Deep X‐Ray Imaging of the Central 20 Parsecs of the Galaxy with Chandra

The Fate of Nonradiative Magnetized Accretion Flows: Magnetically Frustrated Convection

“…This has been observed in nonmagnetic simulations by Proga & Begelman (2003) and by us. It could be avoided if the inner boundary supplied a strong jet that interfered with axial accretion, as occurs in protostars (Matzner & McKee 2000), but suggestions of such behavior in Chandra images are recent and tentative (Morris et al 2002). Similarly, models that invoke rotational support to stem accretion require that rotational support remains important all the way out to r Bimplying an asymmetry to the X-ray images which is not observed.…”

The Galactic Centre Chimney

“…Evidence has increasingly mounted in recent decades that outflows of matter and energy from the central parsecs of our Galaxy have shaped the observed structure of the Milky Way on a variety of larger scales 1 . On scales of ∼ 15 pc, the Galactic centre (GC) has bipolar lobes that can be seen in both X-rays and radio 2,3 , indicating broadly collimated outflows from the centre, directed perpendicular to the Galactic plane. On far larger scales approaching the size of the Galaxy itself, gamma-ray observations have identified the so-called "Fermi Bubble" (FB) features 4 , implying that our Galactic centre has, or has recently had, a period of active energy release leading to a production of relativistic particles that now populate huge cavities on both sides of the Galactic plane.…”