Photospheric flux density of magnetic helicity

Details Photospheric flux density of magnetic helicity Photospheric flux density of magnetic helicity

Publishing date

Sep 2005

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...439.1191p&link_type=abstract

Journals

Astronomy and Astrophysics, Volume 439, Issue 3, September I 2005, pp.1191-1203

Science

Astronomy and Astrophysics

Field

Astrophysics

Additional info 2

48

Additional info 3

Sun: Magnetic Fields, Sun: Photosphere, Sun: Corona

Type

Scientific paper

Abstract

Several recent studies have developed the measurement of magnetic helicity flux from the time evolution of photospheric magnetograms. The total flux is computed by summing the flux density over the analyzed region. All previous analyses used the density GA (=-2 ( A\cdot {u}) B_n) which involves the vector potential A of the magnetic field. In all the studied active regions, the density GA has strong polarities of both signs with comparable magnitude. Unfortunately, the density GA can exhibit spurious signals which do not provide a true helicity flux density. The main objective of this study is to resolve the above problem by defining the flux of magnetic helicity per unit surface. In a first step, we define a new density, Gθ, which reduces the fake polarities by more than an order of magnitude in most cases (using the same photospheric data as G_A). In a second step, we show that the coronal linkage needs to be provided in order to define the true helicity flux density. It represents how all the elementary flux tubes move relatively to a given elementary flux tube, and the helicity flux density is defined per elementary flux tube. From this we define a helicity flux per unit surface, GΦ. We show that it is a field-weighted average of Gθ at both photospheric feet of coronal connections. We compare these three densities (G_A, Gθ, GΦ) using theoretical examples representing the main cases found in magnetograms (moving magnetic polarities, separating polarities, one polarity rotating around another one and emergence of a twisted flux tube). We conclude that Gθ is a much better proxy of the magnetic helicity flux density than GA because most fake polarities are removed. Indeed Gθ gives results close to GΦ and should be used to monitor the photospheric injection of helicity (when coronal linkages are not well known). These results are applicable to the results of any method determining the photospheric velocities. They can provide separately the flux density coming from shearing and advection motions if plasma motions are known.

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