  Searching in the MaNGA IFU survey, I identify 9 galaxies that have strong
Balmer absorption lines and weak nebular emission lines measured from the
spectra integrated over the entire IFUs. The spectral features measured from
the bulk of the stellar light make these galaxies local analogs of
high-redshift spectroscopically-selected post-starburst galaxies, thus, proxies
to understand the mechanisms producing post-starburst galaxies at
high-redshifts. I present the distributions of absorption-line indices and
emission-line strengths, as well as stellar kinematics of these local
post-starburst galaxies. Almost all local post-starburst galaxies have central
compact emission-line regions at the central $<1$ kpc, mostly powered by weak
star-formation activities. The age-sensitive absorption line indices
EW(H$\delta$) and Dn4000 indicate that the stellar populations at the outskirts
are older. Toy stellar population synthesis models suggest that the entire
galaxies are experiencing a rapid decline of star formation with residual
star-formation activities at the centers. These features demand that most
post-starburst galaxies are the aftermath of highly dissipative processes that
drive gas into centers, invoke centrally-concentrated star formation, then
quench the galaxies. Meanwhiles, when measurable, post-starburst galaxies have
the directions of maximum stellar velocity gradients align with photometric
major axes, which suggest against major mergers being the principal driving
mechanism, while gas-rich minor mergers are plausible. While directly obtaining
the same quality of spatially-resolved spectra of high-redshift post-starburst
galaxies is very difficult, finding proper local counterparts provides an
alternative to understand quenching processes in the distant Universe.
