Here, we shall post materials related to scientific talks and discussions.

Topics from Organizing Session

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Word cloud of the topics brought up


Natasha asked "What Problems are Important?" "What Do You Hope to Learn?". Here are the responses (with acronyms etc spelled out -- please feel free to correct if your ideas have been misrepresented)

  1. Supersonic, super-Eddington convection
  2. 3-D modelling methods
  3. Angular momentum and mass loss during critical
  4. Coupling between convection and oscillations
  5. Rotation above 50% critical
  6. Observational knowledge spreading
  7. Theoretical knowledge absorption
  8. Stellar upper mass limit
  9. Multi-D radiation hydrodynamics
  10. Relation between initial mass and final black hole mass, as function of metallicity, rotation, binarity
  11. What are the controlling parameters that cause the diversity of supernovae outcomes
  12. Predictable diversity of phenomena from interacting binaries
  13. Mass loss rates as a function of binarity, metallicity, magnetic fields and rotation
  14. Relationship between pre-collapse and compact object angular momentum
  15. Observational knowledge absorption
  16. Connection between progenitors, late-phase evolution and supernovae
  17. GAIA, AS4, ZTF, BlackGem
  18. Physics in main-sequence stars
  19. Supernovae and compact objects
  20. Physics in main-sequence stars (deliberate duplicate!)
  21. Magnetic fields in main-sequence stars
  22. Physics of mass loss in evolved massive stars
  23. Common envelope evolution in massive stars
  24. Explosion mechanism of most common massive stars
  25. 3-D structure of massive stars as a function of angular momentum and magnetic field
  26. Impact of rotation on stellar evolution
  27. Common envelope evolution
  28. How surveys will impact physics of models
  29. Asteroseismology as a probe of stars
  30. Gravitational wave progenitors
  31. Long-term variability of massive stars
  32. Formation of compact binaries
  33. Observational constraints on cores
  34. Supernova impostors & stellar merger diversity
  35. Low-metallicity binary interactions
  36. Maximizing information extraction from binary population synthesis
  37. Mass-loss rates as a function of mass and luminosity
  38. Multi-D radiation hydrodynamics
  39. Link between explosion physics and binarity
  40. Pulsational pair instability supernovae
  41. 3-D nucleosynthesis
  42. Super-AGB to supernova transition
  43. Ionizing photon production from most massive stars + cosmic chronometers at lower masses
  44. Empirical constraints
  45. Machine learning
  46. How do we constrain the physics of single stars from rotation
  47. Is fast core rotation the only necessary condition to produce a central engine?
  48. What can we learn from 5 years of LIGO observations?
  49. How can we incorporate results from 3-D radiation MHD into 1-D stellar evolution codes?
  50. How can we incorporate 3-D processes (e.g., convection) into 1-D stellar evolution codes?
  51. How do common envelopes behave in massive binaries?
  52. First stars and metal poor stars
  53. How do black hole forming supernovae work and form CEMP stars?
  54. What mass-loss process forms the envelopes around massive supernovae?
  55. What's at the heart of a core collapse supernova? Engines
  56. mapping out instabilities for massive stars
  57. A beet way to understand connection between binaries and exploding events
  58. Do we get a NS, do we get a BH?
  59. Angular momentum transport and mixing throughout stellar evolution before supernova
  60. Late stages (pre SN): stellar evolution, constraints
  61. Effect of binarity on above
  62. Very Massive Stars. Mass loss of the main-sequence.
  63. How to treat envelope inflation in evolutionary models
  64. Linking supernova Mdot to stellar Mdot
  65. Better understanding of convective overshooting on main-sequence
  66. Very Massive Stars and treatment of convection there (MLT++ MESA)
  67. Find the progenitors of GW sources
  68. WInd mass loss and how does this work from really hot stars
  69. How MT working in a binary; how star reacts on MT, what is setting the stop of the Roche lobe
  70. What do I do wrong for contact binaries using 1D
  71. Process of accretion: angular momentum problem
  72. PPISN
  73. How the winds of envelopes of massive stars differ from low-mass. How to build these into simulations involving a range of length of time scales
  74. Understand the impact of binarity on all aspects of evolution of massive stars
  75. Progenitors of peculiar supernova and whether binarity is an necessary answer (II-pec, IIn, II-p etc).
  76. Uncertainty in MESA/stellar evolution (convection etc) and how it affects presupernova structure
  77. A smoking gun from LGRB/ SN Ic etc for what is formed
  78. Magnetic fields of stars
  79. Causes for LBV giant eruptions
  80. Role of pulsation for massive stars
  81. Running MESA, GYRE, and learning more python
  82. Transport by waves, magnetic fields, overshoot
  83. The DEDALUS code (dedalus-project.org)
  84. Understanding errors in codes
  85. Rotation and convection
  86. Latest updates
  87. Mass loss resulting from winds, binarity and LBV outbursts
  88. Relationship/influence of mass loss on supernovae
  89. Structure of core-collapse supernova progenitors
  90. Inferences about progenitor structure from light curves

Convection in Massive Stars [Matteo Cantiello]


Please find below MESA Inlists for 60 Msun model at solar metallicity (showing envelope density inversion and envelope convection regions, including deep iron CZ). This is the model I've shown during my talk on convection. MESA version 9268 (install MESA from here)


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