  The similarity of the absolute luminosity profiles of Type Ia supernovae
(SNIe), as one kind of distance indicator, has led their use in extragalactic
astronomy as secondary standard candles. In general, the empirical relationship
of SNIa on the absolute peak magnitude $M_{\rm B}$ is calibrated by Cepheid
variables in the near distance scale and directly extrapolated to much farther
distances. Two main problems arise. First, their calibration, in particular the
determination of $M_{\rm B}$, depends on the empirical relationship of Cepheid
variables, which suffers from various uncertainties. The second is related to
the homogeneity of SNIa in their true $M_{\rm B}$, which is known to be poor in
different environments. The observed GW signal of the coalescence of compact
binary systems and their electromagnetic counterparts provide the novel and
model-independent way to address these two problems. In the era of
second-generation GW detectors, the low-redshift GW sources provide a novel
method to calibrate the empirical relationship of SNIa, using their
self-calibrated distances. Here, we use the event GW170817 to calibrate the
empirical relationship in different low redshift ranges, and find that the
calibration results are consistent with the ones derived from the Cepheid
variables. Moreover, the uncertainties of $M_{\rm B}$ in both methods are also
comparable. By the observations of third-generation GW detectors, GW sources
can also be used to measure the values of $M_{\rm B}$ for the high-redshift
SNIe, which provides a unique opportunity to study the dependence of $M_{\rm
B}$ on the local environment, strength of gravity, and the intrinsic properties
of the explosion, in addition to test the homogeneity of standard candles. We
find that the uncertainties of $M_{\rm B}$ in both high and low redshifts are
more than one order of magnitude smaller than the current accuracy.
