KUV 11370+4222 is a ZZ Ceti star discovered in 1996, which has not been observed since then. We performed observations for KUV 11370+4222 in 2010 January. From the Fourier transform spectrum of the light curves, ten independent modes are detected. We searched for the best-fitting model by using the observed periods to match the model periods and get it with the total mass of 0.625 M ⊙ , the effective temperature of 10950 K, and the helium mass fraction and hydrogen mass fraction of 10 −2.2 and 10 −4.0 , respectively. We have found a triplet of frequency split by rotation, which are l = 1 modes. Using the frequency shifts we estimate a rotation period of 5.56 ± 0.08 h. Besides it, another l = 1 mode is identified. The other observed periods are identified as l = 2 modes. At last we investigated the property of the mode trapping.
Abstract. Solar models with moderate enrichment of heavy elements in the convective envelope (CSM) and with element diffusion (DSM) are investigated using updated input physics. It is found that both CSM and DSM can result in adequate depth of the convection zone and appropriate surface helium abundance, and the agreement between the calculated and observed p-mode frequencies are also improved. The sound speed of DSM is better than CSM and the standard solar model (SSM) in the deep interior, which means that element diffusion helps improve the sound speed profile in the solar interior. In the area just below the base of the convection zone, CSM is the best of the three models.
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