How long is a cool, dim red dwarf star ($0.1 M_{ ext{odot}}$) calculated to remain fused in hydrogen?

Answer

Trillions of years

Stars at the very low end of the mass spectrum, such as red dwarfs possessing only one-tenth the mass of the Sun ($0.1 M_{ ext{odot}}$), exhibit extremely frugal consumption habits regarding their nuclear fuel. These objects burn their hydrogen reserves incredibly slowly due to their lower core temperatures and pressures, which are sufficient only for a gentle outward pressure against gravity. This slow burn rate results in main-sequence lifetimes that stretch across timescales far exceeding the current age of the universe. Calculations show these frugal stars remain fused in hydrogen for approximately trillions of years, meaning that virtually none of the red dwarfs formed since the universe began have yet neared the end of their hydrogen supply.

$How long is a cool, dim red dwarf star ($0.1 M_{ ext{odot}}$) calculated to remain fused in hydrogen?$

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