This thesis work can be framed in a more general concept designated as "high-solution in solar physics". The work consists of two clearly defined parts. The first part concerning instrumental developments for solar observations and the second one devoted to the scientific exploitation of solar data acquired with cutting edge solar instrumentation.
ESA SMOS (Soil Moisture and Ocean Salinity) Mission: Principles of Operation ...adrianocamps
SMOS basic principles and description of some products developed at the SMOS Barcelona Expert Center.
Disclaimer: these materials were prepared for Eduacational purposes only.
Presentation made by Prof. Adriano Camps (Universitat Politècnica de Catalunya) at ICMARS 2010 (India, 16-December-2010) on the MIRAS instrument aboard ESA's SMOS mission.
SIGGRAPH 2014 Course on Computational Cameras and Displays (part 4)Matthew O'Toole
Recent advances in both computational photography and displays have given rise to a new generation of computational devices. Computational cameras and displays provide a visual experience that goes beyond the capabilities of traditional systems by adding computational power to optics, lights, and sensors. These devices are breaking new ground in the consumer market, including lightfield cameras that redefine our understanding of pictures (Lytro), displays for visualizing 3D/4D content without special eyewear (Nintendo 3DS), motion-sensing devices that use light coded in space or time to detect motion and position (Kinect, Leap Motion), and a movement toward ubiquitous computing with wearable cameras and displays (Google Glass).
This short (1.5 hour) course serves as an introduction to the key ideas and an overview of the latest work in computational cameras, displays, and light transport.
A Novel Approach for Ship Recognition using Shape and Texture ijait
Maritime security includes reliable identification of ship entering and leaving a nation’s territorial waters. Sea target detection from remote sensing imagery is very important, with a wide array of applications in areas such as fishery management, vessel traffic services, and naval warfare. Automated systems that could identify a ship could complement existing electronic signal identification methods. A new classification approach using shape and texture is introduced for Ship detection. Texture information can improve classification performance. This approach uses both shape and texture features. Feature extraction is done by Hu’s moment invariants with several classification algorithms. This paper presents an overview of
automatic ship recognition methods with a view towards embedded implementation on optical smart cameras. Therefore this approach may attain a good classification rate.
SIGGRAPH 2014 Course on Computational Cameras and Displays (part 3)Matthew O'Toole
Recent advances in both computational photography and displays have given rise to a new generation of computational devices. Computational cameras and displays provide a visual experience that goes beyond the capabilities of traditional systems by adding computational power to optics, lights, and sensors. These devices are breaking new ground in the consumer market, including lightfield cameras that redefine our understanding of pictures (Lytro), displays for visualizing 3D/4D content without special eyewear (Nintendo 3DS), motion-sensing devices that use light coded in space or time to detect motion and position (Kinect, Leap Motion), and a movement toward ubiquitous computing with wearable cameras and displays (Google Glass).
This short (1.5 hour) course serves as an introduction to the key ideas and an overview of the latest work in computational cameras, displays, and light transport.
ESA SMOS (Soil Moisture and Ocean Salinity) Mission: Principles of Operation ...adrianocamps
SMOS basic principles and description of some products developed at the SMOS Barcelona Expert Center.
Disclaimer: these materials were prepared for Eduacational purposes only.
Presentation made by Prof. Adriano Camps (Universitat Politècnica de Catalunya) at ICMARS 2010 (India, 16-December-2010) on the MIRAS instrument aboard ESA's SMOS mission.
SIGGRAPH 2014 Course on Computational Cameras and Displays (part 4)Matthew O'Toole
Recent advances in both computational photography and displays have given rise to a new generation of computational devices. Computational cameras and displays provide a visual experience that goes beyond the capabilities of traditional systems by adding computational power to optics, lights, and sensors. These devices are breaking new ground in the consumer market, including lightfield cameras that redefine our understanding of pictures (Lytro), displays for visualizing 3D/4D content without special eyewear (Nintendo 3DS), motion-sensing devices that use light coded in space or time to detect motion and position (Kinect, Leap Motion), and a movement toward ubiquitous computing with wearable cameras and displays (Google Glass).
This short (1.5 hour) course serves as an introduction to the key ideas and an overview of the latest work in computational cameras, displays, and light transport.
A Novel Approach for Ship Recognition using Shape and Texture ijait
Maritime security includes reliable identification of ship entering and leaving a nation’s territorial waters. Sea target detection from remote sensing imagery is very important, with a wide array of applications in areas such as fishery management, vessel traffic services, and naval warfare. Automated systems that could identify a ship could complement existing electronic signal identification methods. A new classification approach using shape and texture is introduced for Ship detection. Texture information can improve classification performance. This approach uses both shape and texture features. Feature extraction is done by Hu’s moment invariants with several classification algorithms. This paper presents an overview of
automatic ship recognition methods with a view towards embedded implementation on optical smart cameras. Therefore this approach may attain a good classification rate.
SIGGRAPH 2014 Course on Computational Cameras and Displays (part 3)Matthew O'Toole
Recent advances in both computational photography and displays have given rise to a new generation of computational devices. Computational cameras and displays provide a visual experience that goes beyond the capabilities of traditional systems by adding computational power to optics, lights, and sensors. These devices are breaking new ground in the consumer market, including lightfield cameras that redefine our understanding of pictures (Lytro), displays for visualizing 3D/4D content without special eyewear (Nintendo 3DS), motion-sensing devices that use light coded in space or time to detect motion and position (Kinect, Leap Motion), and a movement toward ubiquitous computing with wearable cameras and displays (Google Glass).
This short (1.5 hour) course serves as an introduction to the key ideas and an overview of the latest work in computational cameras, displays, and light transport.
Seismic QC & Filtering with GeostatisticsGeovariances
The quality of seismic volumes is critical in building reliable reservoir models. Seismic data are often polluted by acquisition or processing artifacts which may have strong impact on subsequent seismic processing or interpretation. Geostatistics allows filtering efficiently seismic noise and artifacts without modifying the signal.
Geovariances provides solutions from seismic data quality control and filtering to reservoir characterization. This technology is based on geostatistics and all algorithms are available in Isatis, leader in geostatistical software solutions.
Optical Computing for Fast Light Transport AnalysisMatthew O'Toole
Optical Computing for Fast Light Transport Analysis
Matthew O'Toole and Kiriakos N. Kutulakos. ACM SIGGRAPH Asia, 2010.
We present a general framework for analyzing the transport matrix of a real-world scene at full resolution, without capturing many photos. The key idea is to use projectors and cameras to directly acquire eigenvectors and the Krylov subspace of the unknown transport matrix. To do this, we implement Krylov subspace methods partially in optics, by treating the scene as a black box subroutine that enables optical computation of arbitrary matrix-vector products. We describe two methods—optical Arnoldi to acquire a low-rank approximation of the transport matrix for relighting; and optical GMRES to invert light transport. Our experiments suggest that good-quality relighting and transport inversion are possible from a few dozen low-dynamic range photos, even for scenes with complex shadows, caustics, and other challenging lighting effects.
GPS cycle slips detection and repair through various signal combinationsIJMER
Abstract: GPS Cycle slips affect the measured spatial distance between the satellite and the receiver, thus affecting the accuracy of the derived 3D coordinates of any ground station. Therefore, cycle slips must be detected and repaired before performing any data processing. The objectives of this research are to detect the Cycle slips by using various types of GPS signal combinations with graphical and statistical tests techniques, and to repair cycle slips by using average and time difference geometry techniques. Results of detection process show that the graphical detection can be used as a primary detection
technique whereas the statistical approaches of detection are proved to be superior. On the other hand, results of repairing process show that any trial can be used for such process except for the 1st and 2nd time differences averaging all data as they give very low accuracy of the cycle slip fixation.
Gefran controls used for evaluating the focusing performance of mirrors in Ch...Gefran Inc.
The CTA observatory is a project designed by a worldwide consortium that will make use of well demonstrated technologies of present generation Cherenkov telescopes as
well as new ad hoc developed solutions. CTA will be based on telescopes with different sizes installed over a large area. At its southern site e.g. 70 Small Size 20 Telescopes (4 m primary mirror diameter), 20 Medium Size Telescopes (12 m)
and 4 Large Size Telescopes (23 m) will be implemented in order to cover a broad spectral energy range from a few tens of GeV up to 100 TeV.
Explanation of very simple methods for atmospheric corrections and an example adapted from a paper of the Dept. of Thermodynamics, University of Valencia, Spain.
Seismic QC & Filtering with GeostatisticsGeovariances
The quality of seismic volumes is critical in building reliable reservoir models. Seismic data are often polluted by acquisition or processing artifacts which may have strong impact on subsequent seismic processing or interpretation. Geostatistics allows filtering efficiently seismic noise and artifacts without modifying the signal.
Geovariances provides solutions from seismic data quality control and filtering to reservoir characterization. This technology is based on geostatistics and all algorithms are available in Isatis, leader in geostatistical software solutions.
Optical Computing for Fast Light Transport AnalysisMatthew O'Toole
Optical Computing for Fast Light Transport Analysis
Matthew O'Toole and Kiriakos N. Kutulakos. ACM SIGGRAPH Asia, 2010.
We present a general framework for analyzing the transport matrix of a real-world scene at full resolution, without capturing many photos. The key idea is to use projectors and cameras to directly acquire eigenvectors and the Krylov subspace of the unknown transport matrix. To do this, we implement Krylov subspace methods partially in optics, by treating the scene as a black box subroutine that enables optical computation of arbitrary matrix-vector products. We describe two methods—optical Arnoldi to acquire a low-rank approximation of the transport matrix for relighting; and optical GMRES to invert light transport. Our experiments suggest that good-quality relighting and transport inversion are possible from a few dozen low-dynamic range photos, even for scenes with complex shadows, caustics, and other challenging lighting effects.
GPS cycle slips detection and repair through various signal combinationsIJMER
Abstract: GPS Cycle slips affect the measured spatial distance between the satellite and the receiver, thus affecting the accuracy of the derived 3D coordinates of any ground station. Therefore, cycle slips must be detected and repaired before performing any data processing. The objectives of this research are to detect the Cycle slips by using various types of GPS signal combinations with graphical and statistical tests techniques, and to repair cycle slips by using average and time difference geometry techniques. Results of detection process show that the graphical detection can be used as a primary detection
technique whereas the statistical approaches of detection are proved to be superior. On the other hand, results of repairing process show that any trial can be used for such process except for the 1st and 2nd time differences averaging all data as they give very low accuracy of the cycle slip fixation.
Gefran controls used for evaluating the focusing performance of mirrors in Ch...Gefran Inc.
The CTA observatory is a project designed by a worldwide consortium that will make use of well demonstrated technologies of present generation Cherenkov telescopes as
well as new ad hoc developed solutions. CTA will be based on telescopes with different sizes installed over a large area. At its southern site e.g. 70 Small Size 20 Telescopes (4 m primary mirror diameter), 20 Medium Size Telescopes (12 m)
and 4 Large Size Telescopes (23 m) will be implemented in order to cover a broad spectral energy range from a few tens of GeV up to 100 TeV.
Explanation of very simple methods for atmospheric corrections and an example adapted from a paper of the Dept. of Thermodynamics, University of Valencia, Spain.
3 Things Every Sales Team Needs to Be Thinking About in 2017Drift
Thinking about your sales team's goals for 2017? Drift's VP of Sales shares 3 things you can do to improve conversion rates and drive more revenue.
Read the full story on the Drift blog here: http://blog.drift.com/sales-team-tips
Compressive Light Field Photography using Overcomplete Dictionaries and Optim...Ankit Thiranh
In this paper, a design is proposed for a compressive light field camera which will allow to recover light fields with higher resolution from a single image. Also, various other useful applications for light field atoms are discussed, including 4D light field compression and denoising.
Atmospheric Correction of Remote Sensing Data_RamaRao.pptxssusercd49c0
Atmospheric correction of remote sensing data. This PPT describes development of a region sensitive atmospheric correction method for hyperspectral image processing
Definition and Validation of Scientific Algorithms for the SEOSAT/Ingenio GPPEsri
Presentation by Eduardo de Miguel, Raúl Valenzuela, Teodoro Bernardino, Verena Rodríguez, Alberto Pizarro, Diana de Miguel and Severino Fernández from INTA, GMV and EADS-CASA made on Esri European User Conference 2011.
The fourier transform for satellite image compressioncsandit
The need to transmit or store satellite images is growing rapidly with the development of
modern communications and new imaging systems. The goal of compression is to facilitate the
storage and transmission of large images on the ground with high compression ratios and
minimum distortion. In this work, we present a new coding scheme for satellite images. At first,
the image will be downloaded followed by a fast Fourier transform FFT. The result obtained
after FFT processing undergoes a scalar quantization (SQ). The results obtained after the
quantization phase are encoded using entropy encoding. This approach has been tested on
satellite image and Lena picture. After decompression, the images were reconstructed faithfully
and memory space required for storage has been reduced by more than 80%
THE FOURIER TRANSFORM FOR SATELLITE IMAGE COMPRESSIONcscpconf
The need to transmit or store satellite images is growing rapidly with the development of
modern communications and new imaging systems. The goal of compression is to facilitate the
storage and transmission of large images on the ground with high compression ratios and
minimum distortion. In this work, we present a new coding scheme for satellite images. At first,
the image will be downloaded followed by a fast Fourier transform FFT. The result obtained
after FFT processing undergoes a scalar quantization (SQ). The results obtained after the
quantization phase are encoded using entropy encoding. This approach has been tested on
satellite image and Lena picture. After decompression, the images were reconstructed faithfully
and memory space required for storage has been reduced by more than 80%
DUAL BAND GNSS ANTENNA PHASE CENTER CHARACTERIZATION FOR AUTOMOTIVE APPLICATIONSjantjournal
High-accuracy Global Navigation Satellite System (GNSS) positioning is a prospective technology that will be used in future automotive navigation systems. This system will be a composite of the United States' Global Positioning System (GPS), the Russian Federation's Global Orbiting Navigation Satellite System (GLONASS), China Beidou Navigation Satellite System (BDS) and the European Union’s Galileo. The major improvement in accuracy and precision is based on (1) multiband signal transmitting, (2) carrier phase correction, (3) Real Time Kinematic (RTK). Due to the size and high-cost of today’s survey-grade antenna solutions, this kind of technology is difficult to use widely in the automotive sector. In this paper, a low-cost small size dual-band ceramic GNSS patch antenna is presented from design to real sample. A further study of this patch antenna illustrates the absolute phase center variation measured in an indoor range to achieve a received signal phase error correction. In addition, this low-cost antenna solution is investigated when integrated into a standard multi-band automotive antenna product. This product is evaluated both on its own in an indoor range and on a typical vehicle roof at an outdoor range. By using this evaluation file to estimate the receiver position could achieve phase motion error-free result.
DUAL BAND GNSS ANTENNA PHASE CENTER CHARACTERIZATION FOR AUTOMOTIVE APPLICATIONSjantjournal
High-accuracy Global Navigation Satellite System (GNSS) positioning is a prospective technology that will be used in future automotive navigation systems. This system will be a composite of the United States' Global Positioning System (GPS), the Russian Federation's Global Orbiting Navigation Satellite System (GLONASS), China Beidou Navigation Satellite System (BDS) and the European Union’s Galileo. The major improvement in accuracy and precision is based on (1) multiband signal transmitting, (2) carrier phase correction, (3) Real Time Kinematic (RTK). Due to the size and high-cost of today’s survey-grade antenna solutions, this kind of technology is difficult to use widely in the automotive sector. In this paper, a low-cost small size dual-band ceramic GNSS patch antenna is presented from design to real sample. A further study of this patch antenna illustrates the absolute phase center variation measured in an indoor range to achieve a received signal phase error correction. In addition, this low-cost antenna solution is investigated when integrated into a standard multi-band automotive antenna product. This product is evaluated both on its own in an indoor range and on a typical vehicle roof at an outdoor range. By using this evaluation file to estimate the receiver position could achieve phase motion error-free result.
DUAL BAND GNSS ANTENNA PHASE CENTER CHARACTERIZATION FOR AUTOMOTIVE APPLICATIONSjantjournal
High-accuracy Global Navigation Satellite System (GNSS) positioning is a prospective technology that will be used in future automotive navigation systems. This system will be a composite of the United States' Global Positioning System (GPS), the Russian Federation's Global Orbiting Navigation Satellite System (GLONASS), China Beidou Navigation Satellite System (BDS) and the European Union’s Galileo. The major improvement in accuracy and precision is based on (1) multiband signal transmitting, (2) carrier phase correction, (3) Real Time Kinematic (RTK). Due to the size and high-cost of today’s survey-grade antenna solutions, this kind of technology is difficult to use widely in the automotive sector. In this paper, a low-cost small size dual-band ceramic GNSS patch antenna is presented from design to real sample. A further study of this patch antenna illustrates the absolute phase center variation measured in an indoor range to achieve a received signal phase error correction. In addition, this low-cost antenna solution is investigated when integrated into a standard multi-band automotive antenna product. This product is evaluated both on its own in an indoor range and on a typical vehicle roof at an outdoor range. By using this evaluation file to estimate the receiver position could achieve phase motion error-free result.
DUAL BAND GNSS ANTENNA PHASE CENTER CHARACTERIZATION FOR AUTOMOTIVE APPLICATIONSjantjournal
High-accuracy Global Navigation Satellite System (GNSS) positioning is a prospective technology that will be used in future automotive navigation systems. This system will be a composite of the United States' Global Positioning System (GPS), the Russian Federation's Global Orbiting Navigation Satellite System (GLONASS), China Beidou Navigation Satellite System (BDS) and the European Union’s Galileo. The major improvement in accuracy and precision is based on (1) multiband signal transmitting, (2) carrier phase correction, (3) Real Time Kinematic (RTK). Due to the size and high-cost of today’s survey-grade antenna solutions, this kind of technology is difficult to use widely in the automotive sector. In this paper, a low-cost small size dual-band ceramic GNSS patch antenna is presented from design to real sample. A further study of this patch antenna illustrates the absolute phase center variation measured in an indoor range to achieve a received signal phase error correction. In addition, this low-cost antenna solution is investigated when integrated into a standard multi-band automotive antenna product. This product is evaluated both on its own in an indoor range and on a typical vehicle roof at an outdoor range. By using this evaluation file to estimate the receiver position could achieve phase motion error-free result.
DUAL BAND GNSS ANTENNA PHASE CENTER CHARACTERIZATION FOR AUTOMOTIVE APPLICATIONSjantjournal
High-accuracy Global Navigation Satellite System (GNSS) positioning is a prospective technology that will be used in future automotive navigation systems. This system will be a composite of the United States' Global Positioning System (GPS), the Russian Federation's Global Orbiting Navigation Satellite System (GLONASS), China Beidou Navigation Satellite System (BDS) and the European Union’s Galileo. The major improvement in accuracy and precision is based on (1) multiband signal transmitting, (2) carrier phase correction, (3) Real Time Kinematic (RTK). Due to the size and high-cost of today’s survey-grade antenna solutions, this kind of technology is difficult to use widely in the automotive sector. In this paper, a low-cost small size dual-band ceramic GNSS patch antenna is presented from design to real sample. A further study of this patch antenna illustrates the absolute phase center variation measured in an indoor range to achieve a received signal phase error correction. In addition, this low-cost antenna solution is investigated when integrated into a standard multi-band automotive antenna product. This product is evaluated both on its own in an indoor range and on a typical vehicle roof at an outdoor range. By using this evaluation file to estimate the receiver position could achieve phase motion error-free result.
Similar to Study o horizontal flows in solar active regions (20)
Descripción de las regiones en Colombia como preámbulo al tema del café. Historia del café, escritos y leyendas sobre el café, estadísticas, datos cursiosos, farmacología y una descripción paso a paso de su proceso de producción.
June 3, 2024 Anti-Semitism Letter Sent to MIT President Kornbluth and MIT Cor...Levi Shapiro
Letter from the Congress of the United States regarding Anti-Semitism sent June 3rd to MIT President Sally Kornbluth, MIT Corp Chair, Mark Gorenberg
Dear Dr. Kornbluth and Mr. Gorenberg,
The US House of Representatives is deeply concerned by ongoing and pervasive acts of antisemitic
harassment and intimidation at the Massachusetts Institute of Technology (MIT). Failing to act decisively to ensure a safe learning environment for all students would be a grave dereliction of your responsibilities as President of MIT and Chair of the MIT Corporation.
This Congress will not stand idly by and allow an environment hostile to Jewish students to persist. The House believes that your institution is in violation of Title VI of the Civil Rights Act, and the inability or
unwillingness to rectify this violation through action requires accountability.
Postsecondary education is a unique opportunity for students to learn and have their ideas and beliefs challenged. However, universities receiving hundreds of millions of federal funds annually have denied
students that opportunity and have been hijacked to become venues for the promotion of terrorism, antisemitic harassment and intimidation, unlawful encampments, and in some cases, assaults and riots.
The House of Representatives will not countenance the use of federal funds to indoctrinate students into hateful, antisemitic, anti-American supporters of terrorism. Investigations into campus antisemitism by the Committee on Education and the Workforce and the Committee on Ways and Means have been expanded into a Congress-wide probe across all relevant jurisdictions to address this national crisis. The undersigned Committees will conduct oversight into the use of federal funds at MIT and its learning environment under authorities granted to each Committee.
• The Committee on Education and the Workforce has been investigating your institution since December 7, 2023. The Committee has broad jurisdiction over postsecondary education, including its compliance with Title VI of the Civil Rights Act, campus safety concerns over disruptions to the learning environment, and the awarding of federal student aid under the Higher Education Act.
• The Committee on Oversight and Accountability is investigating the sources of funding and other support flowing to groups espousing pro-Hamas propaganda and engaged in antisemitic harassment and intimidation of students. The Committee on Oversight and Accountability is the principal oversight committee of the US House of Representatives and has broad authority to investigate “any matter” at “any time” under House Rule X.
• The Committee on Ways and Means has been investigating several universities since November 15, 2023, when the Committee held a hearing entitled From Ivory Towers to Dark Corners: Investigating the Nexus Between Antisemitism, Tax-Exempt Universities, and Terror Financing. The Committee followed the hearing with letters to those institutions on January 10, 202
Welcome to TechSoup New Member Orientation and Q&A (May 2024).pdfTechSoup
In this webinar you will learn how your organization can access TechSoup's wide variety of product discount and donation programs. From hardware to software, we'll give you a tour of the tools available to help your nonprofit with productivity, collaboration, financial management, donor tracking, security, and more.
The Roman Empire A Historical Colossus.pdfkaushalkr1407
The Roman Empire, a vast and enduring power, stands as one of history's most remarkable civilizations, leaving an indelible imprint on the world. It emerged from the Roman Republic, transitioning into an imperial powerhouse under the leadership of Augustus Caesar in 27 BCE. This transformation marked the beginning of an era defined by unprecedented territorial expansion, architectural marvels, and profound cultural influence.
The empire's roots lie in the city of Rome, founded, according to legend, by Romulus in 753 BCE. Over centuries, Rome evolved from a small settlement to a formidable republic, characterized by a complex political system with elected officials and checks on power. However, internal strife, class conflicts, and military ambitions paved the way for the end of the Republic. Julius Caesar’s dictatorship and subsequent assassination in 44 BCE created a power vacuum, leading to a civil war. Octavian, later Augustus, emerged victorious, heralding the Roman Empire’s birth.
Under Augustus, the empire experienced the Pax Romana, a 200-year period of relative peace and stability. Augustus reformed the military, established efficient administrative systems, and initiated grand construction projects. The empire's borders expanded, encompassing territories from Britain to Egypt and from Spain to the Euphrates. Roman legions, renowned for their discipline and engineering prowess, secured and maintained these vast territories, building roads, fortifications, and cities that facilitated control and integration.
The Roman Empire’s society was hierarchical, with a rigid class system. At the top were the patricians, wealthy elites who held significant political power. Below them were the plebeians, free citizens with limited political influence, and the vast numbers of slaves who formed the backbone of the economy. The family unit was central, governed by the paterfamilias, the male head who held absolute authority.
Culturally, the Romans were eclectic, absorbing and adapting elements from the civilizations they encountered, particularly the Greeks. Roman art, literature, and philosophy reflected this synthesis, creating a rich cultural tapestry. Latin, the Roman language, became the lingua franca of the Western world, influencing numerous modern languages.
Roman architecture and engineering achievements were monumental. They perfected the arch, vault, and dome, constructing enduring structures like the Colosseum, Pantheon, and aqueducts. These engineering marvels not only showcased Roman ingenuity but also served practical purposes, from public entertainment to water supply.
Palestine last event orientationfvgnh .pptxRaedMohamed3
An EFL lesson about the current events in Palestine. It is intended to be for intermediate students who wish to increase their listening skills through a short lesson in power point.
Embracing GenAI - A Strategic ImperativePeter Windle
Artificial Intelligence (AI) technologies such as Generative AI, Image Generators and Large Language Models have had a dramatic impact on teaching, learning and assessment over the past 18 months. The most immediate threat AI posed was to Academic Integrity with Higher Education Institutes (HEIs) focusing their efforts on combating the use of GenAI in assessment. Guidelines were developed for staff and students, policies put in place too. Innovative educators have forged paths in the use of Generative AI for teaching, learning and assessments leading to pockets of transformation springing up across HEIs, often with little or no top-down guidance, support or direction.
This Gasta posits a strategic approach to integrating AI into HEIs to prepare staff, students and the curriculum for an evolving world and workplace. We will highlight the advantages of working with these technologies beyond the realm of teaching, learning and assessment by considering prompt engineering skills, industry impact, curriculum changes, and the need for staff upskilling. In contrast, not engaging strategically with Generative AI poses risks, including falling behind peers, missed opportunities and failing to ensure our graduates remain employable. The rapid evolution of AI technologies necessitates a proactive and strategic approach if we are to remain relevant.
Model Attribute Check Company Auto PropertyCeline George
In Odoo, the multi-company feature allows you to manage multiple companies within a single Odoo database instance. Each company can have its own configurations while still sharing common resources such as products, customers, and suppliers.
Read| The latest issue of The Challenger is here! We are thrilled to announce that our school paper has qualified for the NATIONAL SCHOOLS PRESS CONFERENCE (NSPC) 2024. Thank you for your unwavering support and trust. Dive into the stories that made us stand out!
Synthetic Fiber Construction in lab .pptxPavel ( NSTU)
Synthetic fiber production is a fascinating and complex field that blends chemistry, engineering, and environmental science. By understanding these aspects, students can gain a comprehensive view of synthetic fiber production, its impact on society and the environment, and the potential for future innovations. Synthetic fibers play a crucial role in modern society, impacting various aspects of daily life, industry, and the environment. ynthetic fibers are integral to modern life, offering a range of benefits from cost-effectiveness and versatility to innovative applications and performance characteristics. While they pose environmental challenges, ongoing research and development aim to create more sustainable and eco-friendly alternatives. Understanding the importance of synthetic fibers helps in appreciating their role in the economy, industry, and daily life, while also emphasizing the need for sustainable practices and innovation.
1. Santiago Vargas Domínguez La Laguna, Tenerife - Dec 18, 2008 Study of horizontal flows in solar active regions high-resolution image reconstruction techniques based on THESIS DISSERTATION Supervisors: Jose Antonio Bonet & Valentín Martínez Pillet THESIS DISSERTATION Study of horizontal flows in solar active regions high-resolution image reconstruction techniques based on Santiago Vargas Domínguez Supervisors: Valentín Martínez Pillet & Jose A. Bonet La Laguna, Tenerife - Dic 2008 La Laguna, Tenerife - Dic 2008 THESIS DISSERTATION Study of horizontal flows in solar active regions high-resolution image reconstruction techniques Santiago Vargas Domínguez Supervisors: Valentín Martínez Pillet & Jose A. Bonet based on
2. PART 1 Defining a method for in-flight calibration of IMaX aberrations PART 2 Study of proper motions in solar active regions Outline
3. PART 1 Defining a method for in-flight calibration of IMaX aberrations Aim at: Perform numerical simulations to identify and evaluate possible optical error sources in the IMaX instrument. Develop an in-flight calibration method to characterize the aberrations affecting the images in IMaX. Describe and test the robustness of the calibration method.
4. Outline PART 1 Defining a method for in-flight calibration of IMaX aberrations Introduction Image restoration techniques In-flight calibration of IMaX aberrations Conclusions
5. PART 1 Defining a method for in-flight calibration of IMaX aberrations d) Conclusions c) In-flight calibration of IMaX aberrations a) Introduction b) Image restoration techniques Trying to explain the physics of the Sun requires to resolve very tiny structures
6. PART 1 Defining a method for in-flight calibration of IMaX aberrations d) Conclusions c) In-flight calibration of IMaX aberrations a) Introduction b) Image restoration techniques Earth’s atmosphere can be considered as an isotropic turbulent medium Atmospheric turbulence is a major problem we encounter in ground-based observations affecting the image quality
7. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Image degradation is generally described as the combination of 3 main contributions Structures smearing (blurring) Global displacements of the image (image motion) Distortion of structures caused by differential image motion in different patches (stretching) First problem to deal with if interested on high resolution data seeing
8. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Solutions: Space observatories SOHO HINODE Elevated cost of launching, maintenance and updating Adaptive Optics Only pursues low-order corrections Limited to an isoplanatic patch of a few arcsec
9. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Solutions : Space observatories Adaptive Optics Post-facto techniques Powerful numerical codes for image restoration developed in the last decade. They require a specific observing strategy
10. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Image formation Object plane Image plane Object plane Image plane X Y
11. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Text Object plane Image plane Airy spot Image formation + Point in the object plane observed as a spot on the image plane X Y
12. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Text Text Point Spread Function Space variant Variability of the transmission system For a extended object (e.g Sun) Intensity at each point has a contribution from the neighborhood Image formation PSF =
13. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Text Text Image restoration Image restoration fits into the Inverse Problem in Physics that can be considered as the solution of the Fredholm Inhomogeneous equation of the 1 st kind . The kernel is the PSF Using the convolution theorem, True object where q is the vectorial notation for the coordinates in the image points Isoplanatic assumption Optical Transfer Function (OTF)
14. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction Text Text Noise contribution and filtering Restoration filter (Wiener-Helstrom) Additive noise Some models for SNR are commonly assumed (Collados, 1986)
15. Phase Diversity technique PART 1 Defining a method for in-flight calibration of IMaX aberrations b) Image restoration techniques a) Introduction d) Conclusions c) In-flight calibration of IMaX aberrations focus-defocus image pairs PSFs noise additive terms true object The PD technique was first proposed as a new method to infer phase aberrations working with images of extended incoherent objects formed through an optical system (Gonsalves & Childlaw, 1979). Noise terms force a statistical solution of the problem
16. PART 1 Defining a method for in-flight calibration of IMaX aberrations b) Image restoration techniques a) Introduction d) Conclusions c) In-flight calibration of IMaX aberrations Phase Diversity technique Error metric to be minimized (Paxman et all, 1992) OTF is the auto-correlation of the generalized pupil function Joint phase aberration Zernikes Parametrized by the expansion in Zernike polynomials. Non-linear optimization techniques (SVD) are used to minimize the error metric and get the vector, S 1 , S 2 and I o
17. PART 1 Defining a method for in-flight calibration of IMaX aberrations b) Image restoration techniques Restoration techniques MFBD Multi-Frame Lofdahl, 2002, 1996 Blind Deconvolution MOMFBD Multi-Object Multi-Frame Van Noort, Rouppe van der Voort & Löfdahl, 2005 PD Phase Diversity Results coming up in a few minutes !!!!
18. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction d) Conclusions c) In-flight calibration of IMaX aberr. b) Image restoration techniques Imaging Magnetograph eXperiment Instituto de Astrofísica de Canarias Instituto de Astrofísica de Andalucía Instituto Nacional de Técnica Aeroespacial Grupo de Astronomía y Ciencias del Espacio
19. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction d) Conclusions c) In-flight calibration of IMaX aberr. b) Image restoration techniques SUNRISE Ballon-borne 1-m solar telescope Aims at: High-resolution Spectro-polarimetric observations of the solar atmosphere To be flown: In the framework of NASA Long Duration Ballon Program in 2009 in circumpolar trajectories at 35-40 km. Consist of: Telescope , Image Stabilisation and Light Distribution System , IMaX Sunrise Filter Imager (SUFI)
20. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr.
21. sp PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. ISLiD - Image Stabilisation and Light Distribution System For simultaneous observations with all science instruments based on di-electric dichroic beam splitters. Includes the Correlator and Wavefront Sensor IMaX - Imaging Magnetograph eXperiment Magnetograph providing fast cadence two-dimensional maps of complete magnetic field vector and the LOS velocity as well as white-light images with high-spatial resolution. SUFI - Sunrise Filter Imager Filtegraph for high-resolution images in the visible and the UV spectral lines.
22. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. IMaX description Aim at: Provide magnetograms of extended solar regions by combining high temporal cadence and polarimetric precision, working as: High-efficient image acquisition system Near diffraction limited imager High resolving power spectrograph High sensitivity polarimeter
23. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Cameras Etalon Electronics box
24. A glass-plate can be optionally intercalated in one of the IMaX imaging channels to get simultaneous focus-defocus image-pairs, i.e. Phase Diversity (PD) image-pairs, from which an estimate of the aberrations will be possible in post-processing by means of a PD inversion code. Assuming a long-term variation in the aberrations, their calibration could be performed with a cadence of one hour. A burst of 25-30 PD-pairs in the continuum would be enough each time. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Calibration of aberrations in IMaX We have included in IMaX a system to calibrate the image degradation during the flight that should allow a correction of the residual aberrations in the science images. diversity
25. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction d) Conclusions c) In-flight calibration of IMaX aberr. b) Image restoration techniques Strategy
26. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Testing the robustness of the calibration method Evaluate the robustness of the method versus a variety of aberration assumptions Isoplanatic patch True object Synthetic image (Vöegler et al. 2005)
27. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Testing the robustness of the calibration method Simulate the formation of PD image-pairs produced by 1 -m telescope and a given set of aberrations. Image-pairs are inverted with the PD code. Set of averaged aberrations retrieved from inversions are compared to input aberrations. 30 for diff. photon noise realizations
28. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Identifying error sources The contribution from the error sources can be mathematically represented through the generalized pupil function , Phase diverse Transmission function over pupil Main polishing error Phase error from etalon Low-order aberrations Atm. aberration (IMaX=0)
29. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Quantifying error sources contribution First step is the compilation of data from the design and specifications of all different components
30. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Low-order aberrations (LOA) Empirical measurements for the assembled instrument.
31. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Amplitude in double-pass Phase in double-pass | H ( , ) | e ( , ) Etalon Screens
32. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Main mirror polishing errors Ripple screen High-order aberrations Average power spectrum matches a von Karman power spectrum
33. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Phase Diversity plate
34. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Detector contribution A detector element performs a spatial integration of the irradiance falling onto its surface
35. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Simulations We classify error contributions in 3 groups: Low-order aberrations (LOA) High-order aberrations (HOA) Detector contribution & Noise
36. PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Simulations ERROR SOURCE CONTRIBUTION EXPERIMENT 1 2 3 4 rms-ripple 0, 2/60, 2/28 waves rms-LOA 0, 1/12, 1/7, 1/4, 1/3, 1/2 waves rms-noise 10 -3 x continuum signal rms-etalon 1/26 waves Etalon amplitude | H( , ) | ≠ 1 CCD 12 m/pix PD-defocus DEGRADATION/INVERSION 8.51 mm (PV 1.00 ) / 8.51 mm 9.00 mm (PV 1.06 ) / 8.51 mm
37.
38. A pessimistic case for IMaX + ISLiD + Telescope performance PART 1 Defining a method for in-flight calibration of IMaX aberrations c) In-flight calibration of IMaX aberr. Error contributions rms-ripple=2 /60 rms-etalon= /26 rms-noise=10 -3 CCD rms-LOA= /5 Focus image of a PD-pair True object (from 30 realizations) RESULTS Degraded Restored True
39. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction b) Image restoration techniques d) Conclusions c) In-flight calibration of IMaX aberrations A method for the in-flight calibration of aberrations in IMaX has been proposed. The robustness of the method has been tested by numerical experiments simulating different aberration components. Sources of aberration have been modeled and added in every subsequent experiment. The repercussion of every new added ingredient in the final result from the inversions has been evaluated. In the PART 1 of this work: The calibration method has proved to give satisfactory results even in under pessimistic aberration conditions
40. PART 1 Defining a method for in-flight calibration of IMaX aberrations a) Introduction b) Image restoration techniques d) Conclusions c) In-flight calibration of IMaX aberrations Main conclusions are: The PD-code does not accurately reproduce the shape of the WFE but provides reliable OTFs for satisfactory restorations. Inhomogeneities in the etalon transmission are converted into some extra errors in the resulting wavefront that partially compensate the loss of contrast caused by unsensed HOA. Experiment 3 validates the method proposed to calibrate the errors in the images of IMaX The amount of defocus (diversity) produced by the PD plate is a critical parameter for an optimal performance of the PD code. An error of 0.5 mm in the determination of the diversity value can caused an over restoration of about 5%.
41. PART 2 Study of proper motions in solar active regions Aim at: Analysis of horizontal proper motions, at a photospheric level, around solar active regions from ground-based and space high-resolution time series. Nearly 1000000 images have been used for this study !!!
42. Outline Solar active regions Proper motions in a complex AR Moat flows surrounding sunspots Flow field around solar pores Conclusions PART 2 Study of proper motions in solar active regions
43. a) Solar active regions b) Proper motions in a complex AR d) Flow field around solar pores e) Conclusions c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions Are the evident manifestation of the solar activity Sunspots Are interpreted as complex structures having strong magnetic fields that inhibit the plasma convection (temperature lower than the surrounding photosphere)
44. a) Solar active regions b) Proper motions in a complex AR d) Flow field around solar pores e) Conclusions c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions Monolithic : Mag. field underneath the solar surface is Cowling, 1957 confined to a single flux tube. Structure of Sunspots The responsible for the origin and structure is believed to be the toroidal magnetic flux in the solar interior (Schüssler et al, 2002) Cluster (spaguetti) : Mag. field divides into many separate flux Parker, 1979 tubes in the first Mm below the surface Models
45. a) Solar active regions PART 2 Study of proper motions in solar active regions Umbra Coolest part of the sunspots ~ 3500 - 5000 K Strong Mag.F inhibits convection Vertical magnetic field; more inclined at umbra-penumbra boundary ~ 2000 - 3500 Gauss in average Energy radiation 20% photosphere Features (umbral dots, light bridges) Penumbra Filamentary bright/dark structure The first one has been extensively tested 2 different orientations of mag . field coexist Energy radiation 75% photospheric Mag. Field inner part: ~1500 Gauss outer part: ~700 Gauss Vertical component (~60-70 deg) Horizontal component Different models try to explain the structure of the penumbra: Uncombed, Gappy, MISMAS.
46. a) Solar active regions PART 2 Study of proper motions in solar active regions Evershed Flow Associated to an observational effect in the penumbra registered as a global wavelength shift for spectral lines forming in the penumbrae of sunspots.
47. a) Solar active regions PART 2 Study of proper motions in solar active regions Photosphere surrounding sunspots Convective flows & large-scale plasma circulation plays and important role in dynamics and evolution of solar active regions (Schrijver & Zwaan 2000). Granular convective pattern surrounding sunspots is perturbed by the presence of magnetic elements, moving magnetic features (MMF). MMF’s move radially outward through an annular cell called “ moat ”. (Sheeley 1972, Harvey & Harvey 1973).
48. a) Solar active regions PART 2 Study of proper motions in solar active regions Moat flow (Meyer et al. 1974) Could be: Typical cell scale of up to 10 4 km. A supergranule. Center occupied by a sunspot.
49. (Nye et al. 1988) Excess temperature and pressure generated have been proposed as origin of moat. Sunspot would act as a blocking agent to the upward propagation of heat from below.
50. Averaged horizontal velocities [m s -1 ] a) Solar active regions PART 2 Study of proper motions in solar active regions + Young spots ♢ Old Spots Sobotka & Roudier, 2007
51. d) Flow field around solar pores e) Conclusions c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions a) Solar active regions b) Proper motions in a complex solar AR Observations 1m - Solar Swedish Tower (SST) Roque de los Muchachos Observatory, La Palma. NOAA AR10786 9-Jul-2005 G-band, G-cont 7:47 – 9:06 UT DC G- band δ-configuration sunspot
52. PART 2 Study of proper motions in solar active regions d) Flow field around solar pores e) Conclusions c) Moat flows surrounding sunspots a) Solar active regions b) Proper motions in a complex solar AR Processing Flat-fielding & dark-current substraction Image restoration MOMFBD + PD De-rotation and alignment De-stretching and p-modes filtering Time series G-band and G-cont 428 images each Cadence: 10.0517 s 71 minutes FOV 57.8” x 34.4” Image restoration MOMFBD + PD Low quality Medium quality Good quality Restored quality
55. Moat No Moat Exploding granules dragged by the moat flow (elongated) Recurrent exploding granules
56. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Map of displacements We have used the G-band series to study proper motions of the structures by local correlation technique (LCT) Finding local concordances between two frames (correlation window). First applied by November & Simon (1988) to measure proper motions in solar granulation. Used at diff. spatial scales to study solar dynamics (e.g supergranulation Shine,Simon & Hurlburt, 2000 ) Gaussian tracking window FWHM = 0.78” (half of typical granular size) Map of horizontal displacements averaged over the whole series
57. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR General description of proper motions Flowmap [Mm] Neutral Lines Exploding granules SOUP magnetograms MOMFBD+PD Combining 1500 images SNR=200 Resolution: 0.2 “/pix
58. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Moats Low velocity threshold: 400 m/s V moats = 0.67 km/s V h > 0.4 km/s Moats are closely associated with the presence of a penumbra.
59. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR None of the pores is associated with any moatlike flow. Strong neutral line Not clear evidence of moat flow Moats are absent in granulation regions located next to penumbral sides paralell to the direction of the filaments.
60. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Conclusions We have detected strong outflows (moats) associated to penumbrae ( mean speed 0.67 km/s, rms=0.32 km/s) Furthermore, moats do not developed in directions transversal to the penumbral filaments. Evidence suggestive of a link between moat flow and flows aligned with penumbral filaments (EF) Umbral core sides with no penumbrae do not display moat flows. Neutral lines are seem to play a role in the inhibition of moat flows in places where they are expected to be generated.
61. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Recent findings by Sainz Dalda & Martínez Pillet (2005), and Ravindra (2006) establish that the penumbral filaments extend beyond the photometric sunspot boundary and cross the region dominated by the moat flow. Cabrera Solana et al (2006) found Evershed clouds as precursors of MMFs around sunspots.
62. d) Flow field around solar pores e) Conclusions PART 2 Study of proper motions in solar active regions b) Proper motions in a complex AR c) Moat flows surrounding sunspots a) Solar active regions Extend the sample of solar active regions to consolidate the previous conclusions. Aim at: i.e establish whether the moat-penumbrae relation is sistematically found in other active regions. By using: Gound-based high-resolution observations 7 different sunspots series. Sunspots with different penumbral configurations.
63. d) Flow field around solar pores e) Conclusions PART 2 Study of proper motions in solar active regions b) Proper motions in a complex AR c) Moat flows surrounding sunspots a) Solar active regions 1m - Solar Swedish Tower (SST) S 1 AR440, 22 Aug 2003 S2 AR608, 10 May 2004 S5 AR789, 13 Jul 2005 S6 AR813, 04 Oct 2005 S3 AR662, 20 Aug 2004 S7 AR893, 10 Jun 2006 1 2 3 4 5 6 7 Observations S4 AR662, 21 Aug 2004 Restoration MFBD/MOMFB Time series > 40 min
64. PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Masking moats in 8 steps 1. Select the FOV to analyze. 2. Create a binary mask for the sunspots. 3. Compute the proper motions by LCT. 4. De-project velocities. 5. Create a binary mask using a velocity threshold. 6. Apply the mask to the flowmap in 3. 7. Create a binary mask of moats. 8. Plot the final flow map showing the moat flows.
65. PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Moat flows around sunspots (flowmaps)
66. Penumbral filaments extending radially from the umbra Peculiar regions PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Penumbral filaments curved, tangential to sunspot border No moatlike flows
67. PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Neutral lines affecting the flow behaviour
68. PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Conclusions Moat flows are oriented following the direction of the penumbral filaments. Umbral core sides with no penumbra do not display moat flows. Moat do not develop in the direction transverse to the penumbral filaments. No evidence of moats following penumbral filaments when having a change in the magnetic polarity.
69. b) Proper motions in a complex AR e) Conclusions c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions a) Solar active regions d) Flow field around solar pores Observing and analyzing pores. Since they do not have penumbra at all, our main conclusions. about moat-penumbra relation can be tested. Aim at: By using: Gound-based and space observations. Pores time series.
70. b) Proper motions in a complex AR e) Conclusions c) Moat flows surrounding sunspots a) Solar active regions d) Flow field around solar pores Ground-based observations SST 30 Sep 2007 Study of proper motions in solar active regions Active region NOAA 10971 Standard reduction and processing MOMFBD reconstructions G- band time series (50 min)
71. MOMFBD restorations d) Flow field around solar pores Study of proper motions in solar active regions
72. d) Flow field around solar pores General description of proper motions Study of proper motions in solar active regions Exploding granules
73. d) Flow field around solar pores Space observations HINODE 1 June 2007 30 Sep 2007 Study of proper motions in solar active regions Coordinated obs. with SST Alignment and subsonic filtering 60 min 14 hours
74. HINODE during 14 hours d) Flow field around solar pores Long-term evolution of the velocity field Study of proper motions in solar active regions
75. d) Flow field around solar pores Distribution of horizontal speeds Velocity magnitudes Low < 0.3 km/s Study of proper motions in solar active regions
76. d) Flow field around solar pores Velocity distribution around solar pores Study of proper motions in solar active regions
77. d) Flow field around solar pores Study of proper motions in solar active regions Radial directions Inward (-) Outward (+) t r r Pore center
78. d) Flow field around solar pores Study of proper motions in solar active regions Flow map Gradients Radial directions Cos Mask
79. d) Flow field around solar pores Study of proper motions in solar active regions Results FOV Cos In Out
80. d) Flow field around solar pores Study of proper motions in solar active regions Outflows display larger velocity magnitudes Inflows display lower velocity magnitudes
81. Conclusions First time we tested our algorithms in HINODE data. Flows calculated from different solar observations are coherent and show the overall influence of exploding events in the granulation around pores. Motions toward the pores in their nearest vicinity are dominant and are observed systematically. These motions are basically influenced by external plasma flows deposited by the exploding events. Definitely, there are no signs of moatlike flows around the pores. b) Proper motions in a complex AR d) Flow field around solar pores c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions a) Solar active regions e) Conclusions
82. Overall Conclusions The required software for restoration/inversion of IMaX images has been implemented in the context of this thesis and we make it available for the team. Our simulations validate the method proposed to calibrate the errors in the images of IMaX. PART 1 Defining a method for in-flight calibration of IMaX aberrations We have developed a method for the in-flight calibration of aberrations in IMaX. Note: Only 4 slides left !!
83. Moats do not appear in directions transversal to the penumbral filament ones. All detected properties for moats are also applicable to the Evershed Flow. Moats develop following the direction of the penumbral filaments in granulation surrounding sunspots. There are no signs of moatlike flows around the pores. Overall Conclusions PART 2 Study of proper motions in solar active regions Moats are found to be directly correlated to the presence of penumbra in sunspots. Neutral lines seem to play a role in the inhibition of moats.
84. Before this work .... So what ??? Final fate of the EF unknown. Origin of moat flow unclear. After this work .... EF transforms into moat flow. In agreement with Local Helioseismology ( f-modes ) evidence: moat flow is only 2 Mm deep.
91. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Using the map of average velocities we study the evolution of passive corks homogeneously distributed in the FOV Study of convective cells
92. d) Flow field around solar pores Space observations HINODE 1 June 2007 30 Sep 2007 Study of proper motions in solar active regions Coordinated obs. with SST Alignment and subsonic filtering 60 min 14 hours
93. Moat Granulation V h km/s PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots Threshold used when plotting velocities !!!
94. PART 2 Study of proper motions in solar active regions c) Moat flows surrounding sunspots De-projection of horizontal velocities Measured proper motions are in fact projections of the real horizontal velocities in the sunspot plane onto the plane perpendicular to LOS Sunspot System Observing System
95. PART 2 Study of proper motions in solar active regions b) Proper motions in a complex solar AR Proper motions inside penumbrae
96. Link between the moat flow and flows along the penumbral filaments (Evershed flow). Recent findings by Sainz Dalda & Martínez Pillet (2005) , Cabrera Solana et al (2006) and also Ravindra (2006) establish that the penumbral filaments extend beyond the photometric sunspot boundary and cross the region dominated by the moat flow. b) Proper motions in a complex AR d) Flow field around solar pores c) Moat flows surrounding sunspots PART 2 Study of proper motions in solar active regions a) Solar active regions e) Conclusions
97. d) Flow field around solar pores Study of proper motions in solar active regions Radial directions Inward (-) Outward (+) t r r Pore center
98. What for ???? The material presented here comes from the analysis of images in the continuum with short exposure times ~10 ms (static atmosphere) and combining many images (~100 continuum, ~1500 SOUP) but still low SNR values are reached. IMaX will do polarimetry with: negligible atmospheric turbulence, high SNR, diffraction limit, during hours and furthermore double spatial resolution (from 0.2 to 0.1 arcsec)
99. Why using speckle ???? The speckle summation has been employed as a way (resource) to determine the robustness of the calibration method we propose to characterize the aberrations in IMaX. though in the real case IMaX images are be meant to restored as single PD-pairs with no speckle summation at all.
100. Image blurring permitted for an instrument can be specified by the diameter of the blur spot or angle subtended by it. For instance, we can select the angle as the value of the diffraction cut-off that is slightly greater than the Airy FWHM. Nevertheless this criterion is quite severe and some more flexible ones establish the limit of the defocus tolerance based on the loss of intensity in the central part of the PSF. Defocus Tolerance
101. Why PD if it does not reproduce exactly the WFE ?? We get reliable OTFs to solve our deconvolution problem. Because The error metric depends directly on this OTF. Dispersion of coefficients is low and we do not expect cancellations in the WFE. Repeatability We have inverted real images for different noise realizations and the dispersion of the wavefront is small.
102. Why uncorrelated signal and noise assumption ?? Photon noise is certainly a function of the intensity there are some other noise contributions: Readout and noise related to the fluctuations in atmospheric transparency which are not Nevertheless, Uncorrelated noise and signal is in general a useful approximation giving good results in simulations
103. Small-scale irregularities in the wavefront error are not detectable by the PD-code if we use a finite (rather low) number of Zernike terms. Please goto Pag 78. This limitation mainly produces stray-light over the restored image and consequently a loss of contrast. This effect is tolerable within certain margins, and fixes constraints to the polishing quality in the SUNRISE main mirror and the inhomogeneities in the IMaX etalon.
104. The residual errors in the proposed calibration method induce, in turn, errors in the subsequent restoration mean ( i t - i r ) < 2.5% loss of contrast < 5% IMaX case
Same trend in blue and red histograms. Red one shifted to the right respect to blue. Within the moats, standard velocity values for quiet granulation are still present but with a lower weight.