What limits the maximum mass a star can attain?

Answer 1

Well, darling, just like trying to fit into those skinny jeans after a big holiday meal, a star's maximum mass is limited by its ability to support itself against gravity through the balance of inward squeezing pressure and outward radiation pressure. So, when you reach a point where the star can no longer resist collapsing under its own weight, it's game over. It's basically like when you've had one too many cocktails and things start spiraling out of control - not pretty!

Answer 2

The maximum mass a star can attain is limited by the balance between the force of gravity pulling matter inward and the pressure from nuclear fusion pushing matter outward. This balance is known as hydrostatic equilibrium. If a star's mass exceeds this limit, it can lead to a collapse or explosion, depending on the type of star.

Answer 3

Well, let's talk about that, friend. The maximum mass a star can have is determined by a delicate balance between gravity pulling material in and radiation pressure pushing it out. Too much mass means the gravity overwhelms the ability of radiation inside the star to create pressure, causing the star to either collapse under its own weight or experience a dramatic explosion. It's like painting a beautiful picture: every color and brushstroke needs to be just right to create a masterpiece. Isn't nature fascinating?

Answer 4

Oh, dude, like stars are just like high-maintenance divas, you know? So, the thing that stops them from getting too big is basically gravity. Once this gigantic ball of hot mess starts collapsing in on itself, gravity is like, "Whoa, slow your roll, star, you can't get too massive or you'll collapse under your own weight." Then the star's like, "Fine, whatever, I'll just be a regular-sized star then." It's all about that cosmic balance, man.

Answer 5

What limits the maximum mass a star can attain is a delicate balance between the inward pull of gravity and the outward pressure generated by the nuclear fusion reactions happening in the star's core. This balance is governed by the star's structure and composition.

In the core of a star, nuclear fusion reactions convert lighter elements, such as hydrogen, into heavier elements like helium, releasing energy in the process. This energy generates outward pressure that counteracts the force of gravity trying to collapse the star.

The limit on a star's mass is known as the Eddington limit, named after the British astrophysicist Sir Arthur Eddington. This limit is the point at which the outward radiation pressure generated by the star's energy production is equal to the force of gravity pulling inward. Stars that exceed the Eddington limit would experience such intense radiation pressure that it would blow off their outer layers in a powerful stellar wind, effectively limiting their maximum mass.

For stars like our Sun, the mass is not high enough to overcome the force of gravity and reach the Eddington limit. However, massive stars, which have significantly more mass than the Sun, can approach or exceed this limit. Once a star reaches this threshold, it becomes unstable, leading to dramatic events like supernovae or even the collapse into a black hole, depending on the star's initial mass and characteristics.