iiinova — where your digital self keeps evolving

Falk Herwig

@fherwig.bsky.social

Astrophysics prof at University of Victoria interested in how and where the elements form in stars and stellar explosions and how to use anything computing or digital to find out.

Posts Replies Media

Falk Herwig @fherwig.bsky.social · 17/12/2025

Our new multidisciplinary Nature Reviews Physics article “Unlocking i-process nucleosynthesis by bridging stellar and nuclear physics” (rdcu.be/ePnGP) is a key step in establishing the intermediate neutron-capture (i-process) as an emerging frontier in nuclear astrophysics.

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Falk Herwig @fherwig.bsky.social · 11/05/2025

We are looking forward to hosting Stellar Hydro Days VI in Victoria next week sites.google.com/view/stellar... A week dedicated to a deep dive into 3D simulations of stars, transport phenomena, internal gravity waves, asteroseismology predictions, wave turbulence and more ....

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Falk Herwig @fherwig.bsky.social · 27/03/2025

Great accomplishment @wrtastro.bsky.social !!! William not only did exceptional work in the field of planet imaging but also lead one of our most important projects in recent years in computational stellar astrophysics on internal gravity waves in massive stars ui.adsabs.harvard.edu/abs/2024MNRA...

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Falk Herwig @fherwig.bsky.social · 13/03/2025

First paper by our MSc student Praneet Pathak: model uncertainties in white dwarf cooling ages. For a typical white dwarf, systematic uncertainties can reach 0.8 Gyr at 4000K – comparable to measurement errors! This is key when white dwarfs are used as cosmic clocks. arxiv.org/abs/2410.14014

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Falk Herwig @fherwig.bsky.social · 25/01/2025

Our model invokes a reduced entropy equation with turbulent dissipation input from 3D hydro simulations and takes all terms incl. buoyancy and the pressure-gradient force into account. Extrapolating this model to nominal heating (log b = 0 in the figure) gives penetrative boundary mixing of 0.7Hp.

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Falk Herwig @fherwig.bsky.social · 25/01/2025

... best shown in line plots.Our analysis demonstrates that energetically and on a global scale work done by the large-scale pressure gradients is equally important in core convection as the buoyancy force. That was new to me and has obviously implications for any model of convective penetration.

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