The inner parsec of the Galactic center: hydrodynamics, X-ray modeling, and 360-degree videos

The Galactic Center's inner parsec is a hotbed of astrophysical activity, with the injection of wind material from ∼30 Wolf-Rayet (WR) stars orbiting the supermassive black hole (SMBH) playing an important role. We compute the thermal X-ray emission from a suite of Galactic-center hydrodynamic simulations that have various SMBH feedback mechanisms, which are compared to Chandra X-ray Visionary Program observations of the region. Over a 2-5" ring centered on our galaxy's SMBH (Sgr A*), the spectral shape is well matched, indicating that the WR winds are the dominant source of the thermal X-ray emission. Furthermore, the X-ray flux depends on the SMBH feedback due to the feedback's ability to clear out material from the central parsec. A moderate outburst is necessary to explain the current thermal X-ray flux, even though the outburst ended ∼100 yr ago. We will report on our efforts to expand this modeling by including the ∼100 O stars and the `S' stars in the region. Additionally, we will present our 360-degree videos of the aforementioned Galactic-center simulations. These movies render an image over all 4π steradian, and therefore provide a unique and immersive way to visualize astrophysical simulations. Viewed from the perspective of Sgr A*, the most striking aspect of our latest video, which renders column density, is the inspiraling and stretching of clumps of WR-wind material as they make their way towards the SMBH. Video sharing sites such as YouTube allow these videos to be shared with the masses; they can be viewed in their 360-degree nature on computer screens, with smartphones, or, best of all, in virtual-reality (VR) goggles. Our latest video, powered by a Chandra press release, went viral and has been viewed on multiple platforms over 1.2 million times!