  The mechanism behind the Long Secondary Period (LSP) observed in pulsating
red giants still remains unknown. In this work, I investigate the connection
between the Red Giant Branch and Asymptotic Giant Branch evolution and the
appearance of the LSP - the phenomenon observed in a large fraction the red
giants. I use the OGLE-III sample of the OSARG variables in the Large
Magellanic Cloud. I construct the density maps in the period-luminosity as well
as color-magnitude planes for the stars showing LSP and compare them to the
remaining giants. I also fit the spectral energy distribution to test whether
an additional source of reddening is present in the LSP stars. I post a
hypothesis that the LSP phenomenon may be related to a transition between the
different pulsation period-luminosity sequences. I also show that an
overabundance of the stars showing Long Period Variables can be observed around
the Tip of the Red Giant Branch, and much more prominently, at the upper part
of the Asymptotic Giant Branch. The main over-density region appears to be
slightly fainter and redder than the bulk of the Asymptotic Giant Branch. It
also seems to correspond to the area of the Hertzsprung-Russell diagram where
stable winds and high mass loss are present. The LSP can possibly be a
recurring phenomenon appearing and disappearing in various points of the red
giant evolution. The LSP stars appear to be more reddened than other giants,
which suggests the intrinsic nature of the reddening, likely related to large
dust emission. The analysis seems to confirms the hypothesis that there is a
relation between the mass loss due to the presence of strong stellar wind and
the appearance of LSP.
