A NEW METHOD FOR THE DETERMINATION OF THE HUBBLE PARAMETER

By chance, the slope of the M(v)(max) versus (B - V)(max) relation for recent theoretical models of Type Ia supernovae (SNe Ia) by Hoflich & Khokhlov is indistinguishable from the slope of a reddening line in t he V versus B - V plane. This coincidence allows one to determine a pa rameter M(v)(max) for SNe Ia that is independent of both supernova de tonation model and interstellar reddening. Calibrating M(v)(max) with observations of SNe Ia by Hamuy and coworkers yields values of the Hu bble parameter H-0 in the range 55-60 km s(-1) Mpc(-1). The discrepanc y between this result and values of Ho recently obtained from observat ions of Cepheids in the Virgo Cluster suggests that either (1) the Cep heid distance scale is wrong, (2) the SN Ia models of Hoflich & Khokhl ov are too bright by similar to 0.75 mag near maximum light, or (3) th eir models are too red by similar to 0.25 mag in B - V.