  Solar magnetic fields are closely related to various physical phenomena on
the sun, which can be extrapolated with different models from photospheric
magnetograms. However, the Open Flux Problem (OFP), the underestimation of the
magnetic field derived from the extrapolated model, is still unsolved. To
minimize the impact of the OFP, we propose three evaluation parameters to
quantitatively evaluate magnetic field models and determine the optimal free
parameters in the models by constraining the coronal magnetic fields (CMFs) and
the interplanetary magnetic fields (IMFs) with real observations. Although the
OFP still exists, we find that magnetic field lines traced from the coronal
models effectively capture the intricate topological configurations observed in
the corona, including streamers and plumes. The OFP is lessened by using the
HMI synoptic map instead of the GONG daily synoptic maps, and the PFSS+PFCS
model instead of the CSSS model. For Carrington Rotation (CR) 2231 at the solar
minimum, we suggest that the optimal parameters for the PFSS+PFCS model are
$R_{\mathrm{ss}} = 2.2-2.5\ R_{\mathrm{sun}}$ and $R_{\mathrm{scs}} =
10.5-14.0\ R_{\mathrm{sun}}$, as well as for the CSSS model are
$R_{\mathrm{cs}} = 2.0 - 2.4\ R_{\mathrm{sun}}$, $R_{\mathrm{ss}} = 11.0 -
14.7\ R_{\mathrm{sun}}$ and $a = 1.0\ R_{\mathrm{sun}}$. Despite the IMFs at 1
AU being consistent with the measurements by artificially increasing the polar
magnetic fields, the IMFs near the sun are still underestimated. The OFP might
be advanced by improving the accuracy of both the weak magnetic fields and
polar magnetic fields, especially considering magnetic activities arising from
interplanetary physical processes.
