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Fine-structure constant
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=== Present rate of change === In 2008, Rosenband ''et al.''<ref> {{cite journal |last1=Rosenband |first1=T. |last2=Hume |first2=D. B. |last3=Schmidt |first3=P. O. |last4=Chou |first4=C. W. |last5=Brusch |first5=A. |last6=Lorini |first6=L. |last7=Oskay |first7=W. H. |last8=Drullinger |first8=R. E. |last9=Fortier |first9=T. M. |last10=Stalnaker |first10=J. E. |last11=Diddams |first11=S. A. |last12=Swann |first12=W. C. |last13=Newbury |first13=N. R. |last14=Itano |first14=W. M. |last15=Wineland |first15=D. J. |last16=Bergquist |first16=J. C. |display-authors=6 |date=28 March 2008 |title=Frequency ratio of Al{{sup|+}} and Hg{{sup|+}} single-ion optical clocks; metrology at the 17th decimal place |journal=Science |volume=319 |issue=5871 |pages=1808–1812 |doi=10.1126/science.1154622 |pmid=18323415 |bibcode=2008Sci...319.1808R |s2cid=206511320 |url=https://zenodo.org/record/1230892 |doi-access=free}}</ref> used the frequency ratio of {{chem2|Al+}} and {{chem2|Hg+}} in single-ion optical atomic clocks to place a very stringent constraint on the present-time temporal variation of {{mvar|α}}, namely {{sfrac| {{math|Δ}}{{mvar|α}} | {{mvar|α}} }} = {{val|-1.6|2.3|e=-17}} per year. A present day null constraint on the time variation of alpha does not necessarily rule out time variation in the past. Indeed, some theories<ref> {{cite journal |last1=Barrow |first1=John D. |last2=Sandvik |first2=Håvard Bunes |last3=Magueijo |first3=João |date=21 February 2002 |title=Behavior of varying-alpha cosmologies |journal=[[Physical Review D]] |volume=65 |issue=6 |pages=063504 |doi=10.1103/PhysRevD.65.063504 |arxiv=astro-ph/0109414 |bibcode=2002PhRvD..65f3504B |s2cid=118077783 }}</ref> that predict a variable fine-structure constant also predict that the value of the fine-structure constant should become practically fixed in its value once the universe enters its current [[dark energy]]-dominated epoch.
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