08:09:27	 From Sean Kelly 🌟 : My family loved visiting the McDonald Observatory for a star party a couple of summers ago. Such beautiful dark skies!
08:16:35	 From Sean Kelly 🌟 : Love that HR diagram animation. Can I use it?
08:17:29	 From Nicole Preiser : I agree. How can we get a copy?
08:17:40	 From Matteo Cantiello : I’m pretty sure you can, Sean+Nicole. We’ll ask Mike to share after his talk!
08:17:49	 From Nicole Preiser : thanks
08:17:53	 From Mark Zagaeski : Excellent!
08:17:58	 From Charlie Payne : Thank you!
08:18:04	 From Sean Kelly 🌟 : Awesom!
08:18:09	 From Sean Kelly 🌟 : Awesome!
08:18:20	 From JJ Hermes (Boston University) : I’m not sure about that specific diagram but there’s one from HST that is even prettier in my opinion: https://hubblesite.org/video/35/science/129-features
08:18:34	 From Matteo Cantiello : +1
08:18:39	 From Maggie Sherriffs (she/her/hers) : also, as usual, video recordings of all talks (and accompanying slides) will be at online.kitp.ucsb.edu by Monday (ok probably w/in hours)
08:19:33	 From Gabriel Garcia : I have a bit of a question. How do we know the mass of the stars? Is it just as Michael said where mass is just compared over time? or is there a way to compare to other stars?
08:19:34	 From Marc Afifi Pacific Grove HS : 👍
08:20:24	 From Sean Kelly 🌟 : @Gabriel The surface temperature of the star is a good way to establish the mass
08:20:37	 From Gabriel Garcia : Thank you!
08:23:36	 From Sean Kelly 🌟 : How does the C/O ratio change with mass?
08:25:22	 From Sean Kelly 🌟 : Does the ideal gas law apply as well to Plasma?
08:26:00	 From Jared Goldberg (UCSB; he/him) : Ideal gas law is great for plasma!
08:26:22	 From Sean Kelly 🌟 : What about the electric interaction?
08:27:29	 From Jared Goldberg (UCSB; he/him) : Not all plasma, but in stars the ideal gas law does describe the gas interactions. They’re hot and sparse enough that electric interaction mostly serves to keep the collisions elastic (kind of like magnets and carts on a track)
08:29:44	 From Sean Kelly 🌟 : @Jared Thanks!
08:33:49	 From Sean Kelly 🌟 : What is the time for a white dwarf to cool down to 2.7 K?
08:34:54	 From Jared Goldberg (UCSB; he/him) : I believe it’s something like 50-100 thousand times the age of the universe
08:35:46	 From JJ Hermes (Boston University) : The coolest white dwarfs are still hotter than 3000 K!
08:36:14	 From Sean Kelly 🌟 : 690 Billion years then?
08:36:23	 From JJ Hermes (Boston University) : That is, in our 11-billion-year-old galaxy, the oldest (coolest) white dwarfs are still hotter than 3000 K.
08:36:44	 From Sean Kelly 🌟 : They started at 100,000 K?
08:36:47	 From JJ Hermes (Boston University) : The cooling is not linear, so way longer than that 690 billion years. As they get cooler, they cool more slowly.
08:36:50	 From Jared Goldberg (UCSB; he/him) : Sean, I think Trillions
08:36:54	 From Jared Goldberg (UCSB; he/him) : White dwarfs are hot but faint, which means they need longer to radiate away their heat. Especially if some of that energy goes to latent heat of crystallization or material diffusing or settling
08:37:01	 From Sean Kelly 🌟 : Oops! Yes
08:37:31	 From Sean Kelly 🌟 : Cools by blackbody radiation
08:37:52	 From Sean Kelly 🌟 : OOh!
08:37:56	 From Sean Kelly 🌟 : Z-machine!
08:38:36	 From Mark Zagaeski : That is particularly appealing to me ( Dr. Z to my students and friends)
08:39:20	 From Matteo Cantiello : lol
08:39:38	 From woody maxwell : very cool
08:43:21	 From Natascha Cox : Thank you Michael M., I used to be part of the UT Astronomy Teachers program under Mary Kay and the Keely F.  It's where I learned all my Astronomy! :)
08:43:41	 From Brandon Rodriguez : Awesome talk! Thanks so much.
08:49:52	 From Sean Kelly 🌟 : @Michael Thank you
08:52:15	 From Charlie Payne : Will those extra Z-Machine slides be available as well?
08:53:00	 From woody maxwell : @Michael interesting use of electricity
08:53:06	 From Natascha Cox : https://www.sandia.gov/z-machine/
08:54:20	 From Lynne Stark : Could we get the video of the evolving HR Diagram?
08:54:50	 From Matteo Cantiello : I think Mike will share slides later. Including all the videos.
08:55:16	 From Jared Goldberg (UCSB; he/him) : White dwarf ~ size of the Earth, Neutron star ~ size of Los Angeles
08:56:57	 From woody maxwell : @Jared, thanks
08:58:05	 From Mark Maier : Can the rotation periods of white dwarfs be used to estimate their ages?