Difference between revisions of "Metre"

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==History==
 
==History==
 
===Universal measure===
 
===Universal measure===
−
The standard measures of length in Europe diverged from one another following the fall of Charlemagne's Empire: while measures could be standardized within a given jurisdiction (which was often little more than a single market town), they were numerous varieties of measure between regions. Indeed, as the measures were often used as the basis for taxation (of cloth, for example), the use of a certain measure was associated with the sovereignty of a given ruler and often dictated by law.<ref name="Larousse">{{LarousseXIXe | article = Métrique | volume = 11 | pages = 163–64}}.</ref>
+
The standard measures of length in Europe diverged from one another following the fall of Charlemagne's Empire: while measures could be standardized within a given jurisdiction (which was often little more than a single market town), they were numerous varieties of measure between regions. Indeed, as the measures were often used as the basis for taxation (of cloth, for example), the use of a certain measure was associated with the sovereignty of a given ruler and often dictated by law.<ref name="Larousse">{{LarousseXIXe | article = Métrique | volume = 11 | pages = 163–64}}.</ref><ref name="Nelson">{{citation | first = Robert A. | last = Nelson | title = Foundations of the international system of units (SI) | journal = Phys. Teacher | year = 1981 | pages = 596–613 | url = http://plato.if.usp.br/1-2009/fmt0159n/PDFFiles/ThePhysTeacher_FoundationsOfTheSI.pdf}}.</ref>
  
 
Nevertheless, with the increasing scientific activity of the seventeenth century came calls for the institution of a "universal measure" (as Englishman [[John Wilkins]] called it<ref>{{citation | first = John | last = Wilkins | authorlink = John Wilkins | title = An Essay Towards a Real Character, And a Philosophical Language | location = London | publisher = Gillibrand | year = 1668 | url = http://www.metricationmatters.com/docs/WilkinsTranslationLong.pdf}}.</ref>) or "''metro cattolico''" (Italian [[Tito Livio Burattini]]<ref>{{citation | title = Misura Universale | year = 1675}}.</ref>), which would be based on a natural phenomenon rather than royal decree, and would also be decimal rather than the various systems of multipliers, often duodecimal, that coexisted at the time.
 
Nevertheless, with the increasing scientific activity of the seventeenth century came calls for the institution of a "universal measure" (as Englishman [[John Wilkins]] called it<ref>{{citation | first = John | last = Wilkins | authorlink = John Wilkins | title = An Essay Towards a Real Character, And a Philosophical Language | location = London | publisher = Gillibrand | year = 1668 | url = http://www.metricationmatters.com/docs/WilkinsTranslationLong.pdf}}.</ref>) or "''metro cattolico''" (Italian [[Tito Livio Burattini]]<ref>{{citation | title = Misura Universale | year = 1675}}.</ref>), which would be based on a natural phenomenon rather than royal decree, and would also be decimal rather than the various systems of multipliers, often duodecimal, that coexisted at the time.
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For all of these reasons, it was decided in the early 1870s to make a new, international prototype metre<ref name="MComm"/><ref name="BIPMhist"/><ref group="Note">The term "prototype" does not imply that it was the first in a series and that other standard metres would come after it: the "prototype" metre was the one that came first in the logical chain of comparisons, that is the metre to which all other standards were compared.</ref> and to arrange a system where national standards could be compared with it. The international prototype would also be a "line standard", that is the metre was defined as the distance between two lines marked on the bar, so avoiding the wear problems of end standards.
 
For all of these reasons, it was decided in the early 1870s to make a new, international prototype metre<ref name="MComm"/><ref name="BIPMhist"/><ref group="Note">The term "prototype" does not imply that it was the first in a series and that other standard metres would come after it: the "prototype" metre was the one that came first in the logical chain of comparisons, that is the metre to which all other standards were compared.</ref> and to arrange a system where national standards could be compared with it. The international prototype would also be a "line standard", that is the metre was defined as the distance between two lines marked on the bar, so avoiding the wear problems of end standards.
  
−
The international nature of the standards was ensured by a treaty – the [[Metre Convention]] – signed in Paris on 20&nbsp;May 1875. This set up an international organization, the ''[[Bureau international des poids et mesures]]'' (BIPM), to conserve the prototypes (which were to be the joint property of the signatory nations) and to carry out regular comparisons with national standards. In recognition of the role of France in designing the metric system, the BIPM is based in Sèvres, just outside Paris, but it enjoys the usual privileges of an international organization and is under the ultimate control of a diplomatic conference (the ''[[Conférence générale des poids et mesures]]'', CGPM) and not of the French government.<ref>Article 3, [[Metre Convention]].</ref>
+
The international nature of the standards was ensured by a treaty – the [[Metre Convention]] – signed in Paris on 20&nbsp;May 1875. This set up an international organization, the ''[[Bureau international des poids et mesures]]'' (BIPM), to conserve the prototypes (which were to be the joint property of the signatory nations) and to carry out regular comparisons with national standards. In recognition of the role of France in designing the metric system, the BIPM is based in Sèvres, just outside Paris, but it enjoys the usual privileges of an international organization and is under the ultimate control of a diplomatic conference (the ''[[Conférence générale des poids et mesures]]'', CGPM) and not of the French government.<ref name="Nelson"/><ref>Article 3, [[Metre Convention]].</ref>
  
−
The construction of the international prototype metre and the copies which would be national standards was at the limits of the technology of its time. The bars were to be made of a special alloy, 90%&nbsp;[[platinum]] and 10%&nbsp;[[iridium]], which is significantly harder than pure platinum, and have a special X-shaped cross section to minimise the effects of torsional strain during length comparisons. The first castings proved unsatisfactory, and the job was given to the London firm of [[Johnson Matthey]] who succeded in producing thirty bars to the required specification: one of these (No.&nbsp;6) was determined to be identical in length, and was consacrated as the international prototype metre at the first meeting of the CGPM in 1889. The other bars, duely calibrated against the international prototype, were distributed to the signatory nations of the Metre Convention for use as national standards.<ref name="BIPMhist"/>
+
The construction of the international prototype metre and the copies which would be national standards was at the limits of the technology of its time. The bars were to be made of a special alloy, 90%&nbsp;[[platinum]] and 10%&nbsp;[[iridium]], which is significantly harder than pure platinum, and have a special X-shaped cross section to minimise the effects of torsional strain during length comparisons.<ref name="Nelson"/> The first castings proved unsatisfactory, and the job was given to the London firm of [[Johnson Matthey]] who succeded in producing thirty bars to the required specification: one of these (No.&nbsp;6) was determined to be identical in length, and was consacrated as the international prototype metre at the first meeting of the CGPM in 1889. The other bars, duely calibrated against the international prototype, were distributed to the signatory nations of the Metre Convention for use as national standards.<ref name="BIPMhist"/>
  
−
The first (and only) follow-up comparison of the national standards with the international prototype was carried out between 1921 and 1936.<ref name="BIPMhist"/> At this time, it was decided that a more formal definition of the metre was required (the 1889 decision had said merely that the "prototype, at the temperature of melting ice, shall henceforth represent the metric unit of length"), and this was agreed at the 7th&nbsp;CGPM in 1927:<ref name="oldSI">{{SIbrochure8th|pages=142–43, 148}}.</ref>
+
The first (and only) follow-up comparison of the national standards with the international prototype was carried out between 1921 and 1936,<ref name="Nelson"/><ref name="BIPMhist"/> and indicated that the definition of the metre was preserved to with 0.2&nbsp;µm.<ref name="Barrell">{{citation | first = H. | last = Barrel | title = The Metre | journal = Contemp. Phys. | year = 1962 | volume = 3 | issue = 6 | pages = 415–34 | doi = 10.1080/00107516208217499}}.</ref> At this time, it was decided that a more formal definition of the metre was required (the 1889 decision had said merely that the "prototype, at the temperature of melting ice, shall henceforth represent the metric unit of length"), and this was agreed at the 7th&nbsp;CGPM in 1927:<ref name="oldSI">{{SIbrochure8th|pages=142–43, 148}}.</ref>
 
{{quotation|The unit of length is the metre, defined by the distance, at 0°, between the axes of the two central lines marked on the bar of platinum–iridium kept at the ''Bureau International des Poids et Mesures'' and declared Prototype of the metre by the 1st&nbsp;''Conférence Générale des Poids et Mesures'', this bar being subject to standard atmospheric pressure and supported on two cylinders of at least one centimetre diameter, symmetrically placed in the same horizontal plane at a distance of 571&nbsp;mm from each other.}}
 
{{quotation|The unit of length is the metre, defined by the distance, at 0°, between the axes of the two central lines marked on the bar of platinum–iridium kept at the ''Bureau International des Poids et Mesures'' and declared Prototype of the metre by the 1st&nbsp;''Conférence Générale des Poids et Mesures'', this bar being subject to standard atmospheric pressure and supported on two cylinders of at least one centimetre diameter, symmetrically placed in the same horizontal plane at a distance of 571&nbsp;mm from each other.}}
 
The support requirements represent the [[Airy points]] of the prototype, that is the points, separated by {{frac|5|9}} of the total length of the bar, at which the bending or droop of the bar is minimized.<ref>{{citation | last = Phelps | first = F. M., III | year = 1966 | title = Airy Points of a Meter Bar | journal = Am. J. Phys. | volume = 34 | issue = 5 | pages = 419–22 | doi = 10.1119/1.1973011}}.</ref>
 
The support requirements represent the [[Airy points]] of the prototype, that is the points, separated by {{frac|5|9}} of the total length of the bar, at which the bending or droop of the bar is minimized.<ref>{{citation | last = Phelps | first = F. M., III | year = 1966 | title = Airy Points of a Meter Bar | journal = Am. J. Phys. | volume = 34 | issue = 5 | pages = 419–22 | doi = 10.1119/1.1973011}}.</ref>
  
 
===Krypton standard===
 
===Krypton standard===
−
The first [[Interferometry|interferometric]] measurements carried out using the international prototype metre were those of [[Albert A. Michelson|Michelson]] and [[Benoît]] (1892–93)<ref>{{citation | first1 = A. A. | last1 = Michelson | authorlink1 = Albert A. Michelson | first2 = J.-R. | last2 = Benoît | title =  Détermination expérimentale de la valeur du mètre en longueurs d'ondes lumineuses | journal = Trav. Mem. Bur. Int. Poids Mes. | volume = 11 | issue = 3 | pages = 85 | year = 1895}}.</ref> and of Benoît, [[Charles Fabry|Fabry]] and [[Alfred Perot|Perot]] (1906),<ref>{{citation | last1 = Benoit | first1 = R. | last2 = Fabry | first2 = Ch. | authorlink2 = Charles Fabry | last3 = Perot | first3 = A. | authorlink3 = Alfred Perot | year = 1907 | title = Nouvelle détermination du Mètre en longueurs d'ondes lumieuses | journal = C. R. Hebd. Acad. Sci. Paris | volume = 144 | pages = 1082–86 | url = http://gallica.bnf.fr/ark:/12148/bpt6k3098j.image.f1082.langFR}}.</ref> both using the red line of [[cadmium]]. These results, which gave the [[wavelength]] of the cadmium line (''λ''&nbsp;≈ 644&nbsp;nm), led to the definition of the [[angstrom]] as a secondary unit of length for spectroscopic measurements, first by the [[International Union for Solar Research]] (1907)<ref>{{citation | journal = Trans. Int. Union Solar Res. | volume = 2 | pages = 28 | year = 1907}}.</ref> and later by the CIPM (1927).<ref name="BIPMhist"/> Michelson's work in "measuring" the prototype metre to within {{frac|10}} of a wavelength ({{nowrap|< 0.1}}&nbsp;µm) was one of the reasons for which he was awarded the [[Nobel Prize in Physics]] in 1907.<ref>{{citation | title = Nobel Prize in Physics 1907 – Presentation Speech | url = http://nobelprize.org/nobel_prizes/physics/laureates/1907/press.html | publisher = Nobel Foundation | accessdate = 2010-08-14}}.</ref>
+
The first [[Interferometry|interferometric]] measurements carried out using the international prototype metre were those of [[Albert A. Michelson|Michelson]] and [[Benoît]] (1892–93)<ref>{{citation | first1 = A. A. | last1 = Michelson | authorlink1 = Albert A. Michelson | first2 = J.-R. | last2 = Benoît | title =  Détermination expérimentale de la valeur du mètre en longueurs d'ondes lumineuses | journal = Trav. Mem. Bur. Int. Poids Mes. | volume = 11 | issue = 3 | pages = 85 | year = 1895}}.</ref> and of Benoît, [[Charles Fabry|Fabry]] and [[Alfred Perot|Perot]] (1906),<ref>{{citation | last1 = Benoit | first1 = R. | last2 = Fabry | first2 = Ch. | authorlink2 = Charles Fabry | last3 = Perot | first3 = A. | authorlink3 = Alfred Perot | year = 1907 | title = Nouvelle détermination du Mètre en longueurs d'ondes lumieuses | journal = C. R. Hebd. Acad. Sci. Paris | volume = 144 | pages = 1082–86 | url = http://gallica.bnf.fr/ark:/12148/bpt6k3098j.image.f1082.langFR}}.</ref> both using the red line of [[cadmium]]. These results, which gave the [[wavelength]] of the cadmium line (''λ''&nbsp;≈ 644&nbsp;nm), led to the definition of the [[angstrom]] as a secondary unit of length for spectroscopic measurements, first by the [[International Union for Solar Research]] (1907)<ref>{{citation | journal = Trans. Int. Union Solar Res. | volume = 2 | pages = 28 | year = 1907}}.</ref> and later by the CIPM (1927).<ref name="BIPMhist"/><ref>{{citation | first1 = L. | last1 = Hollberg | first2 = C. W. | last2 = Oates | first3 = G. | last3 = Wilpers | first4 = C. W. | last4 = Hoyt | first5 =  Z. W. | last5 = Barber | first6 = S. A. | last6 = Diddams | first7 = W. H. | last7 = Oskay | first8 = J. C. | last8 = Bergquist | title = Optical frequency/wavelength references | journal = J. Phys. B: At. Mol. Opt. Phys. | volume = 38 | year = 2005 | pages = S469–S495 | doi = 10.1088/0953-4075/38/9/003}}.</ref><ref group="Note">The IUSR (later to be come the [[International Astronomical Union]]) defined the angstrom such that the wavelength (in air) of the cadmium line was {{nowrap|6438.469 63}}&nbsp;Å.</ref> Michelson's work in "measuring" the prototype metre to within {{frac|10}} of a wavelength ({{nowrap|< 0.1}}&nbsp;µm) was one of the reasons for which he was awarded the [[Nobel Prize in Physics]] in 1907.<ref name="Nelson"/><ref name="BIPMhist"/><ref>{{citation | title = Nobel Prize in Physics 1907 – Presentation Speech | url = http://nobelprize.org/nobel_prizes/physics/laureates/1907/press.html | publisher = Nobel Foundation | accessdate = 2010-08-14}}.</ref>
  
 
By the 1950s, interferometry had become the method of choice for precise measurements of length but there remained a practical problem imposed by the system of units used. The natural unit for expressing a length measured by interferometry was the angstrom, but this result then had to be converted into metres using an experimental conversion factor – the wavelength of light used, but measured in metres rather than in angstroms. This added an additional [[measurement uncertainty]] to any length result in metres, over and above the uncertainty of the actual interferometric measurement. The solution was to define the metre in the same manner as the angstrom had been defined in 1907, that is in terms of the best interferometric wavelength available.
 
By the 1950s, interferometry had become the method of choice for precise measurements of length but there remained a practical problem imposed by the system of units used. The natural unit for expressing a length measured by interferometry was the angstrom, but this result then had to be converted into metres using an experimental conversion factor – the wavelength of light used, but measured in metres rather than in angstroms. This added an additional [[measurement uncertainty]] to any length result in metres, over and above the uncertainty of the actual interferometric measurement. The solution was to define the metre in the same manner as the angstrom had been defined in 1907, that is in terms of the best interferometric wavelength available.
  
−
Advances in both experimental technique and theory showed that the cadmium line was actually a cluster of closely separated lines, and that this was due to the presence of different [[isotope]]s in natural cadmium (eight in total). To get the most precisely defined line, it was necessary to use a monoisotopic source and this source should contain an isotope with even numbers of protons and neutrons (so as to have zero [[nuclear spin]]). Several isotopes of cadmium, [[krypton]] and [[mercury]] both fulfill the condition of zero nuclear spin and have bright lines in the visible region of the spectrum: it is easier to perform [[isotopic enrichment]] for krypton than for cadmium or mercury as it is a gas at room temperature, and so it was decided to select the orange line of [[krypton-86]] (''λ''&nbsp;≈ 606&nbsp;nm) as the new wavelength standard.<ref>{{citation | title = The International Length Standard | first1 = K. M. | last1 = Baird | first2 = L. E. | last2 = Howlett | journal = Appl. Opt. | volume = 2 | issue = 5 | pages = 455–63 | year = 1963 | doi = 10.1364/AO.2.000455}}.</ref><ref>{{citation | first = Robert A. | last = Nelson | title = Foundations of the international system of units (SI) | journal = Phys. Teacher | year = 1981 | pages = 596–613 | url = http://plato.if.usp.br/1-2009/fmt0159n/PDFFiles/ThePhysTeacher_FoundationsOfTheSI.pdf}}.</ref><ref>{{citation | first1 = L. | last1 = Hollberg | first2 = C. W. | last2 = Oates | first3 = G. | last3 = Wilpers | first4 = C. W. | last4 = Hoyt | first5 =  Z. W. | last5 = Barber | first6 = S. A. | last6 = Diddams | first7 = W. H. | last7 = Oskay | first8 = J. C. | last8 = Bergquist | title = Optical frequency/wavelength references | journal = J. Phys. B: At. Mol. Opt. Phys. | volume = 38 | year = 2005 | pages = S469–S495 | doi = 10.1088/0953-4075/38/9/003}}.</ref> Accordingly, the 11th&nbsp;CGPM in 1960 agreed a new definition of the metre:<ref name="oldSI"/>
+
Advances in both experimental technique and theory showed that the cadmium line was actually a cluster of closely separated lines, and that this was due to the presence of different [[isotope]]s in natural cadmium (eight in total). To get the most precisely defined line, it was necessary to use a monoisotopic source and this source should contain an isotope with even numbers of protons and neutrons (so as to have zero [[nuclear spin]]).<ref name="Nelson"/> Several isotopes of cadmium, [[krypton]] and [[mercury]] both fulfill the condition of zero nuclear spin and have bright lines in the visible region of the spectrum: it is easier to perform [[isotopic enrichment]] for krypton than for cadmium or mercury as it is a gas at room temperature, and so it was decided to select the orange line of [[krypton-86]] (''λ''&nbsp;≈ 606&nbsp;nm) as the new wavelength standard.<ref name="Nelson"/><ref>{{citation | title = The International Length Standard | first1 = K. M. | last1 = Baird | first2 = L. E. | last2 = Howlett | journal = Appl. Opt. | volume = 2 | issue = 5 | pages = 455–63 | year = 1963 | doi = 10.1364/AO.2.000455}}.</ref> Accordingly, the 11th&nbsp;CGPM in 1960 agreed a new definition of the metre:<ref name="oldSI"/>
 
{{quotation|The metre is the length equal to {{nowrap|1 650 763.73}}&nbsp;wavelengths in vacuum of the radiation corresponding to the transition between the levels 2p<sub>10</sub> and 5d<sub>5</sub> of the krypton&nbsp;86 atom.}}
 
{{quotation|The metre is the length equal to {{nowrap|1 650 763.73}}&nbsp;wavelengths in vacuum of the radiation corresponding to the transition between the levels 2p<sub>10</sub> and 5d<sub>5</sub> of the krypton&nbsp;86 atom.}}
−
The measurement of the wavelength of the krypton line was ''not'' made directly against the international prototype metre.
+
The measurement of the wavelength of the krypton line was ''not'' made directly against the international prototype metre.<ref name="Nelson"/><ref name="Barrell"/>
  
 
==Notes and references==
 
==Notes and references==

Revision as of 11:26, 15 August 2010

The metre (symbol: m), spelled meter in the United States, is the SI unit of length and one of the seven base units in the International System of Units. The name is derived from the Greek μέτρον (metron) meaning "measure", and gives rise to the term "metric system", a system of units of which the metre is one.

The metre was conceived in the aftermath of the French Revolution (1789) as a replacement for the old units of length that were associated with the ancien régime. Although there was initially considerable resistance to the adoption of the new units in France (including an official reversion to the mesures usuelles ["normal units"] for a period), the metre gained following in continental Europe during the mid nineteenth century, particularly in scientific usage, and was consacrated as an international measurement unit by the Metre Convention of 1875.

Definition

The current definition of the metre was agreed at the 17th General Conference on Weights and Measures (CGPM) in 1983:[1]

The metre is the length of the path travelled by light in vacuum during a time interval of 1/299 792 458 of a second.

This definition has the effect that the speed of light in vacuum has an exact, defined value in SI units: 299 792 458 m s−1.

Relativity

The metre is considered to be a unit of proper length. As such, the definition is only adequate in itself for measurements in an area where the local gravitational field can be considered to be uniform, a condition which is met by almost all measurements on the surface of the Earth (the Earth's gravitational field varies by about one part in 1016 per vertical metre, which is far less than the measurement uncertainty in Earth-based length measurements).[2] For astronomical measurements, the effects of general relativity cannot be ignored and the definition of the metre must be completed with a description of the metric tensor which defines the gravitational field.[3]

Realization

The metre can be realized either directly, by measuring the time taken for light to travel a certain distance, or by interferometry.[2][4]

Time-of-flight measurements

Interferometry

Source Stabilizing line (127I2) Frequency
THz 		Wavelength
nm 		ur
Helium–neon laser a16 component, R(127) 11-5 transition 473.612 353 604(10) 632.991 212 579(13) 2.1 × 10−11
Nd:YAG laser a10 component, R(56) 32-0 transition 563.260 223 513(5) 532.245 036 104(5) 8.9 × 10−12

For an unstabilized helium–neon laser (Ne 3s2→2p4 transition):[5]

f = 473.612 7 THz
λ = 632.990 8 nm
ur = 1.5 × 10−6

History

Universal measure

The standard measures of length in Europe diverged from one another following the fall of Charlemagne's Empire: while measures could be standardized within a given jurisdiction (which was often little more than a single market town), they were numerous varieties of measure between regions. Indeed, as the measures were often used as the basis for taxation (of cloth, for example), the use of a certain measure was associated with the sovereignty of a given ruler and often dictated by law.[6][7]

Nevertheless, with the increasing scientific activity of the seventeenth century came calls for the institution of a "universal measure" (as Englishman John Wilkins called it[8]) or "metro cattolico" (Italian Tito Livio Burattini[9]), which would be based on a natural phenomenon rather than royal decree, and would also be decimal rather than the various systems of multipliers, often duodecimal, that coexisted at the time.

Wilkins' idea was to choose the length of a "seconds pendulum" (a pendulum with a half-period of one second) as the unit length: such pendulums had recently been demonstrated by Christiaan Huygens, and their length is very close to one modern metre (as well as to length units which were then in use, such as the yard). However, it was soon discovered that the length of a seconds pendulum varies from place to place: French astronomer Jean Richer had measured the 0.3% difference in length between Cayenne (in French Guiana) and Paris.[10]

Little practical progress was made towards the establishment of the "universal measure" until the French Revolution of 1789. France was particularly affected by the proliferation of length measures, and the need for reform was widely accepted across all political viewpoints, even if needed the push of revolution to bring it about. Talleyrand resurrected the idea of the seconds pendulum before the Constituant Assembly in 1790, suggesting that the new measure be defined at 45°N (a latitude that, in France, runs just north of Bordeaux and just south of Grenoble): dispite the support of the Assembly, and of Great Britain and the newly independent United States, nothing came of Talleyrand's proposal.[6][Note 1]

Meridional definition

The question of measurement reform was placed in the hands of the Academy of Sciences who appointed a commission chaired by Jean-Charles de Borda. Borda could be said to have been a fanatic for decimalization: he had invented the "repeating circle", a surveying instrument which allowed a much-improved precision in the measurement of angles between landmarks, but insisted that it be calibrated in "grades" (1⁄100 of a quarter-circle) rather than degrees, with 100 minutes to a grade and 100 seconds to a minute.[11] For Borda, the seconds pendulum was a poor choice for a standard because the second (as a unit of time) was insufficiently decimal: he preferred a system of 10 hours to the day, 100 minutes to the hour and 100 seconds to the minute…

Instead, the commission – whose members included Lagrange, Laplace, Monge and Condorcet – decided that the new measure should be equal to one ten-millionth of the distance from the North Pole to the Equator (the quadrant of the Earth's circumference), measured along the meridian passing through Paris.[6] Apart from the obvious nationalistic considerations, the Paris meridian was also a sound choice for practical scientific reasons: a portion of the quadrant from Dunkerque to Barcelona (about 1000 km, or one-tenth of the total) could be surveyed with start- and end-points at sea level, and that portion was roughly in the middle of the quadrant, where the effects of the Earth's oblateness were expected to be the largest.[6]

The task of surveying the meridian fell to Pierre Méchain and Jean-Baptiste Delambre, and took more than six years (1792–98).[Note 2] In the meantime, the commission calculated a provisional value from older surveys of 443.44 lignes.[Note 3] Méchain and Delambre's result came out at 0.144 lignes shorter than this, a difference of about 0.03%.[6]

Mètre des Archives

While Méchain and Delambre were completing their survey, the comission had ordered a series of platinum bars to be made based on the provisional metre. When the final result was known, the bar whose length was closest to the meridional definition of the metre was selected and placed in the National Archives on 22 June 1799 (4 messidor An VII in the Republican calendar) as a permanent record of the result:[6] this standard metre bar became known as the mètre des Archives.

The metric system, that is the system of units based on the metre, was officially adopted in France on 10 December 1799 (19 frimaire An VIII) and became the sole legal system of weights and measures from 1801. After the instauration of the Empire, in 1812, the old names for units of length were revived but the units redefined in terms of the metre: this system was known as mesures usuelles, and lasted until 1840 when the decimal metric system was again made the sole legal measure.[6] In the meantime, the Netherlands had adopted the metric system from 1816, the first of several countries to follow the French lead.

It soon became apparent that Méchain and Delambre's result (443.296 lignes)[Note 3] was slightly too short for the meridional definition of the metre. Arago and Biot extended the survey to the island of Formentera in the western Mediterranean Sea in 1806–9, and found that one ten-millionth of the Earth's quadrant should be 443.31 lignes: later work increased the value to 443.39 lignes.[6] The modern value, for the WGS 84 reference spheroid, is 1.000 196 57 m or 443.383 08 lignes.[Note 4]

Nevertheless, the mètre des Archives remained the legal and practical standard for the metre in France, even once it was known that it did not exactly correspond to the meridional definition. When it was decided (in 1867) to create a new international standard metre, the length was taken to be that of the mètre des Archives "in the state in which it shall be found".[12][13]

International prototype metre

With increasing international adoption of the metre, the short-comings of the mètre des Archives as a standard became ever more apparent. Countries which adopted the metre as a legal measure purchased standard metre bars that were intended to be equal in length to the mètre des Archives, but there was no systematic way of ensuring that the countries were actually working to the same standard. The meriodional definition, which had been intended to ensure international reproduceability, quickly proved so impractical that is was abandoned in favour of the artefact standards, but the mètre des Archives (and most of its copies) were "end standards": such standards (bars which are exactly one metre in length) are prone to wear with use, and different standard bars could be expected to wear at different rates.

For all of these reasons, it was decided in the early 1870s to make a new, international prototype metre[12][13][Note 5] and to arrange a system where national standards could be compared with it. The international prototype would also be a "line standard", that is the metre was defined as the distance between two lines marked on the bar, so avoiding the wear problems of end standards.

The international nature of the standards was ensured by a treaty – the Metre Convention – signed in Paris on 20 May 1875. This set up an international organization, the Bureau international des poids et mesures (BIPM), to conserve the prototypes (which were to be the joint property of the signatory nations) and to carry out regular comparisons with national standards. In recognition of the role of France in designing the metric system, the BIPM is based in Sèvres, just outside Paris, but it enjoys the usual privileges of an international organization and is under the ultimate control of a diplomatic conference (the Conférence générale des poids et mesures, CGPM) and not of the French government.[7][14]

The construction of the international prototype metre and the copies which would be national standards was at the limits of the technology of its time. The bars were to be made of a special alloy, 90% platinum and 10% iridium, which is significantly harder than pure platinum, and have a special X-shaped cross section to minimise the effects of torsional strain during length comparisons.[7] The first castings proved unsatisfactory, and the job was given to the London firm of Johnson Matthey who succeded in producing thirty bars to the required specification: one of these (No. 6) was determined to be identical in length, and was consacrated as the international prototype metre at the first meeting of the CGPM in 1889. The other bars, duely calibrated against the international prototype, were distributed to the signatory nations of the Metre Convention for use as national standards.[13]

The first (and only) follow-up comparison of the national standards with the international prototype was carried out between 1921 and 1936,[7][13] and indicated that the definition of the metre was preserved to with 0.2 µm.[15] At this time, it was decided that a more formal definition of the metre was required (the 1889 decision had said merely that the "prototype, at the temperature of melting ice, shall henceforth represent the metric unit of length"), and this was agreed at the 7th CGPM in 1927:[16]

The unit of length is the metre, defined by the distance, at 0°, between the axes of the two central lines marked on the bar of platinum–iridium kept at the Bureau International des Poids et Mesures and declared Prototype of the metre by the 1st Conférence Générale des Poids et Mesures, this bar being subject to standard atmospheric pressure and supported on two cylinders of at least one centimetre diameter, symmetrically placed in the same horizontal plane at a distance of 571 mm from each other.

The support requirements represent the Airy points of the prototype, that is the points, separated by 5⁄9 of the total length of the bar, at which the bending or droop of the bar is minimized.[17]

Krypton standard

The first interferometric measurements carried out using the international prototype metre were those of Michelson and Benoît (1892–93)[18] and of Benoît, Fabry and Perot (1906),[19] both using the red line of cadmium. These results, which gave the wavelength of the cadmium line (λ ≈ 644 nm), led to the definition of the angstrom as a secondary unit of length for spectroscopic measurements, first by the International Union for Solar Research (1907)[20] and later by the CIPM (1927).[13][21][Note 6] Michelson's work in "measuring" the prototype metre to within 1⁄10 of a wavelength (< 0.1 µm) was one of the reasons for which he was awarded the Nobel Prize in Physics in 1907.[7][13][22]

By the 1950s, interferometry had become the method of choice for precise measurements of length but there remained a practical problem imposed by the system of units used. The natural unit for expressing a length measured by interferometry was the angstrom, but this result then had to be converted into metres using an experimental conversion factor – the wavelength of light used, but measured in metres rather than in angstroms. This added an additional measurement uncertainty to any length result in metres, over and above the uncertainty of the actual interferometric measurement. The solution was to define the metre in the same manner as the angstrom had been defined in 1907, that is in terms of the best interferometric wavelength available.

Advances in both experimental technique and theory showed that the cadmium line was actually a cluster of closely separated lines, and that this was due to the presence of different isotopes in natural cadmium (eight in total). To get the most precisely defined line, it was necessary to use a monoisotopic source and this source should contain an isotope with even numbers of protons and neutrons (so as to have zero nuclear spin).[7] Several isotopes of cadmium, krypton and mercury both fulfill the condition of zero nuclear spin and have bright lines in the visible region of the spectrum: it is easier to perform isotopic enrichment for krypton than for cadmium or mercury as it is a gas at room temperature, and so it was decided to select the orange line of krypton-86 (λ ≈ 606 nm) as the new wavelength standard.[7][23] Accordingly, the 11th CGPM in 1960 agreed a new definition of the metre:[16]

The metre is the length equal to 1 650 763.73 wavelengths in vacuum of the radiation corresponding to the transition between the levels 2p10 and 5d5 of the krypton 86 atom.

The measurement of the wavelength of the krypton line was not made directly against the international prototype metre.[7][15]

Notes and references

Notes

  1. ↑ The idea of the seconds pendulum as a length standard did not die completely, and such a standard was used to define the yard in the United Kingdom from 1843 to 1878.
  2. ↑ The technical difficulties were not the only problems the surveyors had to face in the convulsed period of the aftermath of the Revolution: Méchain and Delambre, and later Arago, were imprisoned several times during their surveys, and Méchain died in 1804 of yellow fever, which he contracted while trying to improve his original results in northern Spain.
  3. ↑ 3.0 3.1 All values in lignes are referred to the toise de Pérou, not to the later value in mesures usuelles. 1 toise = 6 pieds; 1 pied = 12 pouces; 1 pouce = 12 lignes; so 864 lignes = 1 toise.
  4. ↑ The WGS 84 reference spheroid has a semi-major axis of 6 378 137.0 m and a flattening of 1⁄298.257 223 563.
  5. ↑ The term "prototype" does not imply that it was the first in a series and that other standard metres would come after it: the "prototype" metre was the one that came first in the logical chain of comparisons, that is the metre to which all other standards were compared.
  6. ↑ The IUSR (later to be come the International Astronomical Union) defined the angstrom such that the wavelength (in air) of the cadmium line was 6438.469 63 Å.

References

  1. ↑ The International System of Units (SI), 8th ed.; International Bureau of Weights and Measures: Sèvres, France, 2006; p 112. ISBN 92-822-2213-6, <http://www.bipm.org/utils/common/pdf/si_brochure_8_en.pdf>.
  2. ↑ 2.0 2.1 Recommendation 1 (CI-2002), 91st Meeting of the International Committee on Weights and Measures, 2002.
  3. ↑ Guinot, B. Application of general relativity to metrology. Metrologia 1997, 34 (3), 261–90. DOI: 10.1088/0026-1394/34/3/9.
  4. ↑ Mise en pratique for the definition of the metre; Interntional Bureau for Weights and Measures, 2009, <http://www.bipm.org/en/si/si_brochure/appendix2/mep.html>. (accessed 13 August 2010).
  5. ↑ Recommendation 2 (CI-2007), 96th Meeting of the International Committee on Weights and Measures, 2007.
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 Métrique. In Grand dictionnaire universel du XIXe siècle; Pierre Larousse: Paris, 1874; Vol. 11, pp 163–64.
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 Nelson, Robert A. Foundations of the international system of units (SI). Phys. Teacher 1981, 596–613, <http://plato.if.usp.br/1-2009/fmt0159n/PDFFiles/ThePhysTeacher_FoundationsOfTheSI.pdf>.
  8. ↑ Wilkins, John An Essay Towards a Real Character, And a Philosophical Language; Gillibrand: London, 1668, <http://www.metricationmatters.com/docs/WilkinsTranslationLong.pdf>.
  9. ↑ Misura Universale, 1675.
  10. ↑ Poynting, John Henry; Thompson, Joseph John A Textbook of Physics: Properties of Matter, 4th ed.; Charles Griffin: London, 1907; p 20, <http://books.google.com/books?id=TL4KAAAAIAAJ&pg=PA20>.
  11. ↑ Jean Charles de Borda; MacTutor, <http://www-history.mcs.st-andrews.ac.uk/Biographies/Borda.html>. (accessed 13 August 2010).
  12. ↑ 12.0 12.1 The International Metre Commission (1870-1872); International Bureau of Weights and Measures, <http://www.bipm.org/en/si/history-si/commission.html>. (accessed 15 August 2010).
  13. ↑ 13.0 13.1 13.2 13.3 13.4 13.5 The BIPM and the evolution of the definition of the metre; International Bureau of Weights and Measures, <http://www.bipm.org/en/si/history-si/evolution_metre.html>. (accessed 15 August 2010).
  14. ↑ Article 3, Metre Convention.
  15. ↑ 15.0 15.1 Barrel, H. The Metre. Contemp. Phys. 1962, 3 (6), 415–34. DOI: 10.1080/00107516208217499.
  16. ↑ 16.0 16.1 The International System of Units (SI), 8th ed.; International Bureau of Weights and Measures: Sèvres, France, 2006; pp 142–43, 148. ISBN 92-822-2213-6, <http://www.bipm.org/utils/common/pdf/si_brochure_8_en.pdf>.
  17. ↑ Phelps, F. M., III Airy Points of a Meter Bar. Am. J. Phys. 1966, 34 (5), 419–22. DOI: 10.1119/1.1973011.
  18. ↑ Michelson, A. A.; Benoît, J.-R. Détermination expérimentale de la valeur du mètre en longueurs d'ondes lumineuses. Trav. Mem. Bur. Int. Poids Mes. 1895, 11 (3), 85.
  19. ↑ Benoit, R.; Fabry, Ch.; Perot, A. Nouvelle détermination du Mètre en longueurs d'ondes lumieuses. C. R. Hebd. Acad. Sci. Paris 1907, 144, 1082–86, <http://gallica.bnf.fr/ark:/12148/bpt6k3098j.image.f1082.langFR>.
  20. ↑ Trans. Int. Union Solar Res. 1907, 2, 28.
  21. ↑ Hollberg, L.; Oates, C. W.; Wilpers, G.; Hoyt, C. W.; Barber, Z. W.; Diddams, S. A.; Oskay, W. H.; Bergquist, J. C. Optical frequency/wavelength references. J. Phys. B: At. Mol. Opt. Phys. 2005, 38, S469–S495. DOI: 10.1088/0953-4075/38/9/003.
  22. ↑ Nobel Prize in Physics 1907 – Presentation Speech; Nobel Foundation, <http://nobelprize.org/nobel_prizes/physics/laureates/1907/press.html>. (accessed 14 August 2010).
  23. ↑ Baird, K. M.; Howlett, L. E. The International Length Standard. Appl. Opt. 1963, 2 (5), 455–63. DOI: 10.1364/AO.2.000455.

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