# The 21st Century H-R Diagram: The Power of Precision Photometry

I’m in Baltimore, MD at the Space Telescope Science Institute for the 2018 Spring Symposium.

# APS April Meeting

I’m in Columbus, OH at the 2018 APS April Meeting. As one of the finalists for the Outstanding Doctoral Thesis Award in Astrophysics, I’m giving a talk entitled The Long-Term Outcomes of Double White Dwarf Mergers.

# Astronomy on Tap

I’m in Santa Cruz, CA giving a public talk on stellar-mass black holes!

# Hubble Fellows Symposium

I’m in Baltimore, MD at the Space Telescope Science Institute for the 2018 Hubble Fellows Symposium. I’m giving a talk entitled The Importance of Mixing in White Dwarfs Evolving towards Explosion.

# Hot Subdwarfs Formed from the Merger of Two He White Dwarfs

Monthly Notices of the Royal Astronomical Society, vol. 476, issue 4, pp. 5303-5311

Josiah Schwab

We perform stellar evolution calculations of the remnant of the merger of two He white dwarfs (WDs). Our initial conditions are taken from hydrodynamic simulations of double WD mergers and the viscous disc phase that follows. We evolve these objects from shortly after the merger into their core He-burning phase, when they appear as hot subdwarf stars. We use our models to quantify the amount of H that survives the merger, finding that it is difficult for $\gtrsim 10^{-4}\;{\rm M}_\odot$ of H to survive, with even less being concentrated in the surface layers of the object. We also study the rotational evolution of these merger remnants. We find that mass loss over the $\sim 10^4\;\rm yr$ following the merger can significantly reduce the angular momentum of these objects. As hot subdwarfs, our models have moderate surface rotation velocities of $30-100\; {\rm km\,s^{-1}}$. The properties of our models are not representative of many apparently-isolated hot subdwarfs, suggesting that those objects may form via other channels or that our modelling is incomplete. However, a sub-population of hot subdwarfs are moderate-to-rapid rotators and/or have He-rich atmospheres. Our models help to connect the observed properties of these objects to their progenitor systems.