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We have analysed oscillations of the red giant star HD 186355 observed by theNASA Kepler satellite. The data consist of the first five quarters of scienceoperations of Kepler, which cover about 13 months. The high-precisiontime-series data allow us to accurately extract the oscillation frequenciesfrom the power spectrum. We find the frequency of the maximum oscillationpower, {\nu}_max, and the mean large frequency separation, {\Delta}{\nu}, arearound 106 and 9.4 {\mu}Hz respectively. A regular pattern of radial andnon-radial oscillation modes is identified by stacking the power spectra in anechelle diagram. We use the scaling relations of {\Delta}{\nu} and {\nu}_max toestimate the preliminary asteroseismic mass, which is confirmed with themodelling result (M = 1.45 \pm 0.05 M_sun) using the Yale Rotating stellarEvolution Code (YREC7). In addition, we constrain the effective temperature,luminosity and radius from comparisons between observational constraints andmodels. A number of mixed l = 1 modes are also detected and taken into accountin our model comparisons. We find a mean observational period spacing for thesemixed modes of about 58 s, suggesting that this red giant branch star is in theshell hydrogen-burning phase.

Modeling Kepler Observations of Solar-like Oscillations in the Red-giant Star HD 186355