Download Stellar Evolution

yes no Was this document useful for you?
   Thank you for your participation!

* Your assessment is very important for improving the work of artificial intelligence, which forms the content of this project

Document related concepts

Spheromak wikipedia, lookup

Microplasma wikipedia, lookup

Planetary nebula wikipedia, lookup

Nucleosynthesis wikipedia, lookup

Polywell wikipedia, lookup

Hayashi track wikipedia, lookup

P-nuclei wikipedia, lookup

Fusor wikipedia, lookup

White dwarf wikipedia, lookup

Standard solar model wikipedia, lookup

Star formation wikipedia, lookup

Main sequence wikipedia, lookup

Stellar evolution wikipedia, lookup

Stellar Evolution
The whole process takes about 10 millions years.
• If a protostar forms with a mass less than 0.08
solar masses, its internal temperature never
reaches a value high enough for thermonuclear
fusion to begin.
• This failed star is called a brown dwarf, halfway
between a planet (like Jupiter) and a star.
• Brown dwarfs still
emit energy, mostly in
the IR, due to the
potential energy of
collapse converted
into kinetic energy.
• Brown dwarfs
eventual fade and cool
to become black
• The helium ash builds up,
• energy generation stops in the core.
• The fusion process moves outward into a shell
surrounding the hot helium core.
• Helium can also undergo fusion but, since it is a
larger atom, it requires over a 100 million degrees
of temperature.
• For small stars, this temperature is never reached
and the helium core remains inert.