questions... are there any electrons in orbitals in a stellar core? The atoms should be fully ionized at those temperatures so it's more about the energy states of the free electrons and the Maxwellian velocity distribution vs what's allowed by Pauli at a given density/temperature, eh? Raise the temp and that will ease the level of degeneracy in the core because there are now more energy states permitted by Pauli (which is why higher mass stars don't develop degenerate cores and then undergo a helium flash when helium burning commences).
Yeah, the electrons should be in a Fermi gas, not bound to atoms. I think that this is a decent 'no math' way to explain it, but without the luxury of mathematical rigor it would be really hard to explain that uncertainty principle stuff.
Professor, What a fantastic video! Do you have any insight into how much pressure an electron can handle before it fuses with a proton to form a neutron and an electron neutrino? It must be an astronomical number! Thanks! 🌟
Thank you. It is a matter of kinetic energy and speed. Since a neutron has more mass than a proton, the electron would need enough speed in order for the mass to be generated.
@@MichelvanBiezen Professor, Your amazing response is extremely insightful! It’s interesting how massive stars can give us a glimpse of the nature of fundamental particles like electrons gaining kinetic energy and increasing relativistic mass. The additional 2.5 MeV/c^2 required to transition from an up quark to a down quark equates to 4.89 me or electron rest masses! I’m guessing the electron would be gaining energy as it increased orbital\valence levels. Calculating the wavelength\orbital level\kinetic energy required to increase an electrons mass by a multiple of 5 would give you a sense of both the properties of an electron as well as a neutron star. Thank you! ✨
Great input. As a last thought. For electrons to gain this amount of energy, they would have to be free from the confines of an atom and must move at speeds of almost 99.9% of the speed of light.
what is the effect of electron degeneracy and hyper density on the energy level of electrons? I mean even small gravity pressures on electron energy levels must have consequences. what is happening at that time?
If you had a solar mass just under 1.4 and rotational relativistic speed that put portions of the mass above the 1.4 needed for black hole formation would Hawking radiation be detected? Great video.thanks
2:40 If electron orbital decrease by 1 % then why it's nucleus attract it because or opposite charge of protons respect to electron , any why you saying it is repailed by electron , if orbit decrease it face struggle with protons so why enetron , you said ???
You misunderstood. It is the distance between nuclei in different atoms which decreases, not the electron orbital. This distance doesn't decrease by 1% (which would be a small change: 100 to 99 is a decrease of 1%); the new distance is only 1% of the old distance (which is a huge change: 100 to 1 results in a new number which is 1% of the old number). The fact that the nuclei are pressed much closer together than normal causes the orbitals to twist. But it is not the nucleus that is repelled by the electron; it is the electrons which repel each other. (They are all negatively charged). Degeneracy pressure prevents the white dwarf from becoming more dense; it cannot collapse further (as long as the mass of the white dwarf is below the chandrasekhar limit; otherwise gravity will win. Then it is neutron degeneracy pressure which will either support a neutron star or play a role in a supernova).
I thought white dwarfs werent able to become nova because they usually occur after a red giant process, which wasnt powerful enough to become nova. Can someone explain.
PureShores The is a difference between a nova and a supernova A nova occurs when enough mass from another star in a binary star system is pulled onto a white dwarf and begins to fuse on the surface under enormous pressure and temperature A super nova occurs (of the type 1A) when a white dwarf gains enough mass from another star to exceed the chandrasakhar limit which is equal to 1.4 times the mass of the Sun
Oh ok. So is a white dwarf always involved in the nuclear process of a supernova?. or does it only nitch off a red giant star when it get ps involved in a binary system and gains density, approaching the C-limit.?. Im aware of the fact that a giant star over 8 solar masses will become a neutron star and or black hole. These nuclear processes are completeley different than those of a white dwarf right? Sorry for the confusion, thanks for the replies.
PureShores You are correct Keep in mind that the vast portion of all white dwarfs, simply remain white dwarfs and slowly cool over billions and billions of years. It is a rare white dwarf that is involved in a nova or super nova event. The very large stars do not become white dwarfs, but instead continue to fuse heavier and heavier elements in their cores until iron is fused, after that they explode as a type 2 super nova
Thats amazing. I also wanted to ask, after electron degeneracy, is it possible for there to be neutron degeneracy after the graviational collapse keeps getting stronger?. Isnt that how neutron stars get their names?. By the collapse of protons and electrons from such powerful grav forces, leaving just neutrons?. Does this happen in a white dwarf phase that approaches or goes past 1.4 solar masses? Or does it just go s(nova). Thanks for the replies professor.
Yep. At a certain point, it becomes energetically favourable for Protons to capture free electrons. As white dwarfs approach the Chandrashekar Limit they undergo sudden Carbon burning. Because the star is degenerate it doesn't have a safefy value... ie it can't expand thus reducing it's temp (and thus the rate of fusion), so a large percentage of the core fuses in a very short period of time (degenerate matter is an excellent conductor of heat, IIRC) and this results in the star being blown apart as a Type IA supernova.
This is the clearest explanation I think I have ever seen. Finally answered some questions I have been asking for a while now. Thank you.
Kaeben I’ve been looking for about an hour for a video like this, did not think it would be this hard.
questions... are there any electrons in orbitals in a stellar core? The atoms should be fully ionized at those temperatures so it's more about the energy states of the free electrons and the Maxwellian velocity distribution vs what's allowed by Pauli at a given density/temperature, eh? Raise the temp and that will ease the level of degeneracy in the core because there are now more energy states permitted by Pauli (which is why higher mass stars don't develop degenerate cores and then undergo a helium flash when helium burning commences).
Yeah, the electrons should be in a Fermi gas, not bound to atoms. I think that this is a decent 'no math' way to explain it, but without the luxury of mathematical rigor it would be really hard to explain that uncertainty principle stuff.
Now I understand how white dwarf sustain without thermo nuclear fusion, Thanks for making this video👍
Now this is the stuff that really interests me.
Professor, What a fantastic video! Do you have any insight into how much pressure an electron can handle before it fuses with a proton to form a neutron and an electron neutrino? It must be an astronomical number! Thanks! 🌟
Thank you. It is a matter of kinetic energy and speed. Since a neutron has more mass than a proton, the electron would need enough speed in order for the mass to be generated.
@@MichelvanBiezen Professor,
Your amazing response is extremely insightful! It’s interesting how massive stars can give us a glimpse of the nature of fundamental particles like electrons gaining kinetic energy and increasing relativistic mass. The additional 2.5 MeV/c^2 required to transition from an up quark to a down quark equates to 4.89 me or electron rest masses! I’m guessing the electron would be gaining energy as it increased orbital\valence levels. Calculating the wavelength\orbital level\kinetic energy required to increase an electrons mass by a multiple of 5 would give you a sense of both the properties of an electron as well as a neutron star.
Thank you! ✨
Great input. As a last thought. For electrons to gain this amount of energy, they would have to be free from the confines of an atom and must move at speeds of almost 99.9% of the speed of light.
thankyou, been asking myself this lots of times and only seen so perfectly explained right now!
You're very welcome!
So.. How does one calculate at what pressure the electron degeneracy density limit is reached for a given element?
what is the effect of electron degeneracy and hyper density on the energy level of electrons? I mean even small gravity pressures on electron energy levels must have consequences. what is happening at that time?
Who could dislike this? It's fascinating. No wonder the thumbs down is in the minority.
Awesome series. Thanks much.
Such a nice explanation for a layman like me, thank you!
You're very welcome!
Excellent lecture, thank you so much!
Glad you liked it. Thank you for your comment. 🙂
Brilliant video, thanks!
watching these videos while high makes me so much immerse, it's almost like i could Undestand every sentence of his :)
Haha. Thinking about the cosmos is the best thing to do when you're baked.
Great video, very helpful!
If you had a solar mass just under 1.4 and rotational relativistic speed that put portions of the mass above the 1.4 needed for black hole formation would Hawking radiation be detected? Great video.thanks
Hawking radiation is a quantum mechanic effect and would probably not be detected in any circumstance.
2:40 If electron orbital decrease by 1 % then why it's nucleus attract it because or opposite charge of protons respect to electron , any why you saying it is repailed by electron , if orbit decrease it face struggle with protons so why enetron , you said ???
You misunderstood. It is the distance between nuclei in different atoms which decreases, not the electron orbital. This distance doesn't decrease by 1% (which would be a small change: 100 to 99 is a decrease of 1%); the new distance is only 1% of the old distance (which is a huge change: 100 to 1 results in a new number which is 1% of the old number). The fact that the nuclei are pressed much closer together than normal causes the orbitals to twist. But it is not the nucleus that is repelled by the electron; it is the electrons which repel each other. (They are all negatively charged). Degeneracy pressure prevents the white dwarf from becoming more dense; it cannot collapse further (as long as the mass of the white dwarf is below the chandrasekhar limit; otherwise gravity will win. Then it is neutron degeneracy pressure which will either support a neutron star or play a role in a supernova).
You are amazing. Thank you!
great video
I thought white dwarfs werent able to become nova because they usually occur after a red giant process, which wasnt powerful enough to become nova. Can someone explain.
PureShores The is a difference between a nova and a supernova
A nova occurs when enough mass from another star in a binary star system is pulled onto a white dwarf and begins to fuse on the surface under enormous pressure and temperature
A super nova occurs (of the type 1A) when a white dwarf gains enough mass from another star to exceed the chandrasakhar limit which is equal to 1.4 times the mass of the Sun
Oh ok. So is a white dwarf always involved in the nuclear process of a supernova?. or does it only nitch off a red giant star when it get ps involved in a binary system and gains density, approaching the C-limit.?. Im aware of the fact that a giant star over 8 solar masses will become a neutron star and or black hole. These nuclear processes are completeley different than those of a white dwarf right? Sorry for the confusion, thanks for the replies.
PureShores You are correct
Keep in mind that the vast portion of all white dwarfs, simply remain white dwarfs and slowly cool over billions and billions of years. It is a rare white dwarf that is involved in a nova or super nova event.
The very large stars do not become white dwarfs, but instead continue to fuse heavier and heavier elements in their cores until iron is fused, after that they explode as a type 2 super nova
Thats amazing. I also wanted to ask, after electron degeneracy, is it possible for there to be neutron degeneracy after the graviational collapse keeps getting stronger?. Isnt that how neutron stars get their names?. By the collapse of protons and electrons from such powerful grav forces, leaving just neutrons?. Does this happen in a white dwarf phase that approaches or goes past 1.4 solar masses? Or does it just go s(nova). Thanks for the replies professor.
Yep. At a certain point, it becomes energetically favourable for Protons to capture free electrons.
As white dwarfs approach the Chandrashekar Limit they undergo sudden Carbon burning. Because the star is degenerate it doesn't have a safefy value... ie it can't expand thus reducing it's temp (and thus the rate of fusion), so a large percentage of the core fuses in a very short period of time (degenerate matter is an excellent conductor of heat, IIRC) and this results in the star being blown apart as a Type IA supernova.
Great. Lecture sir
May I know electron capture it is same like electron degeneracy?
Please do a video on Democrat degeneracy.
LOL
Why did I watch this when I am in 8 th grade😓😓😓