In most of my videos, I don't present an exhaustive discussion of the topic. My goal is to introduce the topic and the Big Ideas a student might get from a textbook reading, and leave most of the calculations and applications for class time.
Hey Mr. T. Just wanted to pass by and drop a HUGE thank you. I watched all your topic 7s and revised for the other topics with your videos. I had a pretty bad teacher that didn't know much of the content, and would always just look at his notes to explain stuff. Physics just never connected. Then through the final days before the exams some strange Boson helps me find you. I have learned more in 3 days than I have in 2 years with a teacher. You are the reason that I not only passed, but am confident I got a 6, and maybe even a 7, as a final grade, despite getting 3s all 2 years. My gratitude to you and to the effort that you put to know the content very intimately while being intellectually capable of simplifying for us newbies in a way that the subject is still comprehensively covered, is immeasurable. You saved my Paper 3 (I took option D!), taught me topic 7 (making me get a 7 on the paper 2, which had tough topic 7 questions!) and made me genuinely interested in the field. I apologize for the mess of a message this is, but I truly feel a deep gratitude towards you. From the bottom of my heart, thank you.
You are welcome, and I’m so glad you’ve found my videos helpful. I appreciate you taking the time to let me know the videos helped - it makes the effort I put into them feel worthwhile. I’ll be rooting for you when the scores come out in July! (And feel free to pass on the channel to any upcoming IB Physics students. I haven’t made all the new videos for the new 2025 curriculum, but they’ll be coming.)
Why don't heavy stars fuse 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 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.
uhm 15:47 ”The strange quark has a strangeness of -1 and particles containing a single strange quark will also have a strangeness of -1. The anti strange quark has a strangeness of +1 and the particles containing a single anti strange quark will also have a strangeness of +1.“ Oxford physics 2014. I mean it doesn't really tho if it's the other way around since we are conserving it.
Good catch! Sorry about the error. Yeah, it’s not a big deal if it’s conserved in the end (unless someone straight up asks you the value of the strangeness of a particle, and then you’ll differ by a sign).
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❤️
Thanks Mister T, you helped me understand a lot of things, the way you explain everything is so intuitive and entertaining that I didn't even realize when the video was over!
what about the resolution of the measuring device. For example if the uncertainty for time was +-0.2 and the uncertainty for the avg was something else, what do we do about the resolution?
Here’s my favorite painting of Feynman (artist: Sylvia Posner): imageio.forbes.com/blogs-images/startswithabang/files/2017/10/21435816_171362216759692_5085771767054598144_n.jpg?height=501&width=640&fit=bounds
I don’t know who these are intended for, but the fast pace and thorough explanation made it so interesting, I’ll definitely binge watch the rest this weekend! Thank you for this densely informative content
Thanks! They’re aimed at the high school students I teach in IB Physics. I usually ask my students to watch/take notes from these for homework, and then in class we apply the ideas to problems. I’m glad to hear you enjoy them!
Thank you for sharing this excellent video! For clarification, during the proton and electron interaction depicted at 22:00, should the exchange particle mediating the interaction be W+? It looks like this would conserve charge.
