Analyzing the Variability of Central Stars in Planetary Nebulae
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Close binary central stars are found at the center of about 10-15% of all planetary nebulae. These close binary systems’ light varies over time, due to different interactions between the two stars. The physical interaction of these close binary stars could have an effect on the shaping of the planetary nebulae around them. Analysis of light variability and spectroscopy of these close binary stars can lead to determining physical characteristics of the stars through modeling of the system, and help to confirm whether or not binary central stars are the cause of the observed structures. Here I focus on the planetary nebula Hartl-Tritton 7 (HaTr 7). Multiple spectra and images have been taken of its central star, confirming that it is a close binary. Computer modeling of the HaTr 7 central binary system is underway with the goal of linking its characteristics to the shape and physical characteristics of the HaTr 7 planetary nebula.
Webb, Andrew C. and Hillwig, Todd, "Analyzing the Variability of Central Stars in Planetary Nebulae" (2015). Fall Interdisciplinary Research Symposium. Paper 34.
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