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A high mass protostar looks like a star but isn't hot enough to become a star yet. On Earth high mass protostars would be considered a vacuum. They are hard to see because their light is blocked by dust surrounding it.

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A blue main sequence star is a main sequence star of spectral type B and luminosity class V. These stars have from 2 to 16 times the mass of the Sun and surface temperatures between 10,000 and 30,000 K.

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The stars outer layers expand while the core is shrinking, increasing the luminosity. This expansion takes a billion years and the radius increases 100 times. Eventually the core becomes hotter and denser and reaches a temperature of 100million K and the helium nuclei begin to fuse into carbon.

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As the helium in the core is exhausted, the star begins helium burning in a shell around an inert carbon core while moving again up the H-R diagram to become a Red Supergiant.

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High mass stars will develop into a heavy element fusing core, and multiple shell burning outer envelop, releasing large amount of energy.

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Gradually, heavier elements build up to the center which at one point surpasses the mass it can handle. Resulting in the star imploding and  it’s stellar material radiating all over space.

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A neutron star is the collapsed core of a massive star. It is what is left over after a supernova explosion. When a high mass star comes to the end of its lifetime, its outer layers collapse onto the core. This squashes the star's core to the point where the atoms are smashed apart, leaving only neutrons.