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In this work we suggest a very simple, approximate formalism for descriptionof some basic (especially thermodynamical) characteristics of a rotating, verythin black ring. (In fact, our formalism is not theoretically dubious, since,at it is not hard to see, it can correspond to an extreme simplification of amore accurate, Copeland-Lahiri string formalism for the black holedescription.) Even if suggested formalism is, generally speaking,phenomenological and rough, obtained final results, unexpectedly, arenon-trivial. Concretely, given formalism reproduces exactly Bekenstein-Hawkingentropy, Bekenstein quantization of the entropy or horizon area and Hawkingtemperature of a rotating, very thin black ring obtained earlier using moreaccurate analysis by Reall, Emparan, Elvang, Virmani etc. (Conceptually it issimilar to situation in Bohr's atomic model where energy levels are determinedpractically exactly even if electron motion is described roughly.) Ourformalism, according to suggestions in our previous works, is physically basedon the assumption that circumference of the horizon tube holds the natural(integer) number of corresponding reduced Compton's wave length. (It isconceptually similar to Bohr's quantization postulate in Bohr's atomic modelinterpreted by de Broglie relation.) Also, we use, mathematically, practicallyonly simple algebraic equations (by determination of Hawking temperature we useadditionally only simple differentiation of Smarr relation).

A Simple Determination of the Thermodynamical Characteristics of a Very Thin Black Ring