Οι ηλιακές παρατηρήσεις υποβαθμίζονται εξαιτίας του φαινομένου του seeing το οποίο σχετίζεται με τις διαταραχές της γήινης ατμόσφαιρας. Για να μελετήσουμε τις λεπτές δομές της ηλιακής επιφάνειας είναι απαραίτητο να εφαρμόσουμε τεχνικές που ενισχύουν τις εικόνες και βελτιώνουν την ορατότητα τους. Επιπλέον, πολλοί από αυτούς τους σχηματισμούς βρίσκονται «κρυμμένοι» μέσα στο υπόβαθρο και πρέπει να διαχωριστούν από αυτό. Σε αυτήν τη διατριβή περιγράφονται τεχνικές που χρησιμοποιούνται για να βελτιωθεί η ορατότητα ηλιακών σχηματισμών διαφορετικών κατηγοριών όπως κηλίδες, λεπτοί σχηματισμοί κοντά στο χείλος και βόμβες Ellerman. Εκμεταλλευόμενοι την ανάλυση πολλαπλής διακριτικής ικανότητας που παρέχουν τα κυματίδια, εφαρμόζουμε αυτό το είδος ανάλυσης σε εικόνες από την ηλιακή επιφάνεια. Ο αλγόριθμος κυματιδίων à trous χρησιμοποιήθηκε ως ο πιο κατάλληλος μετασχηματισμός κυματιδίων. Οι εικόνες ενισχύθηκαν επιτυχώς και οι συγκεκριμένες τεχνικές αποδείχτηκαν πραγματικά αποδοτικές. Αυτές οι τεχνικές μπορεί να βασίστηκαν στον μετασχηματισμό à trous αλλά τροποποιήθηκαν κατάλληλα, ανάλογα με την συγκεκριμένη εφαρμογή. Θα πρέπει να διευκρινίσουμε ότι οι τεχνικές στις οποίες αναφερόμαστε εξαρτώνται κατά πολύ από το πρόβλημα που έχουμε να αντιμετωπίσουμε. Από την άλλη μεριά, οι ηλιακές παρατηρήσεις είναι χρονικές ακολουθίες εικόνων. Έτσι έχουμε να αντιμετωπίσουμε την ανάλυση χρονικών σειρών δεδομένου ότι θέλουμε να μελετήσουμε την χρονική συμπεριφορά και την εξέλιξη των παρατηρούμενων ηλιακών δομών. Αναλύοντας μια χρονική ακολουθία στο χρονο-συχνοτικό χώρο, μπορεί κανείς να προσδιορίσει τον κύριο τρόπο μεταβλητότητας αλλά και πως αυτοί οι τρόποι αλλάζουν με τον χρόνο. Εκμεταλλευόμαστε αυτή την ιδιότητα των κυματιδίων για να εξετάσουμε την χρονική μεταβολή της περιόδου των ταλαντώσεων της σκιάς των κηλίδων χρησιμοποιώντας παρατηρήσεις της ηλιακής ατμόσφαιρας οι οποίες έχουν ληφθεί από γήινα τηλεσκόπια. Χρησιμοποιούμε αυτό το σήμα του πραγματικού κόσμου για να δοκιμάσουμε τις δυνατότητες διαφορετικών κυματιδίων και για να δούμε τι προβλήματα ανακύπτουν αναλύοντας ένα τέτοιο σήμα. Στην μελέτη μας χρησιμοποιούμε τον συνεχή μετασχηματισμό κυματιδίων και τον αλγόριθμο à trous ως detrending εργαλείο. vii Αναφερόμαστε επιγραμματικά σε προηγούμενες μελέτες οι οποίες βασίζονται στις κλασσικές μεθόδους ανάλυσης σήματος ώστε να μπορέσουμε να καταλάβουμε τι μπορούν να προσφέρουν τα κυματίδια στην ηλιακή φυσική. Τα αποτελέσματα μπορούν να συνοψιστούν στα ακόλουθα: τα κυματίδια είναι ένα ισχυρότατο εργαλείο της ανάλυσης σήματος ακόμη και για τους ηλιακούς φυσικούς και θα μας απασχολήσουν πολύ στο μέλλον και στην μελέτη εικόνων της ηλιακής επιφάνειας. / Solar observations are usually degraded due to seeing effects related to the turbulence of earth’s atmosphere. In order to study the fine structure of the solar surface it is necessary to apply techniques that enhance the images and improve the visibility of fine structures. Moreover many of those structures are embedded in the background and we need separate them from it. In this thesis we describe techniques that are used in order to improve the visibility of several categories of solar features like sunspots, fine structures near the limb and Ellerman bombs. Taking advantage of the multiresolution analysis that provides wavelets, we perform that kind of analysis to images from solar atmosphere. The à trous wavelet algorithm has been used as the proper wavelet transform. The images were successfully enhanced and those techniques have been proved really efficient. Those enhancement techniques were based to the à trous wavelet transform but they were modified properly depending on the specific application. We must clarify that the discussed techniques depend by far on the problem we have to deal with. On the other hand, solar observations are time sequences of images. So we have to deal with time series analysis provided that one wants to study the temporal behavior and evolution of the observed solar structures. By decomposing a time series into time-frequency space, one is able to determine both the dominant mode of variability and how those modes vary in time. We take advantage of this property of the wavelet analysis in order to examine the temporal variation of the period of the umbral oscillations using ground–based observations of the solar atmosphere. We use this real-life signal in order to test the capabilities of different wavelets and to see the problems that arise analyzing such a signal. In our study we use the continuous wavelet transform in order to perform the analysis and the “à trous” algorithm as a detrending tool. We make slightly reference to previous works based on classical methods of signal analysis just to be able to understand what wavelets can offer in solar physics. The results can be summarized as follows: wavelets are a powerful tool for signal analysis even for solar scientists and will preoccupy us a lot in the future and for the study of the solar surface.

The Sun is of fundamental importance to life on earth and is studied by scientists from many disciplines. It exhibits phenomena on a wide range of observable scales, timescales and wavelengths and due to technological developments there is a continuing increase in the rate at which solar data is becoming available for study which presents both opportunities and challenges. Two satellites recently launched to observe the sun are STEREO (Solar TErrestrial RElations Observatory), providing simultaneous views of the SUN from two different viewpoints and SDO (Solar Dynamics Observatory) which aims to study the solar atmosphere on small scales and times and in many wavelengths. The STEREO and SDO missions are providing huge volumes of data at rates of about 15 GB per day (initially it was 30 GB per day) and 1.5 terabytes per day respectively. Accessing these huge data volumes efficiently at both high spatial and high time resolutions is important to support scientific discovery but requires increasingly efficient tools to browse, locate and process specific data sets. This thesis investigates the development of new technologies for processing information contained in multiple and overlapping images of the same scene to produce images of improved quality. This area in general is titled Super Resolution (SR), and offers a technique for reducing artefacts and increasing the spatial resolution. Another challenge is to generate 3D images such as Anaglyphs from uncalibrated pairs of SR images. An automated method to generate SR images is presented here. The SR technique consists of three stages: image registration, interpolation and filtration. Then a method to produce enhanced, near real-time, 3D solar images from uncalibrated pairs of images is introduced. Image registration is an essential enabling step in SR and Anaglyph processing. An accurate point-to-point mapping between views is estimated, with multiple images registered using only information contained within the images themselves. The performances of the proposed methods are evaluated using benchmark evaluation techniques. A software application called the SOLARSTUDIO has been developed to integrate and run all the methods introduced in this thesis. SOLARSTUDIO offers a number of useful image processing tools associated with activities highly focused on solar images including: Active Region (AR) segmentation, anaglyph creation, solar limb extraction, solar events tracking and video creation.

The Sun is of fundamental importance to life on earth and is studied by scientists from many disciplines. It exhibits phenomena on a wide range of observable scales, timescales and wavelengths and due to technological developments there is a continuing increase in the rate at which solar data is becoming available for study which presents both opportunities and challenges. Two satellites recently launched to observe the sun are STEREO (Solar TErrestrial RElations Observatory), providing simultaneous views of the SUN from two different viewpoints and SDO (Solar Dynamics Observatory) which aims to study the solar atmosphere on small scales and times and in many wavelengths. The STEREO and SDO missions are providing huge volumes of data at rates of about 15 GB per day (initially it was 30 GB per day) and 1.5 terabytes per day respectively. Accessing these huge data volumes efficiently at both high spatial and high time resolutions is important to support scientific discovery but requires increasingly efficient tools to browse, locate and process specific data sets. This thesis investigates the development of new technologies for processing information contained in multiple and overlapping images of the same scene to produce images of improved quality. This area in general is titled Super Resolution (SR), and offers a technique for reducing artefacts and increasing the spatial resolution. Another challenge is to generate 3D images such as Anaglyphs from uncalibrated pairs of SR images. An automated method to generate SR images is presented here. The SR technique consists of three stages: image registration, interpolation and filtration. Then a method to produce enhanced, near real-time, 3D solar images from uncalibrated pairs of images is introduced. Image registration is an essential enabling step in SR and Anaglyph processing. An accurate point-to-point mapping between views is estimated, with multiple images registered using only information contained within the images themselves. The performances of the proposed methods are evaluated using benchmark evaluation techniques. A software application called the SOLARSTUDIO has been developed to integrate and run all the methods introduced in this thesis. SOLARSTUDIO offers a number of useful image processing tools associated with activities highly focused on solar images including: Active Region (AR) segmentation, anaglyph creation, solar limb extraction, solar events tracking and video creation.

Yes / This paper presents a new method that provides the means to detect sunspots on full-disk solar images recorded by the Solar Diameter Imager and Surface Mapper (SODISM) on the PICARD satellite. The method is a totally automated detection process that achieves a sunspot recognition rate of 97.6%. The number of sunspots detected by this method strongly agrees with the NOAA catalogue. The sunspot areas calculated by this method have a 99% correlation with SOHO over the same period, and thus help to calculate the filling factor for wavelength (W.L.) 607nm.

Yes / The surface of the sun often shows visible sunspots which are located in magnetically active regions of the Sun, and whose number is an indicator of the Sun’s magnetic activity. The detection and classification of sunspots are useful techniques in the monitoring and prediction of solar activity. The automated detection of sunspots from digital images is complicated by their irregularities in shape and variable contrast and intensity compared with their surrounding area. The main aim of this paper is to detect sunspots using images from the Solar Diameter Imager and Surface Mapper (SODISM) on the PICARD satellite and calculate their filling factors. A comparison over time with sunspot numbers obtained using images from the SOHO satellite is also presented.

No / The Solar Feature Catalogues (SFCs) are created from digitized solar images using automated pattern recognition techniques developed in the European Grid of Solar Observation (EGSO) project. The techniques were applied for detection of sunspots, active regions and filaments in the automatically standardized full-disk solar images in Caii K1, Caii K3 and H¿ taken at the Meudon Observatory and white-light images and magnetograms from SOHO/MDI. The results of automated recognition are verified with the manual synoptic maps and available statistical data from other observatories that revealed high detection accuracy. A structured database of the Solar Feature Catalogues is built on the MySQL server for every feature from their recognized parameters and cross-referenced to the original observations. The SFCs are published on the Bradford University web site http://www.cyber.brad.ac.uk/egso/SFC/ with the pre-designed web pages for a search by time, size and location. The SFCs with 9 year coverage (1996¿2004) provide any possible information that can be extracted from full disk digital solar images. Thus information can be used for deeper investigation of the feature origin and association with other features for their automated classification and solar activity forecast.

Yes / PICARD is a space-based observatory hosting the Solar Diameter Imager and Surface Mapper (SODISM) telescope, which has continuously observed the Sun from July 2010 and up to March 2014. In order to study the fine structure of the solar surface, it is helpful to apply techniques that enhance the images so as to improve the visibility of solar features such as sunspots or faculae. The objective of this work is to develop an innovative technique to enhance the quality of the SODISM images in the five wavelengths monitored by the telescope at 215.0 nm, 393.37 nm, 535.7 nm, 607.1 nm and 782.2 nm. An enhancement technique using interpolation of the high-frequency sub-bands obtained by Discrete Wavelet Transforms (DWT) and the input image is applied to the SODISM images. The input images are decomposed by the DWT as well as Stationary Wavelet Transform (SWT) into four separate sub-bands in horizontal and vertical directions namely, low-low (LL), low-high (LH), high-low (HL) and high–high (HH) frequencies. The DWT high frequency sub-bands are interpolated by a factor 2. The estimated high frequency sub-bands (edges) are enhanced by introducing an intermediate stage using a stationary Wavelet Transform (SWT), and then all these sub-bands and input image are combined and interpolated with half of the interpolation factor α/2, used to interpolate the high-frequency sub-bands, in order to reach the required size for IDWT processing. Quantitative and visual results show the superiority of the proposed technique over a bicubic image resolution enhancement technique. In addition, filling factors for sunspots are calculated from SODISM images and results are presented in this work.