This describes the majority of stars in the Universe (by number).
A purely helium composition is the fate of all M-class (red dwarf) stars, below about 40% the Sun's mass.
These fates are determines solely by the star's mass, which in turn determines the maximum temperature that will be reached in the core. Once that mass/temperature threshold is crossed, the star begins fusing hydrogen into helium, and will encounter one of three different fates. Even the stars, the most enormous collections that transform nuclear fuel in the cosmos, will someday all burn out, including our Sun. With gravitational, electromagnetic and nuclear forces all acting on matter, practically everything we observe to exist today will face changes in the future. One of the most profound rules in all the Universe is that nothing lasts forever. Our Sun has about another 5-7 billion years of fusing hydrogen into helium, but there's much more to come after that. E=mc^2, when you think about it, showcases how energetic this is, as the mass of Saturn multiplied by the speed of light (a large constant) squared leads to a tremendous amount of energy produced. System, is dwarfed in terms of 'mass loss' by nuclear fusion, which has reduced the Sun's mass by a total of 0.03% of its starting value: a loss equivalent to the mass of Saturn. A solar flare from our Sun, which ejects matter out away from our parent star and into the Solar.