Based on current depletion rates, they may disappear in 300 million years.[58][59]
There are two main theories regarding the origin of Saturn's inner rings. A theory originally proposed by Édouard Roche in the 19th century, is that the rings were once a moon of Saturn (named Veritas, after a Roman goddess who hid in a well). According to the theory the moon's orbit decayed until it was close enough to be ripped apart by tidal forces (see Roche limit).[60] Numerical simulations carried out in 2022 support this theory; the authors of that study proposed the name "Chrysalis" for the destroyed moon.[61] A variation on this theory is that this moon disintegrated after being struck by a large comet or asteroid.[62] The second theory is that the rings were never part of a moon, but are instead left over from the original nebular material from which Saturn formed.[citation needed]
A 2007 artist impression of the aggregates of icy particles that form the 'solid' portions of Saturn's rings. These elongated clumps are continually forming and dispersing. The largest particles are a few meters across.
A more traditional version of the disrupted-moon theory is that the rings are composed of debris from a moon 400 to 600 km (200 to 400 miles) in diameter, slightly larger than Mimas. The last time there were collisions large enough to be likely to disrupt a moon that large was during the Late Heavy Bombardment some four billion years ago.[63]
A more recent variant of this type of theory by R. M. Canup is that the rings could represent part of the remains of the icy mantle of a much larger, Titan-sized, differentiated moon that was stripped of its outer layer as it spiraled into the planet during the formative period when Saturn was still surrounded by a gaseous nebula.[64][65] This would explain the scarcity of rocky material within the rings. The rings would initially have been much more massive (≈1,000 times) and broader than at present; material in the outer portions of the rings would have coalesced into the moons of Saturn out to Tethys, also explaining the lack of rocky material in the composition of most of these moons.[65] Subsequent collisional or cryovolcanic evolution of Enceladus might then have caused selective loss of ice from this moon, raising its density to its current value of 1.61 g/cm3, compared to values of 1.15 for Mimas and 0.97 for Tethys.[65]
The idea of massive early rings was subsequently extended to explain the formation of Saturn's moons out to Rhea.[66] If the initial massive rings contained chunks of rocky material (>100 km; 60 miles across) as well as ice, these silicate bodies would have accreted more ice and been expelled from the rings, due to gravitational interactions with the rings and tidal interaction with Saturn, into progressively wider orbits. Within the Roche limit, bodies of rocky material are dense enough to accrete additional material, whereas less-dense bodies of ice are not. Once outside the rings, the newly formed moons could have continued to evolve through random mergers. This process may explain the variation in silicate content of Saturn's moons out to Rhea, as well as the trend towards less silicate content closer to Saturn. Rhea would then be the oldest of the moons formed from the primordial rings, with moons closer to Saturn being progressively younger.[66]
The brightness and purity of the water ice in Saturn's rings have also been cited as evidence that the rings are much younger than Saturn,[57] as the infall of meteoric dust would have led to a darkening of the rings. However, new research indicates that the B Ring may be massive enough to have diluted infalling material and thus avoided substantial darkening over the age of the Solar System. Ring material may be recycled as clumps form within the rings and are then disrupted by impacts. This would explain the apparent youth of some of the material within the rings.[67] Evidence suggesting a recent origin of the C ring has been gathered by researchers analyzing data from the Cassini Titan Radar Mapper, which focused on analyzing the proportion of rocky silicates within this ring. If much of this material was contributed by a recently disrupted centaur or moon, the age of this ring could be on the order of 100 million years or less. On the other hand, if the material came primarily from micrometeoroid influx, the age would be closer to a billion years.[68]
The Cassini UVIS team, led by Larry Esposito, used stellar occultation to discover 13 objects, ranging from 27 metres (89') to 10 km (6 miles) across, within the F ring. They are translucent, suggesting they are temporary aggregates of ice boulders a few meters across. Esposito believes this to be the basic structure of the Saturnian rings, particles clumping together, then being blasted apart.[69]
Research based on rates of infall into Saturn favors a younger ring system age of hundreds of millions of years. Ring material is continually spiraling down into Saturn; the faster this infall, the shorter the lifetime of the ring system. One mechanism involves gravity pulling electrically charged water ice grains down from the rings along planetary magnetic field lines, a process termed 'ring rain'. This flow rate was inferred to be 432–2870 kg/s using ground-based Keck telescope observations; as a consequence of this process alone, the rings will be gone in ~292+818 −124 million years.[70] While traversing the gap between the rings and planet in September 2017, the Cassini spacecraft detected an equatorial flow of charge-neutral material from the rings to the planet of 4,800–44,000 kg/s.[71] Assuming this influx rate is stable, adding it to the continuous 'ring rain' process implies the rings may be gone in under 100 million years.[70][72]
Subdivisions and structures within the rings[edit]
The densest parts of the Saturnian ring system are the A and B Rings, which are separated by the Cassini Division (discovered in 1675 by Giovanni Domenico Cassini). Along with the C Ring, which was discovered in 1850 and is similar in character to the Cassini Division, these regions constitute the main rings. The main rings are denser and contain larger particles than the tenuous dusty rings. The latter include the D Ring, extending inward to Saturn's cloud tops, the G and E Rings and others beyond the main ring system. These diffuse rings are characterised as "dusty" because of the small size of their particles (often about a μm); their chemical composition is, like the main rings, almost entirely water ice. The narrow F Ring, just off the outer edge of the A Ring, is more difficult to categorize; parts of it are very dense, but it also contains a great deal of dust-size particles.
Natural-color mosaic of Cassini narrow-angle camera images of the unilluminated side of Saturn's D, C, B, A and F rings (left to right) taken on May 9, 2007 (distances are to the planet's center).
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
This program unpacks Playstation 3 Theme files (.p3t) so that you can touch-up an existing theme to your likings or use a certain wallpaper from it (as many themes have multiple). But remember, if you use content from another theme and release it, be sure to give credit!
Download p3textractor.zip from above. Extract the files to a folder with a program such as WinZip or WinRAR. Now there are multiple ways to extract the theme.
The first way is to simply open the p3t file with p3textractor.exe. If you don’t know how to do this, right click the p3t file and select Open With. Alternatively, open the p3t file and it will ask you to select a program to open with. Click Browse and find p3textractor.exe from where you previously extracted it to. It will open CMD and extract the theme to extracted.[filename]. After that, all you need to do for any future p3t files is open them and it will extract.
The second way is very simple. Just drag the p3t file to p3textractor.exe. It will open CMD and extract the theme to extracted.[filename].
For the third way, first put the p3t file you want to extract into the same folder as p3textractor.exe. Open CMD and browse to the folder with p3extractor.exe. Enter the following: p3textractor filename.p3t [destination path]Replace filename with the name of the p3t file, and replace [destination path] with the name of the folder you want the files to be extracted to. A destination path is not required. By default it will extract to extracted.filename.
Memphis State University (1957–1994) Memphis State College (1941–1957) West Tennessee State Teachers College (1925–1941) West Tennessee State Normal School (1912–1925)
The university maintains the Herff College of Engineering, the Center for Earthquake Research and Information (CERI), the Cecil C. Humphreys School of Law, the School of Communication Sciences and Disorders, the former Lambuth University campus in Jackson, Tennessee (now a branch campus of the University of Memphis), the Loewenberg College of Nursing, the School of Public Health, the College of Communication and Fine Arts, the FedEx Institute of Technology, the Advanced Distributed Learning Workforce Co-Lab, and the Institute of Egyptian Art and Archaeology. The University of Memphis is classified among "R1: Doctoral Universities – Very High research activity".[6]
Mynders Hall (left) and the Admin Building (right) at the West Tennessee Normal School in 1911
In 1909, the Tennessee Legislature enacted the General Education Bill. This bill stated that three colleges be established, one within each grand division of the state and one additional school for African-American students. After much bidding and campaigning, the state had to choose between two sites to build the new college for West Tennessee: Jackson and Memphis. Memphis was chosen, one of the main reasons being the proximity of the rail line to the site proposed to build the new college for West Tennessee. This would allow professors and students to go home and visit their relatives. The other three schools established through the General Education Act evolved into East Tennessee State University (ETSU), Middle Tennessee State University (MTSU), and Tennessee State University (TSU).
Prior to the establishment of the West Tennessee Normal School[clarification needed] pursuant to the General Education Bill, a number of higher education departments existed in Memphis under the banner of the University of Memphis. This earlier University of Memphis was formed in 1909 by adding to an already existing medical school's departments of pharmacy, dentistry, and law.[7]
On September 10, 1912, West Tennessee Normal School opened in Memphis; its first president was Seymour A. Mynders. By 1913 all departments of the earlier University of Memphis, except the law school, had been taken over by West Tennessee Normal School.[7][8] After Mynders' death in 1913, John Willard Brister was chosen to take his place. After Brister's resignation in 1918, Andrew A. Kincannon became president. In 1924, Brister returned to his post as president of the school.
The name changed in 1925 to West Tennessee State Teachers College. In 1931, the campus' first newspaper, The Tiger Rag, was established. In 1939, Richard C. Jones became president of WTSTC. In 1941, the name was changed to Memphis State College, when the college expanded its liberal arts curriculum. In 1943, Dr. Jennings B. Sanders succeeded Jones as president. Three years later, the first alumnus to become president, J. Millard (Jack) Smith, was appointed. In 1951 MSC awarded its first B.A. degree. In 1957 the school received full University status and changed its name accordingly to Memphis State University.
Historical marker on campus honoring the Memphis State Eight
In 1959, five years after Brown v. Board of Education was decided by the Supreme Court of the United States, holding that racial segregation in public education was unconstitutional, the university admitted its first black students. Racial segregation was the norm throughout the South at the time. The Memphis State Eight, as they were known, were admitted to Memphis State University. Their presence on campus was the focus not only of intense media scrutiny but severe criticism from much of the local public. Ostensibly for the black students' safety and to maintain an air of calm on the campus, university administrators placed certain stringent restrictions on where and when the black students could be on campus. They were to go only to their classes, not to any of the public places on campus, such as the cafeteria; and they were to leave the campus immediately after they had finished their last class. These limitations were lifted after the novelty of their presence on campus had subsided and the public's focus on their presence there had lessened, and as more and more black students were admitted to the university, all such social restrictions were dropped. Today, black students make up more than one-third of the campus student body and participate in all campus activities.
Cecil C. Humphreys became president of MSU, succeeding Smith, in 1960. In 1966, the school began awarding doctoral degrees. Humphreys resigned as MSU president to become the first chancellor of the newly formed State University and Community College System, later renamed the Tennessee Board of Regents. John Richardson was appointed interim president.
In 1973, Dr. Billy Mac Jones became president. Also that year, the Memphis State Tigers men's basketball team reached the finals of the NCAA tournament, only to fall at the hands of a UCLA team led by future NBA superstar and Basketball Hall of FamerBill Walton in the NCAA Basketball Championship Game in St. Louis, Missouri. In 1980, Thomas Carpenter became president of MSU; he was succeeded by V. Lane Rawlins in 1991. On July 1, 1994, Memphis State University changed its name again, to the current University of Memphis.
V. Lane Rawlins served from 1991 to 2000; Dr. Ralph Faudree filled in as interim president for one year after V. Lane Rawlins' departure. In 2001, The U of M installed its first female president, Shirley Raines, who retired in the summer of 2013. During her tenure (in 2008), the Tigers men's basketball team again reached the NCAA Finals, only to later have the appearance vacated after an NCAA investigation. After a yearlong search, Dr. M. David Rudd was confirmed as the 12th president on May 1, 2014.[9]
In the spring semester of 2020, the university joined thousands of other institutions and made a mid-semester shift to online classes as a result of the COVID-19 pandemic, and also introduced a credit/no credit grade option in lieu of the traditional grading scale for that semester.[10]
This section's factual accuracy may be compromised due to out-of-date information. Please help update this article to reflect recent events or newly available information.(February 2024)
The University of Memphis campus is located approximately 5 miles (8.0 km) east of downtown in the University District neighborhood of east Memphis. It has an area of 1,160 acres (4.7 km2), although this figure does not include the law school in the former United States federal customshouse in downtown Memphis, which opened in January 2010. The historic core of campus encompasses approximately 30 acres (120,000 m2).
Wilder Tower; the tallest building of the university's main campus
Campus planners have significantly increased the amount of green space and the number of walkways over the past several years while maintaining the original historic architecture of the campus.
Surrounding the university's main campus are several historic neighborhoods to the north and east, as well as the University District neighborhood and the commercial Highland Strip to the west. Many University of Memphis college students also reside in housing south of the main campus.
The University of Memphis campus is set out in a rectilinear format, planned as a geometric design similar to the Jeffersonian style of the University of Virginia.
Despite the gradual expansion of the campus to the West and South, the campus is fairly compact and retains a park-like, tree-lined setting. The farthest distance on campus takes about twenty-five minutes to walk. According to the most recent master plan, the University of Memphis is projected to expand and redevelop additional areas one block west of the main campus' current western boundary of Patterson St., making Highland Avenue the "de facto" entrance to the university.[11]
Students walking in front of Manning HallThe FedEx Institute of Technology is a major research contributor in the areas of Supply Chain Management, robotics, and intelligent systems.
The center of the main campus comprises buildings that made up the original campus. The first college buildings, including Scates Hall, Manning Hall, Mynders Hall, and Administration Building, were erected in the early 20th century. This section stretches from Patterson St. south to the end of the main campus at Walker Ave., with most buildings surrounding Alumni Mall and Student Plaza. The majority of the buildings of the arts and humanities departments, as well as those of the Physics and Astronomy departments of the College of Arts and Sciences, are located in the original areas of campus.
The Administration Building at the University of MemphisScates Hall, the 3rd oldest building on campus
Flanking the original area of campus to the east are the areas of major research for The Life Sciences and Engineering departments, including J.M. Smith Hall, Life Sciences Building and Herff College of Engineering Complex, as well as the College of Education, residing in E.C. Ball Hall, and the Art Museum of the University of Memphis, located in the Communication and Fine Arts Building. The Ned R. McWherter Library, a state-of-the-art library facility and one of the premier research libraries of the Mid-South United States, takes up the eastern part of the campus adjacent to Dunavant Plaza and Emeriti Grove.
UofM "Columns" Plaque
The northwestern area of the main campus includes The Fogelman College of Business and Economics, The Fogelman Executive Center (a major conference center for regional executives visiting The University of Memphis that is now mainly occupied by the University Middle School, with plans to incorporate a predecessor to a High School education completing the long dreamt of k-college experience), and The FedEx Institute of Technology, a major research contributor in the areas of Supply Chain Management, Nanotechnology, Robotics and Intelligent Systems. Originally, at the north end of the campus, Norriswood Ave. was the northern boundary and was an actual street that ran through the campus. The campus expanded into this area in the late 1960s & early 1970s.
University Center at the University of Memphis
The western edge and southwest corner include Johnson Hall (comprising the Geography and Geology Departments), Patterson Hall (housing the English department), John S. Wilder Tower (formerly Brister Tower), Greek Row, and the bulk of The University of Memphis residence halls. As The University of Memphis presses ahead with its planned expansion, many more facilities, pedestrian access, and green space will also be created with the renovation and development of the current residential block west of Patterson St. in the University District neighborhood.
On January 29, 2013, Governor Bill Haslam announced a $44.6 million state budget pledge for the Community Health Building, which is the new home of The Loewenberg College of Nursing and The School of Communication Sciences and Disorders. The University of Memphis was required to raise $15 million from private funds to match the state funds.
In 2017, the university announced plans for a new Veterans Care Center on campus. Located in the Psychological Services Center on campus, the Veterans Care Center "will address the mental health needs of veterans, regardless of era, gender, discharge status or service connection."[12]
In 2019, the university opened the Hunter Harrison Memorial Bridge, providing for the first time in school history a pedestrian crossing that connects the main campus and the campus areas south of the Norfolk-Southern railroad with uninterrupted access. This bridge connects to the new Southern Parking Garage, as well as the new $30 million Student Recreation & Fitness Center completed in 2021, expanding the area of the campus south of the railroad tracks. The university completed construction in November 2022 of the new $44 million Rudi E. Scheidt School of Music building on Central Ave., beginning a major northward expansion of campus across Central Ave.
Directly south of the main campus along the corner of Park Avenue and Getwell Road sits the Park Avenue Campus, formerly known as South Campus. The Park Avenue Campus was formerly the site of Kennedy Veterans Hospital from 1942 until 1967 when the U.S. Government donated the land and buildings to the university. Very few buildings from the Kennedy Hospital days remain on campus. The Park Avenue Campus is home not only to various intramural athletics programs and facilities, but also to various research facilities, classrooms and the Community Health Building, which houses the School of Communication Sciences and Disorders, the Memphis Speech and Hearing Center, and the Loewenberg College of Nursing. The Defense Contract Audit Agency formerly operated its main training facility on the Park Avenue Campus from 1982 to the early 2010s. WKNO formerly operated its FM and television stations on the Park Avenue Campus as well.
Future plans include a regulation indoor soccer stadium and track facility, capable of hosting large-scale NCAA Division I track-and-field meets.[13]
The graduate and family housing units are located at Park Avenue, 1 mile (1.6 km) from the main university campus. The complex has 150 housing units.[14] Residents are zoned to Memphis City Schools.[15] The zoned schools are Sherwood Elementary School,[16] Colonial Middle School,[17] and White Station High School.[18]
In 2006, plans were announced that the University of Memphis, School of Law would relocate to the former U.S. Post Office & Customs House in downtown Memphis. This facility pre-dates the existence of the university itself, having been constructed in multiple sections between 1885 and the early 1920s. In 2010, the law school was moved permanently from the main campus to the newly renovated downtown campus. The new University of Memphis, School of Law campus sits adjacent to downtown courts and the financial and administrative center of the city. It has been ranked multiple times among the top law school facilities in the U.S.
In 2011, the University of Memphis began offering undergraduate and graduate programs on the former Lambuth University campus in Jackson, Tennessee, located approximately 80 miles (130 km) east of Memphis. Now known as the University of Memphis Lambuth Campus, the historic campus includes classroom buildings, dormitories, a library, a planetarium, and athletic facilities. Enrollment in the fall of 2011 stood at 246 students. Enrollment in the spring of 2018 was the first time enrollment surpassed 1,000 students, with a total of 1,038 students. The 2019–2020 term was the first term, to begin with an enrollment of over 1,000 students for the campus, with an official enrollment of 1,070 students. In the fall of 2020, enrollment had risen to 1,285 students.[19]
The Edward J. Meeman Biological Station of the University of Memphis conducts research in ecology, environmental biology, and natural history. It is named for Edward J. Meeman, an editor of the former Memphis Press-Scimitarnewspaper who later established a foundation to fund environmental studies.[20]
In 2007, President Shirley Raines signed the American College and University President's Climate Commitment (ACUPCC), which requires that the university become carbon neutral.[21]
The Green Campus Initiative works to develop and implement a strategic plan to achieve the goals of the APUPCC. Successful events and projects include the May 2009 2nd Annual E-Recycling Day, resulting in 155 tons of electronic items collected, and the Tiger Initiative for Gardening in Urban Settings (TIGUrS), a fruit and vegetable gardening initiative across campus.[22]
In April 2008, the student-run Environmental Action Club ran a Green Power Campaign to promote a student referendum to add a "Green Fee" to tuition payments to fund clean, renewable energy and other campus sustainability projects. The referendum passed with a 69% student approval rate. The university is now purchasing renewable energy through the TVA's Green Power Switch program and offsetting 10% of current energy use. It is now the 2nd largest green power purchaser in the entire TVA distribution region.[23]
In February 2009, the TERRA (Technologically and Environmentally Responsive Residential Architecture) sustainable design demonstration house was completed. Designed by the Department of Architecture, the LEED Platinum TERRA house serves as a studio for which architecture and design students to design "green" housing within urban areas, as well as serve as a demonstration house open for tours and serving as an educational tool for the community.[24]
Memphis received a grade of "C" on the 2009 Campus Sustainability Report Card published by the Sustainable Endowments Institute.[25] Only 34 schools earned a higher grade.[26]
