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UID:UW-Physics-Event-9169
DTSTART:20250403T203000Z
DTEND:20250403T213000Z
DTSTAMP:20260413T201347Z
LAST-MODIFIED:20250324T144357Z
LOCATION:4421 Sterling Hall
SUMMARY:New Phenomena Around Supermassive Black Holes: Dynamics and Ch
 emistry\, Astronomy Colloquium\, Mark Gorski\, CIERA Postdoctoral Fell
 ow
DESCRIPTION:In 1982 Blandford and Payne predicted that magnetic fields
  are fundamental for accretion onto supermassive black holes (SMBHs). 
 Magnetic field lines anchored in the disk accelerate a wind via the ce
 ntrifugal force\, allowing for the angular momentum to be transferred 
 out of the system and gas to accrete onto the central compact object g
 enerating an active galactic nucleus (AGN). The wind can form a few Sc
 hwarzschild radii from the SMBH up to the nuclear torus. Almost a half
  century later\, the detailed mechanisms of SMBH growth are still a pa
 ssionate area of research. Astronomers currently debate whether winds 
 are fuelled by jets\, mechanical winds\, or radiation\, with magnetic 
 processes being the least accepted explanation. Here\, I present detai
 led ALMA observations of the most compact and opaque galactic nuclei i
 n the universe\, appropriately named compact obscure nuclei (CONs). CO
 Ns represent a significant phase of galactic nuclear growth\, with opa
 que and compact centers (r <100 pc)\, that conceal growing SMBHs. The 
 analysis of these observations reveal a wind that exceeds theoretical 
 maximum momentum for an AGN feedback powered galactic wind. The extrem
 e momentum implies the existence of a magneto hydrodynamic (MHD) wind.
  The wind is highly collimated and rotates out to 100pc above the gala
 ctic nucleus. Furthermore\, abundances of complex organic molecules ri
 val Sgr B2 and Galactic hot cores in the nucleus. These results imply 
 that growth of SMBHs is very similar to the growth of hot cores or pro
 tostars\, and feedback from an AGN is not necessary to drive a galacti
 c wind.
URL:https://www.physics.wisc.edu/events/?id=9169
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