BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//ZContent.net//ZapCalLib 1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20191015T123000
DTEND;TZID=Atlantic/Canary:20191015T133000
UID:iactalks-1326
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1326
CREATED:2019-10-15T12:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Arch Filament Systems and their evolution through the layers of the
  solar atmosphere
DESCRIPTION:Arch Filament Systems and their evolution through the layers of
  the solar atmosphere\nDr. Sergio Javier Gonzalez Manrique\n\nEmerging flu
 x regions (EFRs) are seen as magnetic concentrations in the photosphere of
  the Sun. From a theoretical point of view, the EFRs are formed in the con
 vection zone and then emerge because of magnetic buoyancy (Parker instabil
 ity) to the solar surface. During the formation process of EFRs, merging a
 nd cancellation of different polarities occur, leading to various configur
 ations of the magnetic field. Often, EFRs are visible in the chromosphere 
 in form of magnetic loops loaded with plasma, which are often called &ldqu
 o;cool loops” when seen in the chromosphere along with dark fibrils 
 and they can reach up to the corona. Nowadays, we refer to them as an arch
  filament system (AFS) which connects two different polarities.  The 
 AFSs are commonly observed in several chromospheric spectral lines. A suit
 able spectral line to investigate chromospheric features and particularly 
 AFSs is the He I 10830 Å triplet. The new generation of solar telesc
 opes and instruments such EST and DKIST, will allow us to record very high
  spectral, spatial, and temporal resolution observations necessary to inve
 stigate the dynamics, magnetic field, and characteristics of AFSs. These o
 bservations will help us to answer many open questions related to flux eme
 rgence such: (1) What are the observational consequences of the emerging f
 lux? (2) How do EFRs evolve with time in the different layers of the solar
  atmosphere and how are these layers linked? (3) Is it possible to measure
  the height difference between the photosphere and the chromosphere connec
 ted by the legs of the AFSs?
END:VEVENT
END:VCALENDAR