NAM2019
  • NAM2019
    • Registration
    • Key Dates & Outline Schedule
    • Practical Information
    • Exhibitors
    • Grants & Bursaries
    • Contacts
  • Science
    • Science Programme
    • Parallel Sessions
    • Plenary Talks
    • Community Session
    • Special Lunches
    • Posters
    • Presenter Guidelines
  • Social
    • What's On
    • Welcome Reception
    • RAS Awards Dinner
  • Media
  • Outreach
    • Outreach and Education Day
    • Fringe Event
    • School Visit Day
  • Lancaster
    • Travel
    • Accommodation
    • Childcare
    • Campus Map
    • About Lancaster
    • Code of Conduct
  • NAM2019
    • Registration
    • Key Dates & Outline Schedule
    • Practical Information
    • Exhibitors
    • Grants & Bursaries
    • Contacts
  • Science
    • Science Programme
    • Parallel Sessions
    • Plenary Talks
    • Community Session
    • Special Lunches
    • Posters
    • Presenter Guidelines
  • Social
    • What's On
    • Welcome Reception
    • RAS Awards Dinner
  • Media
  • Outreach
    • Outreach and Education Day
    • Fringe Event
    • School Visit Day
  • Lancaster
    • Travel
    • Accommodation
    • Childcare
    • Campus Map
    • About Lancaster
    • Code of Conduct

Wednesday

Schedule

id
date time
AM
09:00
Abstract
Photospheric geometry and the ability to gauge active region magnetic field structure during flux emergence
Wednesday

Abstract details

id
Photospheric geometry and the ability to gauge active region magnetic field structure during flux emergence
Date Submitted
2019-03-19 11:52:29
Christopher
Prior
Durham University
Active Region Laboratories
Invited
Prior C (Durham) MacTaggart D (Glasgow)
Flux emergence is a crucial source of complex magnetic field structure in the corona. State of the art simulations indicate emergence is a vital mechanism behind phenomena such as coronal heating, jets, flaring and CME's. Observationally the most reliable information on the magnetic field structure emerging into this region is through photospheric magnetograms (standard and vector). In comparing simulated and observational emerging magnetogram data there are often significant differences in the variation in magnetic field structure; primarily that the helicity input of observational data shows far more variation than the simulations (which often focus on idealised twisted flux rope emergence). In an attempt to characterise the variation in helicity input structure we have preformed simulations of mixed helicity flux rope structures emerging into the corona; this includes fields with helicity across varying spatial scales. One crucial aspect of this study was an attempt to characterise effect on the helicity input due to the variation in geometry of the simulation's photosphere, represented by a fixed density value. It is found this effect is significant, highlighting the fact that the ability of future missions such as DKIST to resolve the variation in field structure across the photosphere could have a critical impact on our ability to determine what kind of magnetic field structure the sun is transporting into its corona.

RAS Logo

Lancaster University Logo

STFC logo

Science Programme

  • Monday
  • Tuesday
  • Wednesday
  • Thursday
  • Posters

All attendees are expected to show respect and courtesy to other attendees and staff, and to adhere to the NAM Code of Conduct. To report harassment or violation of the code of conduct please click here.

© 2023 Royal Astronomical Society

Login