11:15:36	 From Richard Moore : sorry, I meant period. the O-C (sec) was supposed to be period, I guess
11:18:15	 From BARBARA CASTANHEIRA ENDL (Baylor University) : O-C is in seconds. It’s basically a measurement of the phase. The first point is set to be 0, for instance, when the maximum of the mode is observed. The following points are relative observations of the maxima for the same pulsation mode, but at different times.
11:19:35	 From BARBARA CASTANHEIRA ENDL (Baylor University) : In turn, the pulsations are arriving a bit later. It could mean that the star is moving away from us (but this one is not) or the period is becoming a bit longer overtime.
11:26:39	 From Sean Kelly 🌟 : Also no carbon, oxygen?
11:28:22	 From Sean Kelly 🌟 : Is there an estimation of the number of Type Ia supernovae that will be these white dwarf binaries?
11:30:00	 From Sean Kelly 🌟 : What is the inspiral time for a double white dwarf system?
11:31:20	 From Jim Deane - Ottawa KS : Is that a video or are you running a simulation in realtime?
11:31:53	 From Jim Deane - Ottawa KS : Ah, I see the video control now.
11:32:25	 From Sean Kelly 🌟 : Does the core detonate with a mass smaller than the Chandrasekhar limit?
11:32:33	 From Justin Dillon : yes
11:33:17	 From NIcole Preiser : I read recently about an idea by Horowitz and Caplan that crystallization of uranium during cooling in a WD could lead to runaway nuclear fission and result the core detonating like a nuclear explosion. Where does the U-235 in the core come from? How is there enough uranium for this process to occur?
11:36:45	 From Bryn Bishop (she/her) : Where can I get a video of this snapping shrimp? This is really cool.
11:37:12	 From Matteo Cantiello : I think this is the Radio Lab episode Ken mentioned. Highly recommended: https://www.wnycstudios.org/podcasts/radiolab/articles/bigger-bacon
11:37:24	 From Bryn Bishop (she/her) : @Matteo thank you!
11:38:20	 From Matteo Cantiello : A video also avail here. Not sure it’s the same one that Ken used though: https://www.youtube.com/watch?v=Zg10Et8FEWc&ab_channel=MichelVersluis
11:41:57	 From Sean Kelly 🌟 : Have any stars been found "between" galaxies, other than in tidal streams?
11:43:06	 From Sean Kelly 🌟 : Escape velocity for the Milky Way is 550 km/s
11:47:32	 From Matteo Cantiello : not that I know of (others?). The issue is that it gets very hard because they would need to be bright to be seen from so far away. But the brighter the star you are, the shortest your life is. Massive stars live for only a few million years, so even if you were to slingshot them at ~1000 km/s, they would die shortly after or even before exciting the Galaxy. This said we have seen some Type Ia exploding away from their galaxy
11:49:03	 From JJ Hermes (Boston University) : And we now have back catalogs of images of galaxies that put good limits on the stars that explode, and we would see red giants in most of those images, and don’t.
11:51:53	 From JJ Hermes (Boston University) : Porb = 50 years I think
11:53:10	 From Jared Goldberg (UCSB; he/him) : 10^51 ergs = 2.39006x10^34 tons of TNT. The largest nuclear bomb humans ever made was just 5x10^7 tons...
11:53:51	 From Michael Montgomery (UT-Austin) : I think they may be far enough apart to not really interact...
12:00:30	 From JJ Hermes (Boston University) : I had never found this Wikipedia page until now, thanks for the question about supernova proximity! https://en.wikipedia.org/wiki/Near-Earth_supernova
12:01:25	 From Matteo Cantiello : The OG death star
12:04:47	 From Erminio Maganzini : Has LISA been funded?
12:05:22	 From Jared Goldberg (UCSB; he/him) : I believe it’s primarily ESA, unless NASA goes back in
12:05:32	 From David Wittenberg : Thank you Ken.
12:05:44	 From Richard Moore : "My futures so bright, I gotta wear shades", an 80's song on MTV