Tese de mestrado. Engenharia de Minas de Geo-Ambiente. Universidade do Porto. Faculdade de Engenharia. 2012

Trabalho realizado na Adclick, orientado pelo Engº Pedro Roque / Tese de mestrado integrado. Engenharia Industrial e Gestão. Faculdade de Engenharia. Universidade do Porto. 2012

Tese de mestrado. Mestrado integrado em Engenharia Mecânica. Faculdade de Engenharia. Universidade do Porto. 2012

Tese de mestrado. Mestrado Integrado em Engenharia Civil - Especialização em Estruturas. Faculdade de Engenharia. Universidade do Porto. 2012

<p>Unlicensed Mobile Access (UMA) provides transparent access to 2G and 3G networks for Mobile Stations over the unlicensed radio interface. Unlicensed radio tehnologies such as Bluetooth or WLAN technology connects the Mobile Station to the fixed IP network of the home or office and delivers high bandwith to the Mobile Station.</p><p>The purpose of this report is to examine if subscribers can feel as secure using UMA as they do when using any of the alternetive mobile technologies that UMA supports. The security evaluation is performed by first investigating the current security level of GSM, GPRS and UMTS and then compares them to the security mechanisms of UMA.</p><p>This evaluation noticed two distinct flaws in UMA that could compromise security. The conclusion is that these flaws do not have a major inpact and UMA does provide a general higher level of security than the 2G and 3G counterparts.</p>

Unlicensed Mobile Access (UMA) provides transparent access to 2G and 3G networks for Mobile Stations over the unlicensed radio interface. Unlicensed radio tehnologies such as Bluetooth or WLAN technology connects the Mobile Station to the fixed IP network of the home or office and delivers high bandwith to the Mobile Station. The purpose of this report is to examine if subscribers can feel as secure using UMA as they do when using any of the alternetive mobile technologies that UMA supports. The security evaluation is performed by first investigating the current security level of GSM, GPRS and UMTS and then compares them to the security mechanisms of UMA. This evaluation noticed two distinct flaws in UMA that could compromise security. The conclusion is that these flaws do not have a major inpact and UMA does provide a general higher level of security than the 2G and 3G counterparts.

Η μελέτη των διπλών εκλειπτικών συστημάτων παραμένει ένα από τα πιο ενδιαφέροντα ερευνητικά πεδία της αστροφυσικής γιατί παρέχει την πιο ακριβή μέθοδο υπολογισμού των βασικών αστρικών μεγεθών (μαζών, ακτίνων, θερμοκρασιών) αλλά και κάθε μορφής αστρικής δραστηριότητας που αναπτύσσεται (κηλίδες, δίσκοι προαύξησης ύλης, αναπάλσεις) μέσα από τη μακρόχρονη μεταβολή της περιόδου τους. Επιπλέον επιτρέπει τον έλεγχο των θεωριών αστρικής εξέλιξης μέσα από την αλληλεπίδρασή τους αλλά και την πρόβλεψη παρουσίας τρίτων σωμάτων αστρικής ή μη φύσης. Σε αυτήν τη διατριβή μελετάται μία ιδιαίτερη κατηγορία διπλών εκλειπτικών συστημάτων σε επαφή, τα W UMa τα οποία αποτελούνται από αστέρες κύριας ακολουθίας οι οποίοι βρίσκονται σε υπερεπαφή, και χαρακτηρίζονται από τις μικρότερες περιόδους κι άρα από τη μικρότερη στροφορμή. Σκοπός της είναι τόσο η παρατηρησιακή μελέτη και ανάλυση συστημάτων W UMa που παρουσιάζουν ιδιαίτερο ενδιαφέρον όσο και η ανάγκη ανάπτυξης μεθοδολογίας μοντελοποίησης για την εξαγωγή της μέγιστης πληροφορίας και ελέγχου των εξαγόμενων φυσικών παραμέτρων κάτω από την εφαρμογή σύγχρονων στατιστικών μεθόδων. Το πρώτο μέρος της επικεντρώνεται στη σκιαγράφηση του θεωρητικού επιστημονικού πλαισίου περιγραφής των διπλών εκλειπτικών αστρικών συστημάτων σε επαφή. Το Κεφάλαιο1 αναφέρεται στη γεωμετρία των τροχιών και στη φυσική των αστέρων του συστήματος, στην περιγραφή του μοντέλου Roche και στην αλληλεπίδραση των μελών καθώς και στη δυναμική των συστημάτων όπως αυτή εκδηλώνεται από την παρατηρούμενη μεταβολή της περιόδου του. Το Κεφάλαιο 2 αναφέρεται στις φωτομετρικές παρατηρήσεις που έγιναν κατά την διάρκεια της παρούσας διατριβής καθώς και στις αυτοματοποιημένες μεθόδους επεξεργασίας και ανάλυσης των παρατηρησιακών αστρονομικών δεδομένων οι οποίες αναπτύχθηκαν. Το Κεφάλαιο 3 περιγράφει τις σύγχρονες τεχνικές μοντελοποίησης και τα προγράμματα ανάλυσης για τηλύση του αντίστροφου προβλήματος. Το Κεφάλαιο 4 περιγράφει την αναζήτηση, εξόρυξη και αυτόματη ανάλυση δεδομένων από παρατηρησιακές αστρονομικές επισκοπήσεις και την εφαρμογή του κώδικα τεχνητών νευρωνικών δικτύων EBAI. Το δεύτερο μέρος επικεντρώνεται στην αναλυτική μελέτη επιλεγμένων στενών διπλών συστημάτων W UMa με ιδιαίτερο ενδιαφέρον. Σε όλα τα επιλεγμένα συστήματα παρουσιάζεται η φωτομετρική τους μελέτη κάτω από το φως νέων BV RcIc παρατηρήσεων, η μελέτη της περιόδου, το εξαγόμενο μοντέλο σε συνδυασμό με φασματοσκοπικά δεδομένα, ο προσδιορισμός τροχιακών και φυσικών παραμέτρων και η θέση τους σε εξελικτικά διαγράμματα. Επίσης γίνεται η διερεύνηση του προτεινόμενου μοντέλου για μοναδικότητα στο χώρο των λύσεων μέσα από σάρωση με εισαγωγή διαταραχών ή άλλων στατιστικών μεθόδων και ο στατιστικός προσδιορισμός των σφαλμάτων των παραμέτρων. Συγκεκριμένα στο Κεφάλαιο5 παρουσιάζεται το ενοποιημένο μοντέλο του συστήματος TY Boo δύο κηλίδων που ερμηνεύει τη συμπεριφορά του την περίοδο 1969-2011 και τη μελέτη της περιόδου του. Σύμφωνα με αυτό το σύστημα TY Boo ανήκει στην υποκατηγορία W των W UMa με μικρό βαθμό επαφής f = (7.6 ±0.8)% και η μακρόχρονη μελέτη της περιόδου του δείχνει μακροχρόνια μείωση (dP/dt = −3.65x10^−8 d yr^−1 ) και μία περιοδικότητα (P3 = 58.9yrs, A = 0.0254 days)η οποία, χωρίς να αποκλείεται η παρουσία τρίτου σώματος, ερμηνεύεται με ενεργό μαγνητικό κύκλο που προκαλεί την εμφάνιση κηλίδων.Στο Κεφάλαιο 6 παρουσιάζεται για πρώτη φορά η λεπτομερής ανάλυση του συστήματος WUMa, FI Boo το οποίο ταξινομείται στην υποκατηγορία W, με βαθμό επαφής f = (50.15 ±8.10) %, κάτω από την παρουσία τρίτου σώματος το οποίο μπορεί να παίζει σημαντικό ρόλο στη δημιουργία και την εξέλιξή του. Σύμφωνα με το προτεινόμενο μοντέλο προσδιορίζονται οι μάζες Mh =0.40 ± 0.05 Msun , Mc =1.07 ± 0.05 Msun , και οι θερμοκρασίες Th = 5746±33Κ, Tc = 5420±46 Κ των αστέρων-μελών του καθώς και των προγεννητόρων τους (1.71 ±0.10 Msun και 0.63 ± 0.01 Msun , αντίστοιχα) και διερευνάται το εξελικτικό στάδιο του αστέρα με τη μεγαλύτερη μάζα μέσα από ισόχρονες.Στο Κεφάλαιο 7 διερευνάται σε βάθος το σύστημα σε επαφή V1003 Her, το οποίο χαρακτηρίζεται από μεταβολή μικρού πλάτους, με πολλαπλά μοντέλα για τα οποία ελέγχεται η σταθερότητα των με ανεξάρτητες μεθόδους. Το επικρατέστερο από αυτά δείχνει ότι το σύστημα είναι W UMa με βαθμό επαφής f = (36±10) %, με ασυνήθιστα άνισες θερμοκρασίες μεταξύ των αστέρων του 550 Κ, και λόγο μαζών q = 0.373. Η μικρή του κλίση i = 38^o ±1^ο το καθιστά ένα από τα μεγαλύτερης μάζας στην υποκατηγορίας W.Στο Κεφάλαιο 8 εξετάζεται η φύση του διπλού συστήματος HI Dra, η λεπτομερής ανάλυση του οποίου δείχνει ότι είναι W UMa με μικρό βαθμό επαφής f = (24 ± 4) % και διαφορά θερμοκρασίας μεταξύ των αστέρων του 330 Κ. Προτείνονται και διερευνώνται εξονυχιστικά δύο μοντέλα με κηλίδες από τα οποία επικρατέστερο, με ψυχρή κηλίδα πάνω στον μικρότερης μάζας και ψυχρότερο αστέρα- τον τοποθετεί στην υποκατηγορία Α. Προσδιορίζονται οι φυσικές παράμετροι των μελών του (M = 1.72 ± 0.08Msun , Mc = 0.43 ± 0.02 Msun , Rh =1.98 ± 0.03Rsun , Rc = 1.08 ± 0.02 Rsun , Lh = 9.6 ± 0.1 Lsun , Lc = 2.4 ± 0.1 Lsun ) και των προγεννητόρων τους (1.11 ± 0.03 Msun και 2.25 ± 0.07 Msun, αντίστοιχα) και προσεγγίζεται η ηλικία του συστήματος σε 2.4 Gyr .Τέλος στο Κεφάλαιο 8 παρουσιάζονται τα πρώτα αποτελέσματα από τις φωτομετρικές παρατηρήσεις με το τηλεσκόπιο Αρίσταρχος 2.3 m, διπλών εκλειπτικών συστημάτων με ιδιαίτερο ενδιαφέρον που ανακαλύφθηκαν ή παρατηρήθηκαν από την διαστημική αποστολή Kepler με περιόδους περιφοράς < 0.45 d, τα οποία παρουσιάζουν ασυμμετρίες στην καμπύλη φωτός, χρονικές μεταβολές των εκλείψεων των μελών τους ή είναι εν δυνάμει τριπλά συστήματα. Τα πρώτα αποτελέσματα αφορούν τα συστήματα KIC 11246163 και KIC 4563150τα οποία ταξινομούνται ως συστήματα τύπου W UMa, W υποκατηγορίας με πιθανό τριτο συνοδό. / The study of eclipsing binary systems remains one of the most powerful research fields in stellar astrophysics because it provides the primary source of calculating fundamentals properties of stars (masses, radii, temperatures) and every form of stellar activity (spots, accreting discs, pulsations) through photometry and spectroscopy or/and through the study of long-term variability of their period. Additionally it allows testing of stellar structure and evolution theories and the prediction of third body companions of stellar or sub-stellar origin. This thesis is focused on the study of W UMa type eclipsing binaries containing main sequence stars in overcontact configuration with short periods and,therefore the small angular momentum. The aim is both the multiband observational study, analysis and investigation of WUMa systems of particular interest but also the development of modeling methodology in order to extract the maximum information and to determine a detailed assessment of the parameter uncertainties through the application of modern statistical methods. The first part of the Doctoral Thesis outlines the theoretical framework for describing eclipsing binary stars. Chapter 1 refers to the physics and geometry of orbits and components, the description of the Roche model that led to the classification based on equipotential surfaces, the computation of the total radiated flux in the direction of the observer by including all the corrections needed and the description of systems dynamics as manifested by the observed change of their period. Chapter2 presents the photometric observations made during this research and the automated methods of processing and analysis (pipelines) which were developed. Chapter 3 sketches the modern modeling and analysis software techniques for the solution of inverse problem(Differential Corrections, Levenberg-Marquardt, Downhill Simplex, Genetic Algorithms,Heuristic Scanning, Bootstrap resampling, Metropolis –Hasting Markov Chain MonteCarlo), their implementation to programs developed as part of the present thesis and their application to real data. These also represent the methodology of the analyses implemented for the study of the WUMa systems, described in Part 2. Finally, Chapter4 describes the development of a pipeline for the exploration, extraction and automatic analysis of data from astronomical surveys and its application to ASAS database. In the same chapter the first results from the training and validation of the Artificial Neural Network (ANN), EBAI, and the best topology for the ANN are presented.The second part focuses on the detailed study of selected W UMa systems with particular interest. This includes: the new multiband photometric observations, the longterm period variation, the exported model from photometric and spectroscopic data (from the literature), the determination of orbital and physical parameters and their position in evolutionary diagrams, the investigation of the proposed model for uniqueness in the parameter space through heuristic scanning with parameter kicking or other statistical methods- and the statistical determination of the uncertainties of the derived parameters.In Chapter 5, new CCD four-color light curves of TY Boo made on eight nights over2010–2011 were analyzed in comparison with historical light curves obtained from 1969through 2011. The light curves could all be represented by a unique geometry and by wavelength consistent phototometric parameters of a two-spot model on either stellar component. It is confirmed that TY Boo is a shallow W-type contact binary system with a degree of contact factor of f = 7.6 ± 0.8%. A period investigation based on all available data shows a long-term decrease (dP/dt = −3.65 ×10−8 days yr−1 ) and an oscillation (P3 = 58.9 yr, A = 0.0254 days). Without ruling out the presence of a tertiary companion, the weight of evidence points to an active cyclic magnetic activity that causes spot formation rather than an unseen companion. Mass transfer between the components and angular momentum loss are also considered as possible mechanisms.In Chapter 6, a detailed analysis of the interesting W UMa binary FI Boo in view of the spectroscopic signature of a third body through photometry, period variation, and a thorough investigation of solution uniqueness is presented. We obtained new BVRcIc photometric data that, when combined with spectroscopic data, enable us to analyze the system FI Boo and determine its basic orbital and physical properties through PHOEBE,as well as the period variation by studying the times of the minima. This combined approach allows us to study the long-term period changes in the system for the first time in order to investigate the presence of a third body and to check extensively the solution uniqueness and the uncertainties of derived parameters. Our modeling indicates that FIBoo is a W-type moderate (f = 50.15% ± 8.10%) overcontact binary with component masses of Mh = 0.40 ± 0.05 M and Mc =1.07 ± 0.05 M , temperatures of Th = 5746 ±33 K and Tc = 5420 ± 56 K, and a third body, which may play an important role in the formation and evolution. The results were tested by heuristic scanning and parameter kicking to provide the consistent and reliable set of parameters that was used to obtain the initial masses of the progenitors (1.71 ± 0.10 M and 0.63 ± 0.01 M , respectively). We also investigated the evolutionary status of massive components with several sets of widely used isochrones.In Chapter 7, an extensive analysis of the low amplitude, contact binary V1003 Her is presented, based on the new VRc Ic , CCD photometric light curves in combination with published radial velocity (RV) curves. We investigate the stable configurations for the system with two independent methods and modeling tools: PHOEBE, ROCHE, via heuristic scanning and genetic algorithms, although the very low inclination of the system can place limitations. All methods indicate that V1003 Her is most likely in overcontact state with unequal components with temperature difference of 550 K, a mass ratio of q= 0.373 and a contact degree of 36 ± 10 %. As it is viewed at the very low inclination of i ∼ 38^◦ ± 1^◦ , if its configuration is confirmed, it will be among the most massive W-subtype of W UMa systems. This conclusion is also supported by other published models.However, in order to conclude reliable physical properties of the system, the high-precise based-ground photometry (or satellite photometry) and spectroscopic follow-up of V1003Her is required.In Chapter 8, a detailed investigation of the low-amplitude contact binary HI Dra is presented, based on the new VRc Ic CCD photometric light curves (LCs) combined with published radial velocity (RV) curves. Our completely covered LCs were analyzed using PHOEBE and revealed that HI Dra is an overcontact binary with low fill-out factor f = 24 ± 4 (%) and temperature difference between the components of 330 K.Two spotted models are proposed to explain the LC symmetry, between which the A subtype of W UMa type eclipsing systems, with a cool spot on the less massive and cooler component, proves to be more plausible on evolutionary grounds. The results and stability of the solutions were explored by heuristic scan and parameter perturbation to provide a consistent and reliable set of parameters and their errors. Our photometric modeling and RV curve solution give the following absolute parameters of the hot and cool components, respectively: Mh = 1.72 ± 0.08 Msun and Mc = 0.43 ± 0.02 Msun , Rh =1.98 ± 0.03 Rsun and Rc = 1.08 ± 0.02 Rsun , and Lh = 9.6 ± 0.1 Lsun and Lc = 2.4 ± 0.1Lsun . Based on these results the initial masses of the progenitors (1.11 ± 0.03 Msun and2.25 ± 0.07 Msun , respectively) and a rough estimate of the age of the system of 2.4 Gyr are discussed.Finally, in Chapter 9, our first results from ground based follow up photometric observation of interesting eclipsing binary systems (EBs) from Kepler field are presented.The program was launched in 2013 with the 2.3 m Aristarchos telescope at Helmos Observatory, Greece including eclipsing binary systems with periods < 0.45d and Kp (mag)=12.6-16 mag. The included targets in this program show light curve asymmetries,Eclipse Timings Variation or they are third body candidates. Modern analysis techniques such as heuristic scanning with parameter perturbation and genetic algorithm(PIKAIA), enable to reveal and optimize the astrophysical parameters of selected EBs.The results from BVRI photometry for the third body candidates, WUMa eclipsing binary systems of W-subtype, KIC11246163 and KIC4563150, are presented for the first time, as well as conclusions derived so far.

A trend in parallel computer architecture is that systems with a large shared memory are becoming more and more popular. A shared memory system can be either a uniform memory architecture (UMA) or a cache coherent non-uniform memory architecture (cc-NUMA). In the present thesis, the performance of parallel PDE solvers on cc-NUMA computers is studied. In particular, we consider the shared namespace programming model, represented by OpenMP. Since the main memory is physically, or geographically distributed over several multi-processor nodes, the latency for local memory accesses is smaller than for remote accesses. Therefore, the geographical locality of the data becomes important. The focus of the present thesis is to study multithreaded PDE solvers on cc-NUMA systems, in particular their memory access pattern with respect to geographical locality. The questions posed are: (1) How large is the influence on performance of the non-uniformity of the memory system? (2) How should a program be written in order to reduce this influence? (3) Is it possible to introduce optimizations in the computer system for this purpose? The main conclusion is that geographical locality is important for performance on cc-NUMA systems. This is shown experimentally for a broad range of PDE solvers as well as theoretically using a model involving characteristics of computer systems and applications. Geographical locality can be achieved through migration directives that are inserted by the programmer or — possibly in the future — automatically by the compiler. On some systems, it can also be accomplished by means of transparent, hardware initiated migration and replication. However, a necessary condition that must be fulfilled if migration is to be effective is that the memory access pattern must not be "speckled", i.e. as few threads as possible shall make accesses to each memory page. We also conclude that OpenMP is competitive with MPI on cc-NUMA systems if care is taken to get a favourable data distribution.

Submitted by Diana Alves (ppgdancaufba.adm@gmail.com) on 2018-04-02T14:14:19Z No. of bitstreams: 1 01.ARQUIVO_01_DISSERTAÇAO_SONIA_GONÇALVES.pdf: 284062884 bytes, checksum: 6df3767e72a56feb117758a4f29719ed (MD5) / Approved for entry into archive by Setor de Periódicos (per_macedocosta@ufba.br) on 2018-04-03T18:43:34Z (GMT) No. of bitstreams: 1 01.ARQUIVO_01_DISSERTAÇAO_SONIA_GONÇALVES.pdf: 284062884 bytes, checksum: 6df3767e72a56feb117758a4f29719ed (MD5) / Made available in DSpace on 2018-04-03T18:43:34Z (GMT). No. of bitstreams: 1 01.ARQUIVO_01_DISSERTAÇAO_SONIA_GONÇALVES.pdf: 284062884 bytes, checksum: 6df3767e72a56feb117758a4f29719ed (MD5) / Esta dissertação apresenta uma história do Balé Teatro Castro Alves (BTCA). Buscou traçar um necessário diálogo entre o que é chamado de pesquisa artística e pesquisa acadêmica e intentou tornar esta dicotomia inexistente e assim, portanto, desenvolver uma pesquisa artístico-acadêmica. Ao argumentar que um lugar de fala é sempre envolvido pelo ambiente no qual está inserido (GREINER; KATZ, 2006), um dos objetivos desta história foi trazer, simultaneamente, a experiência de um coletivo formado por bailarinos de uma importante companhia de reconhecimento nacional e internacional, cidadãos da Dança em Salvador, da Bahia e do Brasil. Neste traçado de um longo período foram abordados dados anteriores à criação do BTCA e da Companhia Ilimitada (CI), apresentados alguns fatos da política cultural (da época de fundação do BTCA e da CI). São aqui expostos dados do cotidiano da companhia, diretores, coreógrafos e outros membros, analisados os processos excludentes de bailarinos, seus processos criativos como intérpretes-criadores, suas relações com a comunidade. A trajetória teve como seu agente a noção de corpopassagem, sendo este um corpo que não apenas passa pelos acontecimentos, mas que os experiencia e por isso mesmo os pode narrar (BENJAMIN, 1994). Completando as referências principais Ecléa Bosi (1994) referencia a abordagem do termo “história”. Giorgio Agamben (2010; 2009; 1993) elucida a compreensão do conceito de “exclusão” e Foucault (2013; 2005; 2004) faz entender a disciplina exacerbada com a discussão de um “corpo dócil”. Lenira Rengel (2015; 2007) contribuiu com a noção de “corponectivo”, enquanto corpo não dualista na questão “corpomente”. A história da Dança no Brasil, seja recente ou anterior, carece de dados escritos, iconográficos, relatos, entrevistas com pessoas que são parte desta própria história. A pesquisa traz, portanto, metodologicamente esses procedimentos, junto à pesquisa qualitativa bibliográfica, tendo como metodologia principal a etnografia e a auto etnografia (FORTIN, 2009). Resultados se deram em compilar questões vividas, bem como relatos pessoais que configuram, de fato, uma história, junto a apresentar documentos que, por vezes, são descartados. O BTCA em 2017 continua sua história em intensa tentativa de sobrevivência com produção artísticoacadêmica- social.

MOTA, A. B. Princípios de contagem e aplicação do princípio aditivo: o problema de contagem dos quadrados em uma quadrícula e o código qq. 2017. 77 f. Dissertação (Mestrado Profissional em Matemática) - Departamento de Matemática, Universidade Federal do Ceará, Fortaleza, 2017. / Submitted by Jessyca Silva (jessyca@mat.ufc.br) on 2017-03-13T13:23:42Z No. of bitstreams: 1 2017_dis_abmota.pdf: 1243622 bytes, checksum: 870696f1353ad4f2e4465a68ee6aa95f (MD5) / Approved for entry into archive by Rocilda Sales (rocilda@ufc.br) on 2017-03-14T13:14:14Z (GMT) No. of bitstreams: 1 2017_dis_abmota.pdf: 1243622 bytes, checksum: 870696f1353ad4f2e4465a68ee6aa95f (MD5) / Made available in DSpace on 2017-03-14T13:14:14Z (GMT). No. of bitstreams: 1 2017_dis_abmota.pdf: 1243622 bytes, checksum: 870696f1353ad4f2e4465a68ee6aa95f (MD5) Previous issue date: 2017-02-15 / The present dissertation intends at first to approach the elementary Principles of combinatorics, giving a focus on problem solving without the direct use of ready-made formulas, and in some cases constructing them in order to show that problem solving involving combinatorial requires more of a good idea than of the knowledge of certain standard procedures of resolution. The other point to be highlighted in this work was motivated by a problem seen in a contest of the Federal Institute of Ceará that asked to determine the number of distinct squares, sides not necessarily parallel to the Cartesian axes, whose vertices belong to the set {(a, b); a and b integers, 1≤a≤7; 1≤b≤7}, a problem of counting using the Addition Principle, which will be initiated in this work very simply by points in a line and the count of segments, going through the problem just like the one in the contest but with a grid 10 X 10 until its version in three dimensions with the counting of cubes inserted in it and with the conjecture for n-dimensional spaces. Additionally, an application for this square counting problem is presented in a transformation of these into a read-through type code called by the author of Code QQ (Square squares). / A presente dissertação pretende em um primeiro momento abordar os Princípios elementares de combinatória, com foco na resolução de problemas através da utilização de ferramentas básicas de contagem, e em alguns casos construindo-as de modo a mostrar que a resolução de problemas envolvendo combinatória requer mais de criatividade ao conhecimento de determinados procedimentos padrões de resolução. O outro ponto a se destacar neste trabalho foi motivado por um problema visto em um concurso do Instituto Federal do Ceará de 2016 que pedia para determinar o número de quadrados distintos, de lados não necessariamente paralelos aos eixos cartesianos, cujos vértices pertencem ao conjunto {(a,b); a e b inteiros, 1≤a≤7; 1≤b≤7}. Um problema de contagem utilizando o Princípio da Adição, que será neste trabalho iniciado de forma bem simples por pontos em uma reta e a contagem de segmentos, passando pelo problema tal qual o do concurso pede, mas com uma quadrícula 10 x 10 até sua versão em três dimensões com a contagem de cubos nele inseridos e com a conjectura para espaços n-dimensionais. Além disso, é apresentada uma aplicação para esse problema de contagem de quadrados numa transformação destes em um código do tipo leitura rápida, denominado pelo autor de Código QQ (Quadrados em Quadrículas).