In the field of astrophysics, neutrinos are invaluable. They traverse space without being affected by matter or electromagnetic fields.

In Figures D.1 and D.2 we show the retrieved exoplanet parameters and abundances for the different scenarios with varying R and S/N values.

The details of how gas flows into the galactic nucleus from large cosmic distances and how the SMBH in turn imparts feedback into the galaxy remain unresolved.

Testing the accuracy of our method by numerically stimulating hydrodynamic spherical bondi accretion.

Our numerical scheme utilizes the GRMHD code KHARMA[1], a performance-portable C++ implementation based on iharm3D; iharm3D is itself an extension of HARM.

To investigate the mechanism driving the turbulence, we explore the physics of the outward flow of energy.

The authors HC, RN, PN, KS, AR, and KC acknowledge support from the Gordon and Betty Moore Foundation and the John Templeton Foundation

If you want to continue learning about black holes, here's a list of all the references.

Wrapping up our black hole study: a final rundown.