  An exact determination of the Hubble constant remains one of key problems in
cosmology for almost a century. However, its modern values derived by various
methods still disagree from each other by almost 10%; the greater values being
obtained by measurements at the relatively small distances (e.g., by Cepheid
stars as the standard candles), while the smaller values being characteristic
of the methods associated with huge spatial scales (e.g., the analysis of the
cosmic microwave background fluctuations). A reasonable way to resolve this
puzzle is to assume that the Hubble constant is inherently scale-dependent.
This idea seems to be particularly attractive in light of the latest
observational results on the early-type galaxies, where the dark-matter haloes
are almost absent. Therefore, an average contribution of the
irregularly-distributed dark matter to the rate of the cosmological expansion
should be substantially different at various spatial scales. As follows from
the rough estimates, the corresponding variation of the Hubble constant can be
10% and even more, which well explains the spread in its values obtained by the
various methods.
