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BEGIN:VEVENT
DTSTAMP:20260428T032950Z
DTSTART;VALUE=DATE-TIME:20210226T160000
DTEND;VALUE=DATE-TIME:20210226T170000
SUMMARY:Laura Bercic (MSSL): Using in situ measured electron VDF to estim
 ate solar coronal temperature and ambipolar electric field in the solar 
 wind
TZID:Europe/London
UID:20210226-8a17841a7763c46001776929ecb421ab@warwick.ac.uk
CREATED:20210223T183810Z
DESCRIPTION:Abstract: The solar coronal plasma which escapes the Sun’s gr
 avity and expands through our solar system is called the solar wind. It 
 consists mainly of electrons and protons\, carries the Sun’s magnetic fi
 eld and\, at most heliocentric distances\, remains weakly-collisional. D
 ue to their small mass\, the solar wind electrons have much higher therm
 al velocity than their positively charged counterpart\, and play an impo
 rtant role in the solar wind energetics by carrying the heat flux away f
 rom the Sun. Their velocity distribution functions (VDFs) are complex\, 
 usually modeled by three components. While the majority of electrons bel
 ong to the low-energetic thermal Maxwellian core population\, some reach
  higher velocities\, forming either the magnetic field aligned strahl po
 pulation\, or an isotropic high-energy halo population. This shape of th
 e electron VDF is a product of the interplay between Coulomb collisions\
 , adiabatic expansion\, global and local electro-magnetic fields and tur
 bulence. During the talk I will focus on the effects of two of these: gl
 obal ambipolar electric field and Coulomb collisions. We compare the res
 ults of BiCoP kinetic solar wind model with the in situ solar wind measu
 rements provided by the Parker Solar Probe. Following the kinetic model 
 results we can use features of in situ VDF to estimate plasma conditions
  in the solar corona and some global properties of the solar wind. We de
 monstrate that the fast streaming electrons forming the strahl populatio
 n do not strongly interact with the surrounding plasma and partially pre
 serve the shape of the VDF they had in the solar corona. This allows us 
 to estimate coronal electron temperature at their origin. The interplay 
 between ambipolar electron field and Coulomb collisions defines the loca
 tion of the transitions between separate electron populations in the vel
 ocity space. Recognizing the strahl break-point and the electron cutoff 
 velocity in the in situ VDFs\, thus gives estimations about the strength
  of the ambipolar electric field and potential in the solar wind.
LOCATION:
CATEGORIES:CFSA Seminar
LAST-MODIFIED:20210223T183810Z
ORGANIZER;CN=Anne-Marie Broomhall:
END:VEVENT
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