  Super Li-rich stars form a very small and enigmatic group whose existence
cannot be explained in terms of the standard stellar evolution theory. The goal
of our study is to check the reality of this group of cool giants based on an
independent technique. We have carried out such a check using the K giant HD
77361 (HR 3597), which has previously been assigned to this rare type, as an
example. We have redetermined the effective temperature Teff and surface
gravity log g for this star. We have applied two different methods, photometric
and spectroscopic, to estimate Teff (the accuracy of the Li-abundance
determination depends significantly on this parameter). The value of log g has
been found from the highly accurate parallax of this nearby star. To apply the
photometric method of determining Teff, we have performed UBV observations of
the star, which yielded V = 6.18 +/- 0.03, B - V = 1.13 +/- 0.01, and U - B =
1.18+/-0.05. The following parameters of the star have been found: effective
temperature Teff = 4370+/- 100 K, surface gravity log g = 2.30 +/- 0.10, iron
abundance log e(Fe) = 7.49 +/- 0.14, microturbulence Vt = 1.1 +/- 0.2 km/s,
rotational velocity V sin i = 4.5 km/s, and mass M = 1.3 +/- 0.2 Msun. The
lithium abundance has been determined from a non-LTE analysis of three Li I
lines: the resonance line at 6707.8 ?A and the subordinate lines at 6103.6 and
8126.4 ?A (the latter in a blend with a CN molecular line). We have found a
high lithium abundance, log e(Li) = 3.75 +/- 0.11, which exceeds considerably
the initial abundance log e(Li) = 3.2 +/- 0.1 for young stars in the solar
neighborhood. Thus, we have confirmed that the K giant HD 77361 actually
belongs to the type of super Li-rich stars.
