Type I supernovae and the value of the Hubble constant

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Abstract
An empirical model of the envelopes of Type I supernovae is used to determine the value of H0. An analysis of the composite light and colour curves establishes that near maximum brightness the radius of the photosphere increases linearly with time, over an interval of at least 20 days. This implies a strong density gradient at the photosphere. Calculated profiles of spectral lines formed by scattering in strong density gradients are used to determine the velocity of the photosphere. The derived value of the absolute magnitude at maximum brightness, |${M}_\text{B}=-{20}^\text{m}.25\pm{0}^\text{m}.31$|⁠, combined with the redshift–magnitude relation for Type I supernovae in distant galaxies, gives a value for H0 and an internal rms error of |${H}_{0}-49\pm9$|km/(s Mpc). The most serious possibility of external error is associated with the redshift–magnitude relation, and is such that the best value of H0 would fall in the range 38–49 km/(s Mpc).

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