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I fused observed spectra from the white-dwarf star G191-B2B to constrain the spatial and temporal variation of the fine-structure constant, α = e 2 4 π ε 0 ℏ c . The analysis was combined with laboratory-measured and astronomically observed lines in Ni V to find Δ α / α = ( − 0.003 ± 0.072 ) × 10 − 6 . The obtained result allows a symmetry of the related comparison with previous studies looking for cosmological variations of α using spectra from Quasi Stellar Objects (QSOs). In this way, we can expect higher sensitivity from white-dwarf spectra than QSO spectra. Therefore, this study should have orders-of-magnitude higher sensitivity per system than previous quasar studies, and we should reduce statistical and systematic errors. The results of this study place a more stringent limit on Δ α / α than previous studies using the same data.
T. D. Le (Thu,) studied this question.