BEGIN:VCALENDAR
VERSION:2.0
PRODID:icalendar-ruby
CALSCALE:GREGORIAN
METHOD:PUBLISH
BEGIN:VEVENT
DTSTAMP:20260511T112001Z
UID:https://www.mps.mpg.de/events/16967/7840830
DTSTART:20181213T100000Z
DTEND:20181213T110000Z
CLASS:PUBLIC
CREATED:20181207T082042Z
DESCRIPTION:Are some parts of the Interplanetary Magnetic Field’s (IMF) n
 eutral line more flare energetic than others? What are Hale Sector Boundar
 ies (HSBs) and are they connected with flares? Do they have anything to do
  with Active Longitudes? In this work\, I will discuss how RHESSI flares a
 re associated with structures in the solar magnetic field termed as HSBs. 
 If you think of the large-scale domains of different polarity that the IMF
  is formed of\, they the parts of the boundary between them\, that have th
 e same polarity change as the sunspots back at the Sun. As the polarity of
  sunspots follows Hale’s law\, the HSB of a particular polarity change w
 ill only occur in one hemisphere per cycle\, and then alternate in the nex
 t cycle. It has previously been shown that HSBs coincide with stronger mag
 netic fields and more frequent flare occurrence (Dittmer 1975\, Svalgaard 
 &amp\; Wilcox 1976\, Svalgaard et al. 2011). I will explain how we extende
 d this work through solar cycles 23 and 24 using RHESSI flare locations fr
 om2002 to 2016. We compared these flares to the HSBs determined using two 
 different methods. One uses the polarity change at the Earth to estimate w
 hen the HSB was at solar central meridian and the other uses Potential Fie
 ld Source Surface (PFSS) extrapolations to identify the HSB for all times.
  We found that for both Cycle 23 and 24 more than 40% of non-limb flares w
 ere located near a HSB\, a correlation that varies with cycle phase and he
 misphere. I will describe how this evolves with time and the potential of 
 these approaches for assisting flare forecasting. We then used the locatio
 ns of HSBs calculated with the first method\,using Earth-based data\, to a
  Carrington rotation system and comparedthem with the migration paths of A
 ctive Longitudes as show in Gyenge et al. (2016). We found that there are 
 times where they overlap\, but that is not happening in a consistent manne
 r. They often move at different rates relative to each other (and the Carr
 ington solar rotation rate) and these vary over each Cycle.\nVortragende(r
 ): Konstantina Loumou 
LAST-MODIFIED:20260220T073512Z
LOCATION:University of Glasgow (broadcasted at MPS)\, Raum: Auditorium
ORGANIZER;CN=Andreas Lagg:mailto:
SUMMARY:ESPOS: ESP Online Seminar: The association of RHESSI flares to the 
 Hale Sector Boundary and Active Longitudes (K. Loumou)
URL;VALUE=URI:https://www.mps.mpg.de/events/16967/7840830
END:VEVENT
END:VCALENDAR