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BEGIN:VEVENT
DTSTAMP:20260612T151714Z
DTSTART;VALUE=DATE-TIME:20220302T163000
DTEND;VALUE=DATE-TIME:20220302T173000
SUMMARY:Dynamics of solar flares with microwave imaging spectroscopy by D
 r G. Fleishman (NJIT\, USA)
TZID:Europe/London
UID:20220302-8a17841a7ef83658017f049ec61f5fa5@warwick.ac.uk
CREATED:20220216T221948Z
DESCRIPTION:Release of magnetic energy due to reconnection is believed to
  drive such transient phenomena as solar flares\, eruptions\, and jets. 
 This energy release should be associated with a decrease of the coronal 
 magnetic field. Quantitative measurements of the evolving magnetic field
  strength in the corona are required to find out where exactly and with 
 what rate this decrease takes place. The only available methodology capa
 ble of providing such measurements employs microwave imaging spectroscop
 y of gyrosynchrotron emission from nonthermal electrons accelerated in f
 lares. Here\, we report microwave observations of a solar flare\, showin
 g spatial and temporal changes in the coronal magnetic field at the cusp
  region\; well below the nominal reconnection X point. The field decays 
 at a rate of ~5 Gauss per second for 2 minutes. This fast rate of decay 
 implies a highly enhanced\, turbulent magnetic diffusivity and sufficien
 tly strong electric field to account for the particle acceleration that 
 produces the microwave emission. Moreover\, spatially resolved maps of t
 he nonthermal and thermal electron densities derived from the same micro
 wave spectroscopy data set allow us to detect the very acceleration site
  located within the cusp region. The nonthermal number density is extrem
 ely high\, while the thermal one is undetectably low in this region indi
 cative of a bulk acceleration process exactly where the magnetic field d
 isplays the fast decay. The decrease in stored magnetic energy is suffic
 ient to power the solar flare\, including the associated eruption\, part
 icle acceleration\, and plasma heating. We discuss implications of these
  findings for understanding particle acceleration in solar flares and in
  a broader space plasma context.
LOCATION:MS Teams
URL:
ATTACH:
CATEGORIES:Departmental Colloquium
LAST-MODIFIED:20220216T221948Z
ORGANIZER;CN=Valery Nakariakov:
END:VEVENT
END:VCALENDAR