Sometimes this white dwarf starts revollving itself with another main sequence star. This is called binary system. The white dwarf starts to pull energy from the main sequence star, and something (electron degeneracy ressure is defeated by gravity) happens and then the white dwarf collapses. This is called Type 1 A supernova.

After white dwarf

..., the only thing fusing is the outskirts of the core. Now these hydrogen particles are like "We don't have any core to stick to, where do we go?". So they start repelling each other. Now, as we know, fusion gives radiation. As the star starts to cool down (as more of its mass gets fused), it starts to get bigger because the radiation from the fusion is pushing the outer particles of this star outwards. The outer layer of this star starts radiating outwards because the gravity of this star can't hold it anymore. This colorful outer layer is planetary nebulae. This phase is called red giant.

After the core get fused

So n high mass stars, after the red giant phase, there is still a hell of a helium to burn. So, this helium slowly fuses to carbon, carbon to something and on and on and on untill (!) you reach Iron. Because iron is very hard to fuse. So here the core, gets done. Now, as there is no radiation pushing outwards. This core (only the coree, not the star) collapses itself into itself. Because there was just gravity pulling it. Creating shock waves with such high energy that they fore iron to fuse into platinum/silver/gold. Some supernova threw gold to our earth.

High mass stars

As the core is completely fused, it becomes trapped. Its outer layers are gone. This lonely core is called the white dwarf. For a low mass star, this is where you die. The helium particles in this star just radiate outwards slowly and slowly. After some time, they have no power to radiate. This is when it is called the brown dwarf. In astrophysics, brown means no light and white means all colors. Hence, after all of this losing of power it dies. It's pretty sad. :(

The white dwarf

Protons and eletrons start to form a cloud of hydrogen. This cloud has LOADS of mass and are GIGANTIC. Due to gravity, the atoms around it get attracted to the cloud too. But there is a repulsion between atoms which gets them not into each other. These atoms of hydrogen get attracted to each other hardly due to gravity. These atoms start getting crushed. And then nuclear fusion takes place. 4 hydrogen atoms get together to make 1 helium atom(helium was not like you can take it from anywhere, it had to be created through nuclear fusion).

<ul><li>Our sun will last 10 billion years but a star 10 times bigger than our sun will last 20 million years only.</li></ul>This is because the larger the star, the higher the gravity, the higher the amount of hydrogen to be burnt, the faster you burn, the faster you die. This shows how much important the mass of star is to affect its lifespan.

Fun fact

.., The star can get collapsed into a neutron star. This is the most dense star in the universe. And they rotate very fast (due to conservation of angular momentum). Here the gravity is so immense that nearly 90% of the star's electrons get fused into neutrons. A neutron star of a size of the city of Manhattan can be 2x heavier than our sun.

After collapse

Jeans mass- this is the minimum mass required for a gas cloud to collapse into a star.In middle of being a gas cloud and being a star, there is a protostar phase. Here the star is not really a star but there is some gas that has been concentrated. Lots of things can happen in this phase.<ol><li>More of mass can be attracted to this protostar and form this star even bigger.</li><li>Not more mass is attracted and the outermost layer of this cloud cools down. Cools down into rocks. Rocks that we now live on.</li></ol>

3. As the fusion takes place, the radiation radiating outwards from the fusion takes the particles with it off the gas cloud and the star may never form. Because the radiation is in the oposite direction of the gravitational pull to collapse. When both are equal, it's called equillibrium.

Today we bring back a topic that we haven't spoken about in a long time, astronomy. We dive into the different phases of a star and the different possibilities that are presented once we start to analyze their masses. Enjoy the episode.     Instagram: @math.physics.podcast  Tiktok: @math.physics.podcast  Email: math.physics.podcast@gmail.com  Twitter: @MathPhysPod      HelloFresh:  Link: https://hellofresh-ca.o5kg.net/c/2544961/791027/7893  Code: HFAFF80  Offer: $80 Discount ($50 - $20 - $10) Including Free Shipping on First Box!

scienceandnature

Science & Nature

Today we bring back a topic that we haven't spoken about in a long time, astronomy. We dive into the different phases of a star and the different possibilities that are presented once we start to analyze their masses. Enjoy the episode.   Instagram: @math.physics.podcast Tiktok: @math.physics.podcast Email: math.physics.podcast@gmail.com Twitter: @MathPhysPod    HelloFresh: Link: https://hellofresh-ca.o5kg.net/c/2544961/791027/7893 Code: HFAFF80 Offer: $80 Discount ($50 - $20 - $10) Including Free Shipping on First Box!

Two University of Toronto students in the math and physics program discuss interesting topics in the field.

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