  The formation of extremely hot outer atmospheres is one of the most prominent
manifestations of magnetic activity common to the late-type dwarf stars,
including the Sun. It is widely believed that these atmospheric layers, the
corona, transition region, and chromosphere, are heated by the dissipation of
energy transported upwards from the stellar surface by the magnetic field. This
is signified by the spectral line fluxes at various wavelengths, scaled with
power-law relationships against the surface magnetic flux over a wide range of
formation temperatures, which are universal to the Sun and Sun-like stars of
different ages and activity levels. This study describes a catalog of power-law
indices between solar activity proxies and various spectral line fluxes.
Compared to previous studies, we expanded the number of proxies, which now
includes the total magnetic flux, total sunspot number, total sunspot area, and
the F10.7 cm radio flux, and further enhances the number of spectral lines by a
factor of two. This provides the data to study in detail the flux-flux scaling
laws from the regions specified by the temperatures of the corona
(log(T/K)=6-7) to those of the chromosphere (log(T/K)~4), as well as the
reconstruction of various spectral line fluxes of the Sun in the past, F-, G-,
and K-type dwarfs, and the modeled stars.
