Desde Diciembre 20, 2016 13:15 hasta Diciembre 20, 2016 13:45
En Seminar Room
Massive-star mass loss through stellar winds plays an important role in a variety of phenomena: stellar evolution, the shaping of star-forming regions, the circumstellar ejecta into which supernovae explode, and as sources of material for accretion. Hydrodynamic simulations of such colliding winds in multi-star systems, and then direct synthesis of the thermal X-ray emission, provides a direct model-to-data comparison to constrain its wind, stellar, and orbital parameters. I will discuss these efforts applied to massive-star binaries, which have explained phase-locked X-ray emission in long-period (multi-year) systems such as eta Carinae, as well as short-period (few days) systems such as delta Orionis A. Next, I will present the X-ray modeling of Prof. Jorge Cuadra's hydrodynamic simulations of the Galactic Center, where the good agreement in spectral shape supports the hypothesis that the diffuse emission observed with Chandra around Sgr A* is from massive-star-wind collisions, and the flux comparison suggests that a strong outburst from Sgr A* several centuries ago cleared out material from around Sgr A*, including hot, X-ray emitting gas.
I will conclude with my recent foray into 360 degrees (or more accurately 4pi steradian) videos of our hydrodynamic simulations. It places the observer inside the simulation domain to give a new perspective, and has unique outreach potential given the ability of video-sharing sites such as YouTube to play 360 degrees videos on both smartphones and computers. Better yet is to experience the 360 degrees videos with virtual reality goggles, which I will be happy to demonstrate to you all at the end of the talk.