2010 Student Research Conference:
23rd Annual Student Research Conference

Color Magnitude Diagram of Our Galaxy
Prayash Sharma Pyakurel
Dr. Vayujeet Gokhale, Faculty Mentor

To theoretically generate the color-magnitude diagram we use a stellar evolution algorithm developed by Hurley [Hurley et al (2002)]. An analytically prescribed Initial Mass Function (IMF) is used to simulate a population of stars that represent the original population of stars in a star-birth event. We assume a ratio of 2:1 for the number density of stars in binary star system versus single stars. We also incorporate subsequent star formation by injecting stars into our galaxy by using a prescribed Star Formation Rate (SFR). This composite population of stars is then evolved to present day using Hurleys code, which enables us to represent the color and the magnitude of every star in our galaxy on a Color-Magnitude diagram. One of the objectives of this research is to compare our simulated CMD to the observed CMDs of stellar clusters and the Milky Way Galaxy and interpret the similarities and differences between the two. In particular, we will focus on the relative numbers of white dwarf stars, red giants, main sequence stars etc. in the respective populations.

Keywords: Color Magnitude diagram, Initial Mass Function, Stellar Evolution, Binary Star, Single Stars, Galaxy, Milky Way Galaxy, White Dwarf


Presentation Type: Oral Paper

Session: 33-3
Location: MG 1096
Time: 1:45

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