## Some of the Current Projects

### Magnetar Powered Supernovae

###### with Ke-Jung Chen and Stan Woosley

Two dimensional CASTRO results for a magnetar powered supernova explosion of a bare CO core. The density profile is shown at t=0, 800, 1600 and 2400 seconds since the deposition started.

### Overshooting In The Upper Main-Sequence

###### with Casey Meakin, Hassen Yesuf and Zeyana Musthafa

Figure 1 of Meakin et al. (2011) - overshoot parameter estimates from detached Eclipsing Binaries (diamonds) and asteroseismological data (triangles). The values adopted by Girardi et al. (2000) and Pietrinferni et al. (2004) for populations synthesis are labeled as G2000 and P2004. The mass uncertainties for the eclipsing binary data are negligible on the log(M) scale used. It is one big mess!

## Some of the Published/Submitted Works

#### The Most Luminous Supernovae

###### with Stan Woosley. Submitted to The Astrophysical Journal Letters.

Fig. 2 from the paper. Top: The luminous transient ASASSN-15lh (red bars) compared with a magnetar-powered model. Similar magnetars embedded in a smaller ejecta with lower opacity can, in principle, give even brighter light curves exceeding $\mathrm{10^{46}\ erg\ s^{-1}}$. Bottom: The same magnetar used in the top panel for fitting ASASSN-15lh is embedded in the ejecta of a massive red supergiant progenitor. The light curve is dimmer than the Type I case, but substantially brighter than the high energy prompt explosion (gray). The dashed part of curves mark the transition to nebular phase.

#### Survey of CCSNe between $\mathrm{9-120\ M_{\odot}}$ based on Neutrino-Powered Explosions

###### with Thomas Ertl, Stan Woosley, Justin Brown and Thomas Janka. The Astrophysical Journal.

Fig. 13 from the paper. The explosion outcomes are shown for five different 'engines' all calibrated to SN1987A. Engines are listed in increasing strength. NS=neutron star; BH=black hole.

#### The Compactness of Presupernova Stellar Cores

###### with Stan Woosley. The Astrophysical Journal.

Fig. 1 of Sukhbold et al. (2015). The compactness parameter, $\mathrm{\xi_{2.5}}$ , enclosing inner $\mathrm{2.5\ M_{\odot}}$ at the time of presupernova is shown as a function of initial mass for 200 solar metallicity non-rotating progenitors.