Here's why:

* Initial Mass Sets the Course: A star's initial mass dictates its core temperature, pressure, and the rate of nuclear fusion. These factors directly influence its lifetime, energy output, and final evolutionary stages.

* Mass Loss is a Result: Stars do lose mass throughout their lives due to stellar winds and, in some cases, planetary nebulae. However, this mass loss is a consequence of the star's initial mass and its evolutionary processes, not the other way around.

* Final Mass is a Consequence: The final mass of a star is determined by how much mass it loses during its lifetime. This is influenced by its initial mass, but doesn't change its fundamental fate.

Think of it like this: Imagine a person starting a journey with a certain amount of fuel in their car. The amount of fuel they start with determines how far they can travel, not how much fuel they have left at the end. The same applies to stars.

Here's a quick breakdown of how initial mass affects a star's fate:

* Low-mass stars: Live long, burn slowly, and eventually become white dwarfs.

* Intermediate-mass stars: Become red giants, then shed their outer layers to form planetary nebulae, leaving behind a white dwarf.

* High-mass stars: Live short, bright lives, become supergiants, explode as supernovae, and leave behind either neutron stars or black holes.

So, while a star's final mass is important in understanding its specific end state, it's the initial mass that ultimately sets the stage for its entire life and death.