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Eclipse
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For other uses, see Eclipse (disambiguation) and Total Eclipse (disambiguation).
Totality during the 1999 solar eclipse. Solar prominences can be seen along the limb (in red) as well as extensive coronal filaments.
An eclipse is an astronomical event that occurs when an astronomical object is temporarily obscured, either by passing into the shadow of another body or by having another body pass between it and the viewer. This alignment of three celestial objects is known as a syzygy.[1] Apart from syzygy, the term eclipse is also used when a spacecraft reaches a position where it can observe two celestial bodies so aligned. An eclipse is the result of either an occultation (completely hidden) or a transit (partially hidden).
The term eclipse is most often used to describe either a solar eclipse, when the Moon's shadow crosses the Earth's surface, or a lunar eclipse, when the Moon moves into the Earth's shadow. However, it can also refer to such events beyond the Earth–Moon system: for example, a planet moving into the shadow cast by one of its moons, a moon passing into the shadow cast by its host planet, or a moon passing into the shadow of another moon. A binary star system can also produce eclipses if the plane of the orbit of its constituent stars intersects the observer's position.
For the special cases of solar and lunar eclipses, these only happen during an "eclipse season", the two times of each year when the plane of the Earth's orbit around the Sun crosses with the plane of the Moon's orbit around the Earth. The type of solar eclipse that happens during each season (whether total, annular, hybrid, or partial) depends on apparent sizes of the Sun and Moon. If the orbit of the Earth around the Sun, and the Moon's orbit around the Earth were both in the same plane with each other, then eclipses would happen each and every month. There would be a lunar eclipse at every full moon, and a solar eclipse at every new moon. And if both orbits were perfectly circular, then each solar eclipse would be the same type every month. It is because of the non-planar and non-circular differences that eclipses are not a common event. Lunar eclipses can be viewed from the entire nightside half of the Earth. But solar eclipses, particularly a total eclipse, as occurring at any one particular point on the Earth's surface, is a rare event that can span many decades from one to the next.
Contents
[hide]
1 Etymology
2 Umbra, penumbra and antumbra
3 Eclipse cycles
4 Earth–Moon system
4.1 Solar eclipse
4.2 Lunar eclipse
4.3 Historical record
5 Other planets and dwarf planets
5.1 Gas giants
5.2 Mars
5.3 Pluto
5.4 Mercury and Venus
6 Eclipsing binaries
7 See also
8 Eclipse Types Index
9 References
10 External links
Etymology[edit]
The term is derived from the ancient Greek noun ἔκλειψις (ékleipsis), which means "the abandonment", "the downfall", or "the darkening of a heavenly body", which is derived from the verb ἐκλείπω (ekleípō) which means "to abandon", "to darken", or "to cease to exist,"[2] a combination of prefix ἐκ- (ek-), from preposition ἐκ (ek), "out," and of verb λείπω (leípō), "to be absent".[3][4]
Umbra, penumbra and antumbra[edit]
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Main article: Umbra, penumbra and antumbra
Umbra, penumbra and antumbra cast by an opaque object occulting a larger light source
For any two objects in space, a line can be extended from the first through the second. The latter object will block some amount of light being emitted by the former, creating a region of shadow around the axis of the line. Typically these objects are moving with respect to each other and their surroundings, so the resulting shadow will sweep through a region of space, only passing through any particular location in the region for a fixed interval of time. As viewed from such a location, this shadowing event is known as an eclipse.[5]
Typically the cross-section of the objects involved in an astronomical eclipse are roughly disk shaped.[5] The region of an object's shadow during an eclipse is divided into three parts:[6]
The umbra, within which the object completely covers the light source. For the Sun, this light source is the photosphere.
The antumbra, extending beyond the tip of the umbra, within which the object is completely in front of the light source but too small to completely cover it.
The penumbra, within which the object is only partially in front of the light source.
Sun-moon configurations that produce a total (A), annular (B), and partial (C) solar eclipse
A total eclipse occurs when the observer is within the umbra, an annular eclipse when the observer is within the antumbra, and a partial eclipse when the observer is within the penumbra. During a lunar eclipse only the umbra and penumbra are applicable. This is because Earth's apparent diameter from the viewpoint of the Moon is nearly four times that of the Sun. The same terms may be used analogously in describing other eclipses, e.g., the antumbra of Deimos crossing Mars, or Phobos entering Mars's penumbra.
The first contact occurs when the eclipsing object's disc first starts to impinge on the light source; second contact is when the disc moves completely within the light source; third contact when it starts to move out of the light; and fourth or last contact when it finally leaves the light source's disc entirely.
For spherical bodies, when the occulting object is smaller than the star, the length (L) of the umbra's cone-shaped shadow is given by:
L = r ⋅ R o R s − R o {\displaystyle L\ =\ {\frac {r\cdot R_{o}}{R_{s}-R_{o}}}}
where Rs is the radius of the star, Ro is the occulting object's radius, and r is the distance from the star to the occulting object. For Earth, on average L is equal to 1.384×106 km, which is much larger than the Moon's semimajor axis of 3.844×105 km. Hence the umbral cone of the Earth can completely envelop the Moon during a lunar eclipse.[7] If the occulting object has an atmosphere, however, some of the luminosity of the star can be refracted into the volume of the umbra. This occurs, for example, during an eclipse of the Moon by the Earth—producing a faint, ruddy illumination of the Moon even at totality.
On Earth, the shadow cast during an eclipse moves very approximately at 1 km per sec. This depends on the location of the shadow on the Earth and the angle in which it is moving.[8]
Eclipse cycles[edit]
Main article: Eclipse cycle
An eclipse cycle takes place when eclipses in a series are separated by a certain interval of time. This happens when the orbital motions of the bodies form repeating harmonic patterns. A particular instance is the saros, which results in a repetition of a solar or lunar eclipse every 6,585.3 days, or a little over 18 years. Because this is not a whole number of days, successive eclipses will be visible from different parts of the world.[9]
Earth–Moon system[edit]
A symbolic orbital diagram from the view of the Earth at the center, with the sun and moon projected upon the celestial sphere, showing the Moon's two nodes where eclipses can occur.
An eclipse involving the Sun, Earth, and Moon can occur only when they are nearly in a straight line, allowing one to be hidden behind another, viewed from the third. Because the orbital plane of the Moon is tilted with respect to the orbital plane of the Earth (the ecliptic), eclipses can occur only when the Moon is close to the intersection of these two planes (the nodes). The Sun, Earth and nodes are aligned twice a year (during an eclipse season), and eclipses can occur during a period of about two months around these times. There can be from four to seven eclipses in a calendar year, which repeat according to various eclipse cycles, such as a saros.
Between 1901 and 2100 there are the maximum of seven eclipses in:[10]
four (penumbral) lunar and three solar eclipses: 1908, 2038.
four solar and three lunar eclipses: 1918, 1973, 2094.
five solar and two lunar eclipses: 1934.
Excluding penumbral lunar eclipses, there are a maximum of seven eclipses in:[11]
1591, 1656, 1787, 1805, 1918, 1935, 1982, and 2094.
Solar eclipse[edit]
Main article: Solar eclipse
The progression of a solar eclipse on August 1, 2008, viewed from Novosibirsk, Russia. The time between shots is three minutes.
As observed from the Earth, a solar eclipse occurs when the Moon passes in front of the Sun. The type of solar eclipse event depends on the distance of the Moon from the Earth during the event. A total solar eclipse occurs when the Earth intersects the umbra portion of the Moon's shadow. When the umbra does not reach the surface of the Earth, the Sun is only partially occulted, resulting in an annular eclipse. Partial solar eclipses occur when the viewer is inside the penumbra.[12]
Each icon shows the view from the centre of its black spot, representing the moon (not to scale)
The eclipse magnitude is the fraction of the Sun's diameter that is covered by the Moon. For a total eclipse, this value is always greater than or equal to one. In both annular and total eclipses, the eclipse magnitude is the ratio of the angular sizes of the Moon to the Sun.[13]
Solar eclipses are relatively brief events that can only be viewed in totality along a relatively narrow track. Under the most favorable circumstances, a total solar eclipse can last for 7 minutes, 31 seconds, and can be viewed along a track that is up to 250 km wide. However, the region where a partial eclipse can be observed is much larger. The Moon's umbra will advance eastward at a rate of 1,700 km/h, until it no longer intersects the Earth's surface.
Geometry of a total solar eclipse (not to scale)
During a solar eclipse, the Moon can sometimes perfectly cover the Sun because its apparent size is nearly the same as the Sun's when viewed from the Earth. A total solar eclipse is in fact an occultation while an annular solar eclipse is a transit.
When observed at points in space other than from the Earth's surface, the Sun can be eclipsed by bodies other than the Moon. Two examples include when the crew of Apollo 12 observed the Earth to eclipse the Sun in 1969 and when the Cassini probe observed Saturn to eclipse the Sun in 2006.
Lunar eclipse[edit]
Main article: Lunar eclipse
The progression of a lunar eclipse from right to left. Totality is shown with the first two images. These required a longer exposure time to make the details visible.
Lunar eclipses occur when the Moon passes through the Earth's shadow. This happens only during a full moon, when the Moon is on the far side of the Earth from the Sun. Unlike a solar eclipse, an eclipse of the Moon can be observed from nearly an entire hemisphere. For this reason it is much more common to observe a lunar eclipse from a given location. A lunar eclipse lasts longer, taking several hours to complete, with totality itself usually averaging anywhere from about 30 minutes to over an hour.[14]
There are three types of lunar eclipses: penumbral, when the Moon crosses only the Earth's penumbra; partial, when the Moon crosses partially into the Earth's umbra; and total, when the Moon crosses entirely into the Earth's umbra. Total lunar eclipses pass through all three phases. Even during a total lunar eclipse, however, the Moon is not completely dark. Sunlight refracted through the Earth's atmosphere enters the umbra and provides a faint illumination. Much as in a sunset, the atmosphere tends to more strongly scatter light with shorter wavelengths, so the illumination of the Moon by refracted light has a red hue,[15] thus the phrase 'Blood Moon' is often found in descriptions of such lunar events as far back as eclipses are recorded.[16]
Historical record[edit]
Records of solar eclipses have been kept since ancient times. Eclipse dates can be used for chronological dating of historical records. A Syrian clay tablet, in the Ugaritic language, records a solar eclipse which occurred on March 5, 1223 B.C.,[17] while Paul Griffin argues that a stone in Ireland records an eclipse on November 30, 3340 B.C.[18] Positing classical-era astronomers' use of Babylonian eclipse records mostly from the 13th century BC provides a feasible and mathematically consistent[19] explanation for the Greek finding all three lunar mean motions (synodic, anomalistic, draconitic) to a precision of about one part in a million or better. Chinese historical records of solar eclipses date back over 4,000 years and have been used to measure changes in the Earth's rate of spin.[20]
By the 1600s, European astronomers were publishing books with diagrams explaining how lunar and solar eclipses occurred.[21][22] In order to disseminate this information to a broader audience and decrease fear of the consequences of eclipses, booksellers printed broadsides explaining the event either using the science or via astrology.[23]
Other planets and dwarf planets[edit]
Gas giants[edit]
See also: Solar eclipses on Jupiter, Solar eclipses on Saturn, Solar eclipses on Uranus, and Solar eclipses on Neptune
A picture of Jupiter and its moon Io taken by Hubble. The black spot is Io's shadow.
Saturn occults the Sun as seen from the Cassini–Huygens space probe
The gas giant planets (Jupiter,[24] Saturn,[25] Uranus,[26] and Neptune)[27] have many moons and thus frequently display eclipses. The most striking involve Jupiter, which has four large moons and a low axial tilt, making eclipses more frequent as these bodies pass through the shadow of the larger planet. Transits occur with equal frequency. It is common to see the larger moons casting circular shadows upon Jupiter's cloudtops.
The eclipses of the Galilean moons by Jupiter became accurately predictable once their orbital elements were known. During the 1670s, it was discovered that these events were occurring about 17 minutes later than expected when Jupiter was on the far side of the Sun. Ole Rømer deduced that the delay was caused by the time needed for light to travel from Jupiter to the Earth. This was used to produce the first estimate of the speed of light.[28]
On the other three gas giants, eclipses only occur at certain periods during the planet's orbit, due to their higher inclination between the orbits of the moon and the orbital plane of the planet. The moon Titan, for example, has an orbital plane tilted about 1.6° to Saturn's equatorial plane. But Saturn has an axial tilt of nearly 27°. The orbital plane of Titan only crosses the line of sight to the Sun at two points along Saturn's orbit. As the orbital period of Saturn is 29.7 years, an eclipse is only possible about every 15 years.
The timing of the Jovian satellite eclipses was also used to calculate an observer's longitude upon the Earth. By knowing the expected time when an eclipse would be observed at a standard longitude (such as Greenwich), the time difference could be computed by accurately observing the local time of the eclipse. The time difference gives the longitude of the observer because every hour of difference corresponded to 15° around the Earth's equator. This technique was used, for example, by Giovanni D. Cassini in 1679 to re-map France.[29]
Mars[edit]
Main article: Transit of Phobos from Mars
Transit of Phobos from Mars, as seen by the Mars Opportunity rover (10 March 2004).
On Mars, only partial solar eclipses (transits) are possible, because neither of its moons is large enough, at their respective orbital radii, to cover the Sun's disc as seen from the surface of the planet. Eclipses of the moons by Mars are not only possible, but commonplace, with hundreds occurring each Earth year. There are also rare occasions when Deimos is eclipsed by Phobos.[30] Martian eclipses have been photographed from both the surface of Mars and from orbit.
Pluto[edit]
Main article: Solar eclipses on Pluto
Pluto, with its proportionately largest moon Charon, is also the site of many eclipses. A series of such mutual eclipses occurred between 1985 and 1990.[31] These daily events led to the first accurate measurements of the physical parameters of both objects.[32]
Mercury and Venus[edit]
Eclipses are impossible on Mercury and Venus, which have no moons. However, both have been observed to transit across the face of the Sun. There are on average 13 transits of Mercury each century. Transits of Venus occur in pairs separated by an interval of eight years, but each pair of events happen less than once a century.[33] According to NASA, the next pair of transits will occur on December 10, 2117 and December 8, 2125. Transits on Mercury are much more common.[34]
Eclipsing binaries[edit]
A binary star system consists of two stars that orbit around their common centre of mass. The movements of both stars lie on a common orbital plane in space. When this plane is very closely aligned with the location of an observer, the stars can be seen to pass in front of each other. The result is a type of extrinsic variable star system called an eclipsing binary.
The maximum luminosity of an eclipsing binary system is equal to the sum of the luminosity contributions from the individual stars. When one star passes in front of the other, the luminosity of the system is seen to decrease. The luminosity returns to normal once the two stars are no longer in alignment.[35]
The first eclipsing binary star system to be discovered was Algol, a star system in the constellation Perseus. Normally this star system has a visual magnitude of 2.1. However, every 2.867 days the magnitude decreases to 3.4 for more than nine hours. This is caused by the passage of the dimmer member of the pair in front of the brighter star.[36] The concept that an eclipsing body caused these luminosity variations was introduced by John Goodricke in 1783.[37]
See also[edit]
List of solar eclipses in the 21st century
Mursili's eclipse
Transit of Venus
Eclipse Types Index[edit]
Sun - Moon - Earth: Solar eclipse | annular eclipse | hybrid eclipse | partial eclipse
Sun - Earth - Moon: Lunar eclipse | penumbral eclipse | partial lunar eclipse | central lunar eclipse
Sun - Phobos - Mars: Transit of Phobos from Mars | Solar eclipses on Mars
Sun - Deimos - Mars: Transit of Deimos from Mars | Solar eclipses on Mars
Other Eclipse Types list: Solar eclipses on Jupiter | Solar eclipses on Saturn | Solar eclipses on Uranus | Solar eclipses on Neptune | Solar eclipses on Pluto
References[edit]
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Jump up ^ See DIO 16 p.2 (2009). Though those Greek and perhaps Babylonian astronomers who determined the three previously unsolved lunar motions were spread over more than four centuries (263 BC to 160 AD), the math-indicated early eclipse records are all from a much smaller span: the 13th century BC. The anciently attested Greek technique: use of eclipse cycles, automatically providing integral ratios, which is how all ancient astronomers' lunar motions were expressed. Long-eclipse-cycle-based reconstructions precisely produce all of the 24 digits appearing in the three attested ancient motions just cited: 6247 synod = 6695 anom (System A), 5458 synod = 5923 drac (Hipparchos), 3277 synod = 3512 anom (Planetary Hypotheses). By contrast, the System B motion, 251 synod = 269 anom (Aristarchos?), could have been determined without recourse to remote eclipse data, simply by using a few eclipse-pairs 4267 months apart.
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Jump up ^ "When will the next transits of Mercury and Venus occur during a total solar eclipse? | Total Solar Eclipse 2017". eclipse2017.nasa.gov. Retrieved 2017-09-25.
Jump up ^ Bruton, Dan. "Eclipsing binary stars". Midnightkite Solutions. Archived from the original on 2007-04-14. Retrieved 2007-05-01.
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Jump up ^ Goodricke, John; Englefield, H. C. (1785). "Observations of a New Variable Star". Philosophical Transactions of the Royal Society of London. 75: 153–164. Bibcode:1785RSPT...75..153G. doi:10.1098/rstl.1785.0009.
External links[edit]
Wikimedia Commons has media related to Eclipse.
Wikiquote has quotations related to: Eclipse
Look up eclipse in Wiktionary, the free dictionary.
Phobos Eclipsing Mars Observed by Curiosity Rover on YouTube
A Catalogue of Eclipse Cycles
Search 5,000 years of eclipses
NASA eclipse home page
International Astronomical Union's Working Group on Solar Eclipses
Mark's eclipse chasing website
Interactive eclipse maps site
Image galleries
The World at Night Eclipse Gallery
Solar and Lunar Eclipse Image Gallery
Williams College eclipse collection of images
Prof. Druckmüller's eclipse photography site
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text:
Pentium III
From Wikipedia, the free encyclopedia
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Pentium III
Produced
From early 1999 to 2003
Common manufacturer(s)
Intel
Max. CPU clock rate
450 MHz to 1.4 GHz
FSB speeds
100 MHz to 133 MHz
Min. feature size
0.25 µm to 0.13 µm
Instruction set
IA-32, MMX, SSE
Microarchitecture
P6
Cores
1
Core name(s)
Katmai
Coppermine
Coppermine T
Tualatin
Socket(s)
Slot 1
Socket 370
Socket 479 (mobile)
Predecessor
Pentium II
Successor
Pentium 4, Xeon, Celeron, Pentium M
The Pentium III[1] (marketed as Intel Pentium III Processor, informally PIII) brand refers to Intel's 32-bit x86 desktop and mobile microprocessors based on the sixth-generation P6 microarchitecture introduced on February 26, 1999. The brand's initial processors were very similar to the earlier Pentium II-branded microprocessors. The most notable differences were the addition of the SSE instruction set (to accelerate floating point and parallel calculations), and the introduction of a controversial serial number embedded in the chip during the manufacturing process.
Contents
1 Processor cores
1.1 Katmai
1.2 Coppermine
1.3 Coppermine T
1.4 Tualatin
2 Pentium III's SSE implementation
3 Core specifications
3.1 Katmai (0.25 µm)
3.2 Coppermine (0.18 µm)
3.3 Coppermine T (0.18 µm)
3.4 Tualatin (0.13 µm)
4 Controversy about privacy issues
5 See also
6 References
7 External links
Processor cores[edit]
Similarly to the Pentium II it superseded, the Pentium III was also accompanied by the Celeron brand for lower-end versions, and the Xeon for high-end (server and workstation) derivatives. The Pentium III was eventually superseded by the Pentium 4, but its Tualatin core also served as the basis for the Pentium M CPUs, which used many ideas from the P6 microarchitecture. Subsequently, it was the Pentium M microarchitecture of Pentium M branded CPUs, and not the NetBurst found in Pentium 4 processors, that formed the basis for Intel's energy-efficient Core microarchitecture of CPUs branded Core 2, Pentium Dual-Core, Celeron (Core), and Xeon.
Intel Pentium III processor family
Standard Logo (1999-2002)
Mobile Logo (1999-2003)
Desktop
Code-named
Core
Date released
Katmai
Coppermine
Coppermine T
Tualatin (250 nm)
(180 nm)
(180 nm)
(130 nm) Feb 1999
Oct 1999
June 2001
June 2001
List of Intel Pentium III microprocessors
Katmai[edit]
A Pentium III Katmai SECC2 cartridge with heatsink removed.
The first Pentium III variant was the Katmai (Intel product code 80525). It was a further development of the Deschutes Pentium II. The Pentium III saw an increase of 2 million transistors over the Pentium II. The differences were the addition of execution units and SSE instruction support, and an improved L1 cache controller[citation needed] (the L2 cache controller was left unchanged, as it would be completely redesigned for Coppermine anyway), which were responsible for the minor performance improvements over the "Deschutes" Pentium IIs. It was first released at speeds of 450 and 500 MHz in February 1999. Two more versions were released: 550 MHz on May 17, 1999 and 600 MHz on August 2, 1999. On September 27, 1999 Intel released the 533B and 600B running at 533 & 600 MHz respectively. The 'B' suffix indicated that it featured a 133 MHz FSB, instead of the 100 MHz FSB of previous models.
The Katmai contains 9.5 million transistors, not including the 512 Kbytes L2 cache (which adds 25 million transistors), and has dimensions of 12.3 mm by 10.4 mm (128 mm2). It is fabricated in Intel's P856.5 process, a 0.25 micrometre CMOS process with five levels of aluminum interconnect.[2] The Katmai used the same slot-based design as the Pentium II but with the newer SECC2 cartridge that allowed direct CPU core contact with the heat sink. There have been some early models of the Pentium III with 450 and 500 MHz packaged in an older SECC cartridge intended for OEMs.
A notable stepping for enthusiasts was SL35D. This version of Katmai was officially rated for 450 MHz, but often contained cache chips for the 600 MHz model and thus usually was capable of running at 600 MHz.
Coppermine[edit]
A 900 MHz Coppermine FC-PGA Pentium III.
The second version, codenamed Coppermine (Intel product code: 80526), was released on October 25, 1999, running at 500, 533, 550, 600, 650, 667, 700, and 733 MHz. From December 1999 to May 2000, Intel released Pentium IIIs running at speeds of 750, 800, 850, 866, 900, 933 and 1000 MHz (1 GHz). Both 100 MHz FSB and 133 MHz FSB models were made. For models that were already available with the same frequency, an "E" was appended to the model name to indicate cores using the new 0.18 μm fabrication process. An additional "B" was later appended to designate 133 MHz FSB models, resulting in an "EB" suffix. In terms of overall performance, the Coppermine held a slight advantage over the AMD Athlons it was released against, which was reversed when AMD applied their own die shrink and added an on-die L2 cache to the Athlon. Athlon held the advantage in floating-point intensive code, while the Coppermine could perform better when SSE optimizations were used, but in practical terms there was little difference in how the two chips performed, clock-for-clock. However, AMD were able to clock the Athlon higher, reaching speeds of 1.2 GHz before the launch of the Pentium 4.
In terms of performance, Coppermine arguably marked a bigger step than Katmai by introducing an on-chip L2 cache (which Intel called Advanced Transfer Cache, or ATC). The ATC operates at the core clock rate and has a capacity of 256 KB, twice that of the on-chip cache previously seen on Mendocino Celerons. It is eight-way set-associative and is accessed via a Double Quad Word Wide 256-bit bus, four times as wide as Katmai's. Furthermore, latency was dropped to a quarter compared to Katmai. Another marketing term by Intel was Advanced System Buffering, which encompassed improvements to better take advantage of a 133 MHz system bus. These include 6 fill buffers (vs. 4 on Katmai), 8 bus queue entries (vs. 4 on Katmai) and 4 write-back buffers (vs. 1 on Katmai).[3] Under competitive pressure from the AMD Athlon, Intel re-worked the internals, finally removing some well-known pipeline stalls.[citation needed] The result was that applications affected by these pipeline stalls ran faster on the Coppermine by up to 30%.[citation needed] The Coppermine contained 29 million transistors and was fabricated in a 0.18 µm process.
Although its codename gives the impression that it used copper interconnects, its interconnects were in fact aluminium. The Coppermine was packaged in a 370-pin FC-PGA or FC-PGA2 for use with Socket 370, or in SECC2 for Slot 1. Early PGA versions have an exposed die, whereas higher frequency SKUs (866, 933, 1000EB, 1133) were also produced in an FC-PGA2 variant with integrated heat spreader (IHS) to improve contact between the die and the heatsink. This in itself did not improve thermal conductivity, since it added another layer of metal and thermal paste between the die and the heatsink, but it greatly assisted in holding the heatsink flat against the die. Earlier Coppermines without the IHS made heatsink mounting challenging.[4] If the heatsink was not flat against the die, heat transfer efficiency was greatly reduced. Some heatsink manufacturers began providing pads on their products, similar to what AMD did with the "Thunderbird" Athlon to ensure that the heatsink was mounted flatly. The enthusiast community went so far as to create shims to assist in maintaining a flat interface.[5]
A 1.13 GHz version was released in mid-2000 but famously recalled after a collaboration between HardOCP and Tom's Hardware[6] discovered various instabilities with the operation of the new CPU speed grade. The Coppermine core was unable to reliably reach the 1.13 GHz speed without various tweaks to the processor's microcode, effective cooling, additional voltage (1.75 V vs. 1.65 V), and specifically validated platforms.[6] Intel only officially supported the processor on its own VC820 i820-based motherboard, but even this motherboard displayed instability in the independent tests of the hardware review sites. In benchmarks that were stable, performance was shown to be sub-par, with the 1.13 GHz CPU equalling a 1.0 GHz model. Tom's Hardware attributed this performance deficit to relaxed tuning of the CPU and motherboard to improve stability.[7] Intel needed at least six months to resolve the problems using a new cD0 stepping and re-released 1.1 GHz and 1.13 GHz versions in 2001.
Microsoft's Xbox game console uses a variant of the Pentium III/Mobile Celeron family in a Micro-PGA2 form factor. The sSpec designator of the chips is SL5Sx, which makes it most similar to the Mobile Celeron Coppermine-128 processor. It shares with the Coppermine-128 Celeron its 128 KB L2 cache, and 180 nm process technology, but keeps the 8-way cache associativity from the Pentium III.[8]
Coppermine T[edit]
This revision is an intermediate step between Coppermine and Tualatin, with support for lower-voltage system logic present on the latter but core power within previously defined voltage specs of the former so it could work in older system boards.
Intel used the latest Coppermines with the cD0-Stepping and modified them so that they worked with low voltage system bus operation at 1.25 V AGTL as well as normal 1.5 V AGTL+ signal levels, and would auto detect differential or single-ended clocking. This modification made them compatible to the latest generation Socket-370 boards supporting FC-PGA2 packaged CPUs while maintaining compatibility with the older FC-PGA boards. The Coppermine T also had two way symmetrical multiprocessing capabilities, but only in FC-PGA2 boards.
They can be distinguished from Tualatin processors by their part numbers, which include the digits: 80533 e.g. the 1133 MHz SL5QK P/N is: RK80533PZ006256, while the 1000 MHz SL5QJ P/N is: RK80533PZ001256.[9]
Tualatin[edit]
A 1.13 GHz FC-PGA2 Tualatin-256 Intel Pentium III-T.
The third revision, Tualatin (80530), was a trial for Intel's new 0.13 µm process. Tualatin-based Pentium IIIs were released during 2001 until early 2002 at speeds of 1.0, 1.13, 1.2, 1.26, 1.33 and 1.4 GHz. A basic shrink of Coppermine, no new features were added, except for added data prefetch logic similar to Pentium 4 and Athlon XP for potentially better use of the L2 cache, although its use compared to these newer CPUs is limited due to the relatively smaller FSB bandwidth (FSB was still kept at 133 MHz).[10] Variants with 256 and 512 KB L2 cache were produced, the latter being dubbed Pentium III-S; this variant was mainly intended for low-power consumption servers and also exclusively featured SMP support within the Tualatin line.
Although the Socket 370 designation was kept, the use of 1.25 AGTL signaling in place of 1.5V AGTL+ rendered previous motherboards incompatible.[10] This confusion carried over to the chipset naming, where only the B-stepping of the i815 chipset was compatible with Tualatin processors.[11] A new VRM guideline was also designed by Intel, version 8.5, which required finer voltage steps and debuted load line Vcore (in place of fixed voltage regardless of current on 8.4).[12][13][14] Some motherboard manufacturers would mark the change with blue sockets (instead of white), and were often also backwards compatible with Coppermine CPUs.
The Tualatin also formed the basis for the highly popular Pentium III-M mobile processor, which became Intel's front-line mobile chip (the Pentium 4 drew significantly more power, and so was not well-suited for this role) for the next two years. The chip offered a good balance between power consumption and performance, thus finding a place in both performance notebooks and the "thin and light" category.
The Tualatin-based Pentium III performed well in some applications compared to the fastest Willamette-based Pentium 4, and even the Thunderbird-based Athlons. Despite this, its appeal was limited due to the aforementioned incompatibility with existing systems, and Intel's only officially supported chipset for Tualatins (except 3rd party server-line chipsets found on expensive server boards), the i815, could only handle 512 MB RAM and had slightly inferior performance because of a maximum in-order queue depth of 4, compared to 8 with the older, incompatible 440BX chipset. However, the enthusiast community found a way to run Tualatins on then-ubiquitous BX chipset based boards, although it was often a non-trivial task and required some degree of technical skills.
Tualatin-based Pentium III CPUs can usually be visually distinguished from Coppermine-based processors by the metal integrated heat-spreader (IHS) fixed on top of the package. However, the very last models of Coppermine Pentium IIIs also featured the IHS — the integrated heat spreader is actually what distinguishes the FC-PGA2 package from the FC-PGA — both are for Socket 370 motherboards.[15]
Before the addition of the heat spreader, it was sometimes difficult to install a heatsink on a Pentium III. One had to be careful not to put force on the core at an angle because doing so would cause the edges and corners of the core to crack and could destroy the CPU. It was also sometimes difficult to achieve a flat mating of the CPU and heatsink surfaces, a factor of critical importance to good heat transfer. This became increasingly challenging with the Socket 370 CPUs, compared with their Slot 1 predecessors, because of the force required to mount a socket-based cooler and the narrower, 2-sided mounting mechanism (Slot 1 featured 4-point mounting). As such, and because the 0.13 µm Tualatin had an even smaller core surface area than the 0.18 µm Coppermine, Intel installed the metal heatspreader on Tualatin and all future desktop processors.
The Tualatin core was named after the Tualatin Valley and Tualatin River in Oregon, where Intel has large manufacturing and design facilities.
Pentium III's SSE implementation[edit]
Slot 1 Pentium III CPU mounted on a motherboard
Since Katmai was built in the same 0.25 µm process as Pentium II "Deschutes", it had to implement SSE using as little silicon as possible.[16] To achieve this goal, Intel implemented the 128-bit architecture by double-cycling the existing 64-bit data paths and by merging the SIMD-FP multiplier unit with the x87 scalar FPU multiplier into a single unit. To utilize the existing 64-bit data paths, Katmai issues each SIMD-FP instruction as two μops. To compensate partially for implementing only half of SSE’s architectural width, Katmai implements the SIMD-FP adder as a separate unit on the second dispatch port. This organization allows one half of a SIMD multiply and one half of an independent SIMD add to be issued together bringing the peak throughput back to four floating point operations per cycle — at least for code with an even distribution of multiplies and adds.[2][17]
The issue was that Katmai’s hardware-implementation contradicted the parallelism model implied by the SSE instruction-set. Programmers faced a code-scheduling dilemma: Should the SSE-code be tuned for Katmai's limited execution resources, or should it be tuned for a future processor with more resources? Katmai-specific SSE optimizations yielded the best possible performance from the Pentium III family but was suboptimal for Coppermine onwards as well as future Intel processors, such as the Pentium 4 and Core series.
Core specifications[edit]
Main article: List of Intel Pentium III microprocessors
Katmai (0.25 µm)[edit]
L1-Cache: 16 + 16 KB (data + instructions)
L2-Cache: 512 KB, external chips on CPU module at 50% of CPU-speed
MMX, SSE
Slot 1 (SECC, SECC2)
VCore: 2.0 V, (600 MHz: 2.05 V)
Clockrate: 450–600 MHz
100 MHz FSB: 450, 500, 550, 600 MHz (These models have no letter after the speed)
133 MHz FSB: 533, 600 MHz
Coppermine (0.18 µm)[edit]
L1-Cache: 16 + 16 KB (data + instructions)
L2-Cache: 256 KB, fullspeed
MMX, SSE
Slot 1 (SECC2), Socket 370 (FC-PGA, FC-PGA2)
Front side bus: 100, 133 MHz
VCore: 1.6 V, 1.65 V, 1.70 V, 1.75 V
First release: October 25, 1999
Clockrate: 500–1133 MHz
100 MHz FSB: 500, 550, 600, 650, 700, 750, 800, 850, 900, 1000, 1100 MHz (E-Models)
133 MHz FSB: 533, 600, 667, 733, 800, 866, 933, 1000, 1133 MHz (EB-Models)
Coppermine T (0.18 µm)[edit]
L1-Cache: 16 + 16 KB (data + instructions)
L2-Cache: 256 KB, fullspeed
MMX, SSE
Socket 370 (FC-PGA, FC-PGA2)
Front side bus: 133 MHz
VCore: 1.75 V
First release: August 2000
Clockrate: 800–1133 MHz
133 MHz FSB: 800, 866, 933, 1000, 1133 MHz
Tualatin (0.13 µm)[edit]
L1-Cache: 16 + 16 KB (data + instructions)
L2-Cache: 256 or 512 KB, fullspeed
MMX, SSE, Hardware prefetch
Socket 370 (FC-PGA2)
Front side bus: 133 MHz
VCore: 1.45, 1.475 V
First release: 2001
Clockrate: 1000–1400 MHz
Pentium III (256 KB L2-Cache): 1000, 1133, 1200, 1333, 1400 MHz
Pentium III-S (512 KB L2-Cache): 1133, 1266, 1400 MHz
Controversy about privacy issues[edit]
The Pentium III was the first x86 CPU to include a unique, retrievable, identification number, called PSN (Processor Serial Number). A Pentium III's PSN can be read by software through the CPUID instruction if this feature has not been disabled through the BIOS.
On November 29, 1999, the Science and Technology Options Assessment (STOA) Panel of the European Parliament, following their report on electronic surveillance techniques asked parliamentary committee members to consider legal measures that would "prevent these chips from being installed in the computers of European citizens."[18]
Intel eventually removed the PSN feature from Tualatin-based Pentium IIIs, and the feature was not present in Pentium 4 or Pentium M.
See also[edit]
Intel Pentium 4 microprocessor
List of Intel Pentium III microprocessors
List of Intel Celeron microprocessors
References[edit]
Jump up ^ Microprocessor Hall of Fame, Intel Corporation, archived from the original on April 6, 2008, retrieved August 11, 2007
^ Jump up to: a b Diefendorff, Keith (March 8, 1999). "Pentium III = Pentium II + SSE: Internet SSE Architecture Boosts Multimedia Performance" (PDF). Microprocessor Report. Volume 13, Number 3. Retrieved September 1, 2017.
Jump up ^ Pabst, Thomas (October 25, 1999). "Coppermine's New Enhancements". Retrieved September 1, 2017.
Jump up ^ "Alpha FC-PAL35T & POP66T Cooler Review". The Tech Zone. April 12, 2000. Archived from the original on June 27, 2006.
Jump up ^ Verbist, Tim. Copper Shims, Overclockers Online, December 3, 2000.
^ Jump up to: a b Pabst, Thomas. "Intel Admits Problems With Pentium III 1.13 GHz: Production and Shipments Halted". Tom's Hardware.
Jump up ^ Pabst, Thomas (August 28, 2000). "Latest Update On Intel's 1.13 GHz Pentium III". Tom's Hardware.
Jump up ^ "VHJ: More on the Xbox CPU". Van's Hardware Journal.
Jump up ^ Intel Pentium III Coppermine-T core, retrieved July 8, 2010
^ Jump up to: a b Shimpi, Anand Lal (July 30, 2001). "Intel Pentium III 1.2GHz 0.13-micron Tualatin: The Celeron of the Future". Anandtech. Retrieved April 5, 2018.
Jump up ^ "B-Stepping With The I815/Solano - Last Passing Maneuver: Tualatin 1266 With 512 kB Versus Athlon And P4". Tom's Hardware. September 19, 2001. Retrieved April 5, 2018.
Jump up ^ Labs, iXBT. "Server Tualatin CPU review". iXBT Labs. Retrieved April 5, 2018.
Jump up ^ Labs, iXBT. "iXBT Labs Review - Tualatin based Intel Celeron 1.2 GHz for Socket 370". iXBT Labs. Retrieved April 5, 2018.
Jump up ^ http://cdn14.21dianyuan.com/download.php?id=89124
Jump up ^ Lal Shimpi, Anand. Intel Pentium III 1.2 GHz 0.13-micron Tualatin: The Celeron of the Future, Anandtech, July 30, 2001.
Jump up ^ Jagannath Keshava, Vladimir Pentkovski (1999). "Pentium III Processor Implementation Tradeoffs" (PDF). Intel Technology Journal. Retrieved September 1, 2017.
Jump up ^ "Intel®Architecture Optimization - Reference Manual" (PDF). 1999. Retrieved September 1, 2017.
Jump up ^ Advisory group asks EU to consider Pentium III ban, CNN, November 29, 1999.
External links[edit]
Listing of various PII, PIII, and Celeron alphanumeric model designations
Comparison of 7th generation x86 CPU architectures
Intel FAQ about the pentium III processor serial number
Intel datasheets
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values: Pentium III – Belarusian (Taraškievica orthography)

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values: පෙන්ටියම් III – Sinhala

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