Main Sequence Star Flashcards, test questions and answers

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What is Main Sequence Star?

A main sequence star is a type of star that occupies the majority of the stellar population in the Milky Way galaxy. It is characterized by having a hydrogen-fusing core, which gives it its luminosity. Main sequence stars are typically between 0.08 and 100 times the mass of our own Sun, with most stars falling in the middle range of this mass spectrum. The life cycle of any given main sequence star depends on its initial mass and composition at birth. The more massive a star is, the shorter its life cycle will be due to higher energy demands for fusion reactions. A light main sequence star might last for several billion years before becoming a white dwarf or other remnant object, while an ultra-massive main sequence star could burn through all of its fuel within just 10 million years or less. In terms of their internal structure, main sequence stars generally have an outer envelope made up mostly of hydrogen gas and dust particles, along with an inner core where nuclear fusion takes place. As hydrogen atoms fuse together to form helium atoms, they release tremendous amounts of energy that then travels outward from the core towards the star’s surface where it escapes as visible light and other forms radiation. This process allows for a steady supply of energy that can be used by planets orbiting around them to sustain life. As far as our own Solar System goes, all four terrestrial planets orbit around our Sun which is classified as a G-type main sequence star one at the midpoint size range on the mass spectrum mentioned earlier (approximately 1 solar mass). This means that our Sun will continue burning hydrogen fuel in its core for another five billion years or so until eventually expanding into what’s known as a red giant phase and then ultimately cooling down into a white dwarf remnant state after 10 billion years total.