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BEGIN:VEVENT
DTSTAMP:20260427T151154Z
DTSTART;VALUE=DATE-TIME:20181114T110000
DTEND;VALUE=DATE-TIME:20181114T120000
SUMMARY:Larisa Kashapova (Institute of Solar Terrestrial Physics\, Irkuts
 k) & Elena Kupriyanova (Pulkovo)
TZID:Europe/London
UID:20181114-8a17841a669b2d5b0166a56d90347a1d@warwick.ac.uk
CREATED:20181109T114002Z
DESCRIPTION:Why we are interesting in study in faint solar flares? L. Kas
 hapova\, D. Zhdanov\, S. Lesovoi\, A. Kudryavtseva (ISTP SB RAS\, Irkuts
 k\, Russia) and Lomonosov BDRG collaboration( The Skobeltsyn Institute\,
  MSU\, Moscow\, Russia) Institute of Solar Terrestrial Physics SB RAS\, 
 Irkutsk\, Russia Studying the solar flares we are usually facing with th
 at the powerful events are combination of phenomena and processes of dif
 ferent nature. This results to different explanations based on different
  scenarios which sometimes contradict to each other. The faint solar fla
 res ( the B\, C GOES classes and lower) are attractive objects for study
  of the processes of energy release and transport . They mostly present 
 В«pure casesВ» and provide more clear data for revealing of the mechanis
 ms and testing of the theoretical models and hypothesis. However the low
  level of their emission both in X-rays and microwaves is obstacle for t
 he progress in this field. New generation of radio telescopes and combin
 ation of X-ray data (time profiles and spectral data) with observations 
 in radio (microwaves) and results of modeling allow to diagnose the ener
 gy release processes with confidence even for very weak events. Nowadays
  we have the multiple scenario set for weak solar flare from the high te
 mperature events to "cold flares". We present the possibilities of such 
 diagnostics by the example of the several events and discuss limits of s
 uch approach basing on the modern observational data. Non-stationary pro
 perties of quasi-periodic pulsations in flare emission Elena Kupriyanova
 1\, Dmitrii Kolotkov2\, Anastasiya Kudryavtseva3\, Larisa Kashapova3 1 C
 entral Astronomical Observatory at Pulkovo of RAS\, Saint Petersburg\, R
 ussia 2 CFSA\, University of ÌÇÐÄTV\, Coventry\, UK 3 Institute of Sola
 r-Terrestrial Physics SB RAS\, Irkutsk\, Russia Abstract One of the prin
 cipal questions in solar physics is related to the energy release and en
 ergy transport in solar flares. Quasi-periodic pulsations (QPPs) are an 
 intrinsic property of the flares. They are observed in various frequency
  ranges of electromagnetic spectrum\, from gamma rays to radio waves\, d
 uring all phases of solar flares. Development of diagnostics of mechanis
 ms of the QPPs allows for understanding the processes both qualitatively
  and quantitatively. Current methods of diagnostics of QPPs are develope
 d based on the QPPs having either stationary or slowly varying parameter
 s. However\, non-stationarity of the parameters (deviation from a sine c
 urve) of the QPPs is predicted from theoretical models of QPPs based on 
 either on MHD oscillations of plasma structures or on auto-oscillations 
 or on a combination of the previous two. Recently\, the evidences were f
 ound on the presence of the QPPs with the time dependent parameters (her
 einafter\, non-stationary QPPs) in solar and stellar flares. Here we pre
 sent first results of analysis of three solar flares aiming to distingui
 sh between natural non-stationarity associated with a time-dependent phy
 sical process and the one appeared due to a multi-modal structure of QPP
 s. First time\, data of the renewed Siberian Radioheliograph (SRH) at 4–
 8 GHz are applied for this reason.
LOCATION:PS017
CATEGORIES:CFSA Seminar
LAST-MODIFIED:20181109T114002Z
ORGANIZER;CN=Anne-Marie Broomhall:
END:VEVENT
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