A new method of light curve inversion with bipartite regularization (LIBR), which is complementary to the previous treatments by Bonomo and Lanza and Estrela and Valio, is used to reconstruct the physical properties of star spots on the solar-type star Kepler-17 by using the full Q1- Q17 data set. The Markov Chain Monte Carlo (MCMC) method was applied to find the best profile of the reconstructed surface. The known value of the rotation inclination of Kepler-17 allows the generation of a star spot model in a sequence of stellar rotation with a period of 12.26 d. Because of the nature of the light curve inversion, the spot model is limited to the equatorial region. We also investigated the starspot lifetimes of Kepler-17 utilizing the MCMC method. Combined with the LIBR inversion results, it was found that the star spots typically last from one to several stellar rotations. From the time evolution of the spot size, a magnetic cycle period of 437 d can be derived. This value is comparatively shorter than the solar cycle which might be a consequence of the younger age (∼ 1.78 Gyr) of Kepler-17. The light curve of Kepler-17 is characterized by the presence of large-amplitude variation caused by star spots but no superflare activity. An interesting possibility is that the magnetic energy stored in the star spot regions could have been constantly dissipated by electrodynamic interaction between the central star and the hot Jupiter, Kepler-17b, via a lower-level energy release process.

一种新的具有二分正则化（LIBR）的光变曲线反演方法，是对 Bonomo 和 Lanza 以及 Estrela 和 Valio 先前处理的补充，用于重建太阳型恒星 Kepler-17 上星斑的物理性质：使用完整的 Q1-Q17 数据集。马尔可夫链蒙特卡罗（MCMC）方法被用来寻找重建表面的最佳轮廓。Kepler-17 的自转倾角的已知值允许在周期为 12.26 d 的恒星自转序列中生成星斑模型。由于光变曲线倒置的性质，光斑模型仅限于赤道地区。我们还利用 MCMC 方法研究了 Kepler-17 的星斑寿命。结合LIBR反演结果，人们发现，这些星点通常会持续一到几个恒星自转。从光斑尺寸的时间演化可以推导出一个437 d的磁循环周期。这个值比太阳周期短，这可能是 Kepler-17 年龄较小（~ 1.78 Gyr）的结果。Kepler-17的光变曲线的特点是存在由星斑引起的大幅度变化，但没有超耀斑活动。一个有趣的可能性是，存储在星斑区域的磁能可能会通过中央恒星和热木星 Kepler-17b 之间的电动相互作用通过较低水平的能量释放过程不断消散。这个值比太阳周期短，这可能是 Kepler-17 年龄较小（~ 1.78 Gyr）的结果。Kepler-17的光变曲线的特点是存在由星斑引起的大幅度变化，但没有超耀斑活动。一个有趣的可能性是，存储在星斑区域的磁能可能会通过中央恒星和热木星 Kepler-17b 之间的电动相互作用通过较低水平的能量释放过程不断消散。这个值比太阳周期短，这可能是 Kepler-17 年龄较小（~ 1.78 Gyr）的结果。Kepler-17的光变曲线的特点是存在由星斑引起的大幅度变化，但没有超耀斑活动。一个有趣的可能性是，存储在星斑区域的磁能可能会通过中央恒星和热木星 Kepler-17b 之间的电动相互作用通过较低水平的能量释放过程不断消散。