Why don't heavy stars fuze iron even at the net energy loss? Why heavy stars don't overshoot the iron peak? Iron cores have enough gravitational energy to spend on iron fusion but they don't.
Why don't Ni(p,γ)Cu or Ni(α,γ)Zn processes happen in heavy stars during Si burn but before core collapse begins? Assume stellar core has grav-energy to spend.
When I refer to stars with mass greater than or less than 4 solar masses, I am referring to their initial mass, not the mass of the leftover stellar remnant at the end of the star’s life. When the initial mass is less than about 4 solar masses, the stellar remnant (essentially the core) will have a mass less than 1.4 solar masses (the Chandrasekhar limit), and it will be a white dwarf. When the initial mass is greater than 4 solar masses, the stellar remnant will have a mass greater than 1.4 solar masses, and it will be a neutron star or, if the mass is over the O-V limit, a black hole. The Chandrasekhar limit and Oppenheimer-Volkoff limit are relevant to the mass of the stellar remnant, which is different than the initial mass of the star. Sorry for any confusion!
Thank you so much sir, this is really great from you, this comment made a great difference for me as my exams are in 5 days, and you videos are life saving, please do more of them, THANKS ALOT❤️
its crazy how this video doesnt have more views, honestly one of the best explanations of astrophysics across any channel!!!
What are the other astrophysics courses on yt
Thanks! RUclips has mysterious algorithms, so who knows? But I’m glad you found it to be a good explanation!
Mr. T, where were you this entire time????
BEST ASTROPHYSICS VIDEO OUT THERE!!! THANK YOU FOR THIS GONNA SURVIVE P3 TOMORROW!!!
I was hidden under the RUclips search algorithm! I’m glad you found it useful! 😀
And good luck tomorrow!
ahaha man me too i got paper 3 and paper 1
Im so happy I found this right before tomorrow. Thank you!!!!
You’re welcome! Good luck!
THANK YOU SO MUCH!!
thanks so much, learning this asap before thursday 😭😭
Good luck!
me tooooo 😭😭😭
Thank you so much I have my physics HL paper 3 trmw!
You’re welcome! Good luck!
Why don't heavy stars fuze iron even at the net energy loss? Why heavy stars don't overshoot the iron peak? Iron cores have enough gravitational energy to spend on iron fusion but they don't.
Why don't Ni(p,γ)Cu or Ni(α,γ)Zn processes happen in heavy stars during Si burn but before core collapse begins? Assume stellar core has grav-energy to spend.
it should be 1.4 MO not 4 MO
When I refer to stars with mass greater than or less than 4 solar masses, I am referring to their initial mass, not the mass of the leftover stellar remnant at the end of the star’s life.
When the initial mass is less than about 4 solar masses, the stellar remnant (essentially the core) will have a mass less than 1.4 solar masses (the Chandrasekhar limit), and it will be a white dwarf.
When the initial mass is greater than 4 solar masses, the stellar remnant will have a mass greater than 1.4 solar masses, and it will be a neutron star or, if the mass is over the O-V limit, a black hole.
The Chandrasekhar limit and Oppenheimer-Volkoff limit are relevant to the mass of the stellar remnant, which is different than the initial mass of the star.
Sorry for any confusion!
Thank you so much sir, this is really great from you, this comment made a great difference for me as my exams are in 5 days, and you videos are life saving, please do more of them, THANKS ALOT❤️