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SUMMARY:Lecture: Manifestations and Physics of Galactic Winds and Outflows
  (1/2)
DTSTART;VALUE=DATE-TIME:20240904T120000Z
DTEND;VALUE=DATE-TIME:20240904T140000Z
DTSTAMP;VALUE=DATE-TIME:20260314T134939Z
UID:indico-event-412@cern.ch
DESCRIPTION:The lecture is held in two parts. 1st part on Wednesday\, 2nd 
 part on Thursday.\n\nBy registering you agree to be listed as participant 
 here on the event page.\n\n\nOutline:\n\n1. Manifestations of Galactic Out
 flows\n\n\n	emphasis on Milky Way\, but the physics is applicable to all G
 alaxies at all redshifts\n	observed features\n	\n		bipolar outflow on 10-p
 c scale\n		 the Galactic center chimneys\, radio an X-ray - large-scale s
 ynchrotron radio features\n		Fermi Bubbles\n		eRosita Bubbles\n	\n	\n\n\n2
 . Sources of gas outflow from galaxies\n\n\n	AGNs: jets versus winds\n	tid
 al disruption events\n	star formation\, —> supernovae\n	collective super
 novae\n\n\n3. The Galactic wind\n\n\n	broad angular distribution relative 
 to Galactic center\n	entrained neutral gas clumps as best evidence\n	fate 
 of dense gas clumps: disintegration or growth\n	\n		ablation\n		instabilit
 ies: Rayleigh-Taylor\, Kelvin-Helmholtz\n		compression —> enhanced cooli
 ng\, density growth\n	\n	\n\n\n4. Determinants of the expansion rate of ou
 tflows\n\n\n	initial ejection velocity\, if any\n	temperature (sound speed
 ) —> adiabatic expansion\n	\n		plasma cooling time versus expansion time
 \n	\n	\n	gravitational deceleration\n	shocks with ambient gas\, mass loadi
 ng\n\n\n5. The Galactic Magnetic Field\n\n\n	a collimator for the wind\n	\
 n		versus collimation caused by Galactic density gradient\n	\n	\n	magnetic
  pressure versus ram pressure versus gas pressure how strong does the fiel
 d need to be?\n\n\n6. Relativistic gas —> Cosmic Rays\n\n\n	acceleration
  mechanisms\n	diffusion\n	role of magnetic fields\n	anisotropy of diffusio
 n coefficients\n	synchrotron emission\n	application to Fermi Bubbles\n\n\n
 7. Interaction with the Galactic halo\n\n\n	shocks\n	sharp bubble edges: q
 uasi-steady shock or surface moving in response to energy injection?\n	wha
 t goes up must come down: the Galactic fountain\n	\n		cooling instabilitie
 s\n	\n	\n\n\n \n\nhttps://events.mpifr-bonn.mpg.de/indico/event/412/
LOCATION:MPIfR 0.02
URL:https://events.mpifr-bonn.mpg.de/indico/event/412/
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