Add to ORKGThis thesis presents an observational analysis of structures in the solar corona. The plasmafl in the corona is low (<I), therefore, the emitting material is intimately linked to the magnetic fleldlines. The initial aim of this work, outlined in Chapter 3, is to take advantage of this relationship to calculate realistic magnetic reconnection rates from EUV observations. Then, Chapters 4-6 concentrate upon examining a colour-colour method to provide temperature profiles of coronal structures. Firstly, TRACE 171 A and 195 A data are used to indirectly determine a magnetic reconnection rate for a flare loop system on the limb of the Sun. The magnetic reconnection rate is calculated by measuring the footpoint velocity of the loop system and fo...
The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photosp...
Understanding coronal heating remains a central problem in solar physics. Many mechanisms have been ...
In solar eruption events, coronal mass ejections (CMEs) and flares often occur, albeit not simultane...
We report an initial study of temperature and emission measure distributions along four steady loops...
Context. Different models for the heating of solar corona assume or predict different locations of t...
The temperature of the Sun's outer atmosphere (the corona) exceeds that of the solar surface by abou...
ABSTRACT Magnetic loops are building blocks of the closed-field corona. While active region loops ar...
In the present work SOHO Coronal Diagnostic Spectrometer (CDS) observations of a quiescent active re...
One of the paradigms about coronal heating has been the belief that the mean or summit temperature o...
In the wake of the 2003 November 4 coronal mass ejection associated with the largest solar flare of ...
Magnetic loops are building blocks of the closed-field corona. While active region loops are readily...
Magnetic loops are building blocks of the closed-field corona. While active region loops are readily...
High time resolution Transition Region And Coronal Explorer (TRACE) 171 and 195 Å observations of th...
Context. We investigate the chromospheric counterpart of small-scale coronal loops constituting a co...
One of the paradigms about coronal heating has been the belief that the mean or summit temperature o...
The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photosp...
Understanding coronal heating remains a central problem in solar physics. Many mechanisms have been ...
In solar eruption events, coronal mass ejections (CMEs) and flares often occur, albeit not simultane...
We report an initial study of temperature and emission measure distributions along four steady loops...
Context. Different models for the heating of solar corona assume or predict different locations of t...
The temperature of the Sun's outer atmosphere (the corona) exceeds that of the solar surface by abou...
ABSTRACT Magnetic loops are building blocks of the closed-field corona. While active region loops ar...
In the present work SOHO Coronal Diagnostic Spectrometer (CDS) observations of a quiescent active re...
One of the paradigms about coronal heating has been the belief that the mean or summit temperature o...
In the wake of the 2003 November 4 coronal mass ejection associated with the largest solar flare of ...
Magnetic loops are building blocks of the closed-field corona. While active region loops are readily...
Magnetic loops are building blocks of the closed-field corona. While active region loops are readily...
High time resolution Transition Region And Coronal Explorer (TRACE) 171 and 195 Å observations of th...
Context. We investigate the chromospheric counterpart of small-scale coronal loops constituting a co...
One of the paradigms about coronal heating has been the belief that the mean or summit temperature o...
The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photosp...
Understanding coronal heating remains a central problem in solar physics. Many mechanisms have been ...
In solar eruption events, coronal mass ejections (CMEs) and flares often occur, albeit not simultane...