Loading presentation...

Present Remotely

Send the link below via email or IM

Copy

Present to your audience

Start remote presentation

  • Invited audience members will follow you as you navigate and present
  • People invited to a presentation do not need a Prezi account
  • This link expires 10 minutes after you close the presentation
  • A maximum of 30 users can follow your presentation
  • Learn more about this feature in our knowledge base article

Do you really want to delete this prezi?

Neither you, nor the coeditors you shared it with will be able to recover it again.

DeleteCancel

Stellar Evolution

No description
by

Emily McGrath

on 16 January 2014

Comments (0)

Please log in to add your comment.

Report abuse

Transcript of Stellar Evolution

Stellar Evolution
Ch. 29 sec. 3

Star Formation
Next, the cloud contracts and takes on the shape of a disk. At the center is hot, condensed object called a
protostar
.
Star Formation
As the temperature inside the protostar increase, it eventually gets hot enough for nuclear fusion to begin.
Life Cycle
Life Cycle
Supernova formation:
Core is too massive to be supported by electron pressure
Once Fe is created, no further reactions can take place & star violently collapses on itself
Eventually, the core stops collapsing and becomes a collapsed star remnant, or
neutron star
.
Life Cycle
Some neutron stars pulsating patterns of light, this type of star is called a
pulsar
.

A massive explose occurs as material & gas fall in on the neutron star and strike the hard surface. The entire outer portion of the star is blown off in this
supernova
.

If the core of a star continues to collapse, a small extremely dense object that remains is a
black hole
.
First, a cloud of interstellar gas & dust, called a
nebula
, collapses on itself as a result of its own gravity.
Star Formation
Full transcript