Context : Asteroseismology is an efficient tool not only for testing stellar structure and evolutionary theory but also constraining the parameters of stars for which solar-like oscillations are detected , presently .
As an important southern asteroseismic target , \tau Ceti , is a metal-poor star .
The main features of the oscillations and some frequencies of \tau Ceti have been identified .
Many scientists propose to comprehensively observe this star as part of the Stellar Observations Network Group .

Aims : Our goal is to obtain the optimal model and reliable fundamental parameters for the metal-poor star \tau Ceti by combining all non-asteroseismic observations with these seismological data .

Methods : Using the Yale stellar evolution code ( YREC ) , a grid of stellar model candidates that fall within all the error boxes in the HR diagram have been constructed , and both the model frequencies and large- and small- frequency separations are calculated using the Guenther ’ s stellar pulsation code .
The \chi ^ { 2 } _ { \nu c } minimization is performed to identify the optimal modelling parameters that reproduce the observations within their errors .
The frequency corrections of near-surface effects to the calculated frequencies using the empirical law , as proposed by Kjeldsen and coworkers , are applied to the models .

Results : We derive optimal models , corresponding to masses of about 0.775 – 0.785 M _ { \odot } and ages of about 8 – 10 Gyr .
Furthermore , we find that the quantities derived from the non-asteroseismic observations ( effective temperature and luminosity ) acquired spectroscopically are more accurate than those inferred from interferometry for \tau Ceti , because our optimal models are in the error boxes B and C , which are derived from spectroscopy results .

Conclusions :