5 Conclusion

As stated above, we made period analyses for three data sets: Li and Jiang's data set, our data set and the combined data set. The main results obtained are given in three tables and three figures. A coherent solution of two frequencies: 11.3484 and 6.9840 cd^-1 was obtained. We used the stellar structure and evolution code developed by Luo (1991, 1997) and Li's program (1990, 1994) to calculate the evolution sequences of a star with 1.0-2.0 solar mass and all pulsation frequencies of each evolution phase. we found two frequencies: 11.3357 cd^-1 (radial

p mode, l=0, n=4) and 7.0235 cd^-1 (nonradial p mode, l=1, n=1) in the 140th evolution phase of the evolution sequence of a star with 1.9 solar mass. These two calculated frequencies were the same values as the observed frequencies within the errors. So, we tend to suggest that HR 5437 pulsates in the two modes: radial p mode with l=0, n=4 and nonradial p mode with l=1, n=1. Furthermore, from the known parameters: $M_{\rm bol}=1.25$ mag and $T_{\rm eff}=7900$ K we obtained $\log L/L_{\hbox{$\odot$}}=1.4$ and $\log T_{\rm eff}=3.9$. These two parameters are consistent with the calculated values in the 140th evolution phase of the evolution sequence of a star with 1.9 solar mass. It means that the mode identification is reliable.

Acknowledgements

The authors would like to express their thanks to the National Natural Science Foundation of China for the research grants.