Making Supernovae with Jets
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The document discusses the implementation of high-order magnetohydrodynamics to explore the generation of jets in supernovae, focusing on their role as endpoints of stellar evolution that create and disperse heavy elements. It highlights collaborations among computational scientists at Michigan State University to advance research in astrophysics through the development of advanced models. Key concepts include the mechanism behind core-collapse supernovae and the associated magneto-rotational instability necessary for jet formation.
![resolution issue: modes start small
0
ρ∇Φ
pv∙∇Φ
0
Ω : rotation profile (3D)
N: buoyancy (Brunt-Väisälä frequency)
R: differential rotation term
equatorial:
C = (N2 + R)/Ω2 < 0
unstable
scale of fastest growing mode:
λFGM ~ |v⃗A| [-(N2 + R)]-1/2
e.g., Obergaulinger+ 2009
growth time ~10 ms](https://image.slidesharecdn.com/charris-200127212728/85/Making-Supernovae-with-Jets-47-320.jpg)
![SparkJoy: high order version of Spark
CPU hours
resolution (cells per length)
numericalviscosity[cm2s-1]
goal
5th
7th
9th
Rembiasz+ 2017
5th
2nd
Zhang, Zhang & Shu (2011)](https://image.slidesharecdn.com/charris-200127212728/85/Making-Supernovae-with-Jets-49-320.jpg)
Making Supernovae with Jets
- 1. Making Supernovae with Jets Chelsea Harris Sean Couch, Andrew Christlieb, Luke Roberts
- 2. implementing high-order magnetohydrodynamics to explore jets in stellar explosions making jets in a supernova high-order magnetorotational hydrodynamics with SparkJoy the cool things I’m a part of
- 3. implementing high-order magnetohydrodynamics to explore jets in stellar explosions the cool things I’m a part of
- 4. MSU Department of Computational Mathematics, Science, and Engineering CMSE … will enable application-driven computational modeling (“pull”), while also exposing disciplinary computational scientists to advanced tools and techniques (“push”), which will ignite new transformational connections in research and education. MSU CMSE …scientists who may reside in science, mathematics, engineering or computer science departments but share an interest in research using computing and mathematical methods. … DOE CSGF helps these computational scientists develop a sense of community that’s often difficult to find in a single academic department. DOE CSGF
- 5. MSU Department of Computational Mathematics, Science, and Engineering March 16 February 21
- 6. TEAMS Toward Exascale Astrophysics of Mergers and Supernovae SciDAC
- 7. implementing high-order magnetohydrodynamics to explore jets in stellar explosions making jets in a supernova the cool things I’m a part of
- 9. ✦ star ripped apart by shock in <1 second ✦ different explosion mechanisms ✦ bright from radioactivity supernovae: stellar explosions
- 12. create & disperse heavy elements endpoints of stellar evolution
- 13. energize galaxiescreate & disperse heavy elements endpoints of stellar evolution
- 14. energize galaxiescreate & disperse heavy elements cosmological tools endpoints of stellar evolution
- 15. energize galaxiescreate & disperse heavy elements cosmological tools endpoints of stellar evolution site of r-process elements?
- 16. elements heavier than Fe: neutron capture Cowan+ 2019
- 17. s r r-process: rapid neutron capture onto nuclei ‣ some elements/isotopes come only from r-process ‣ we have tracers! ‣ requires neutron-rich environment Cowan+ 2019
- 18. best candidates for r-process sites neutron star mergers supernovae
- 19. TEAMS Toward Exascale Astrophysics of Mergers and Supernovae SciDAC
- 20. TEAMS Toward Exascale Astrophysics of Mergers and Supernovae SciDAC WURP What’s Up with the R-Process?
- 21. core-collapse supernovae create neutron stars HST
- 22. core-collapse supernovae create neutron stars 1054 AD HST
- 23. core-collapse supernovae create neutron stars 1054 AD HST Chandra VLA+Spitzer+HST+XMM Newton+Chandra
- 24. neutrons = r-process? heavy seed nuclei n-rich material PNS 😀
- 25. heavy seed nuclei n-rich material PNS ν 🤔 neutrons = r-process?
- 26. heavy seed nuclei n-rich material PNS νe p-rich 😢 neutrons = r-process?
- 29. creating jets in core-collapse SNe ‣ seen in nature: long gamma- ray bursts associated with SNe ‣ magnetic confinement - narrow jet ‣ stars have magnetic fields! ‣ need to amplify field over one billion times … in ~10 ms. Mösta+ 2015 Bφ 133km
- 30. creating jets in core-collapse SNe ‣ seen in nature: long gamma- ray bursts associated with SNe ‣ magnetic confinement - narrow jet ‣ stars have magnetic fields! ‣ need to amplify field over one billion times … in ~10 ms. Mösta+ 2015 Bφ 133km
- 31. rotation Balbus & Hawley (1991) speed increases inward angular momentum increases outward the Magneto-Rotational Instability
- 32. rotation Balbus & Hawley (1991) speed increases inward angular momentum increases outward the Magneto-Rotational Instability
- 33. magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 34. magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 35. magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 36. Balbus & Hawley (1991) the Magneto-Rotational Instability
- 37. SIDE VIEW TOP VIEW Balbus & Hawley (1991) the Magneto-Rotational Instability
- 38. SIDE VIEW TOP VIEW rotation rotation Balbus & Hawley (1991) the Magneto-Rotational Instability
- 39. SIDE VIEW TOP VIEW to NS fast & low energy slow & high energy rotation weak magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 40. SIDE VIEW TOP VIEW to NS fast & low energy slow & high energy rotation weak magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 41. SIDE VIEW TOP VIEW to NS fast & low energy slow & high energy rotation weak magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 42. SIDE VIEW TOP VIEW to NS fast & low energy slow & high energy rotation weak magnetic field, B Balbus & Hawley (1991) the Magneto-Rotational Instability
- 43. initial B⃗ (purely poloidal) final B⃗ (poloidal piece) amplification! (lines squeezed) Balbus & Hawley (1991) the Magneto-Rotational Instability
- 44. initial B⃗ (purely poloidal) final B⃗ (poloidal piece) amplification! (lines squeezed) Balbus & Hawley (1991) the Magneto-Rotational Instability
- 45. implementing high-order magnetohydrodynamics to explore jets in stellar explosions making jets in a supernova high-order magnetorotational hydrodynamics with SparkJoy the cool things I’m a part of
- 46. resolution issue: modes start small p ρ ℰ B⃗
- 47. resolution issue: modes start small 0 ρ∇Φ pv∙∇Φ 0 Ω : rotation profile (3D) N: buoyancy (Brunt-Väisälä frequency) R: differential rotation term equatorial: C = (N2 + R)/Ω2 < 0 unstable scale of fastest growing mode: λFGM ~ |v⃗A| [-(N2 + R)]-1/2 e.g., Obergaulinger+ 2009 growth time ~10 ms
- 48. MHD in FLASH with Spark FLASH - AMReX explicit Runge-Kutta WENO reconstruction 1 2 3 4
- 49. SparkJoy: high order version of Spark CPU hours resolution (cells per length) numericalviscosity[cm2s-1] goal 5th 7th 9th Rembiasz+ 2017 5th 2nd Zhang, Zhang & Shu (2011)
- 50. numerical resistivity creates turbulence kilometers from PNS kilometers from PNS kilometers from PNS verticalposition(km) verticalposition(km) verticalposition(km) Obergaulinger+ 2009
- 51. components of SparkJoy Helzel et al. (2013); Buchmuller et al. (2016) FLASH - AMReX finite volume explicit Runge-Kuttamulti-D flux using neighbors constrained transport WENO reconstruction conserved variables p ρℰ B⃗ 1 2 3 4 A⃗ B⃗ B⃗=∇×A⃗ → ∇∙B⃗=0
- 52. current status: talk-killer bug
- 53. print *, SELF prolonged stress + devaluation of human interactions + criticism over validation + work/self blur (i.e. creative) = terrible for mental health
- 54. implementing high-order magnetohydrodynamics to explore jets in stellar explosions making jets in a supernova high-order magnetorotational hydrodynamics with SparkJoy the cool things I’m a part of