The document discusses the atmospheres of terrestrial planets. It begins by defining what an atmosphere is and its basic structure. It then discusses atmospheric structure and composition for Earth, Venus, and Mars. Key points are made about how planetary atmospheres developed over time based on interactions between gravity, heating from the sun, and geological processes like volcanism. The document notes that atmospheric conditions on these planets have changed dramatically since their formations.
Site of asteroid impact changed the history of life on Earth: the low probabi...Sérgio Sacani
Sixty-six million years ago, an asteroid approximately 9km in diameter hit the hydrocarbon- and
sulfur-rich sedimentary rocks in what is now Mexico. Recent studies have shown that this impact at
the Yucatan Peninsula heated the hydrocarbon and sulfur in these rocks, forming stratospheric soot
and sulfate aerosols and causing extreme global cooling and drought. These events triggered a mass
extinction, including dinosaurs, and led to the subsequent macroevolution of mammals. The amount
of hydrocarbon and sulfur in rocks varies widely, depending on location, which suggests that cooling
and extinction levels were dependent on impact site. Here we show that the probability of signifcant
global cooling, mass extinction, and the subsequent appearance of mammals was quite low after an
asteroid impact on the Earth’s surface. This signifcant event could have occurred if the asteroid hit the
hydrocarbon-rich areas occupying approximately 13% of the Earth’s surface. The site of asteroid impact,
therefore, changed the history of life on Earth.
09-28-17 Lifelong Learning Lecture: Jim HaynesEllsworth1835
"Natural and Human Causes of Climate Change: What Scientists Know and How They Know It"
Presented by James M. Haynes, PhD, Interim Provost and Vice President for Academic Affairs, Professor of Environmental Science and Ecology
For eons, six slowly, often intermittently acting natural forces have changed the Earth's temperature within a range of +7 degrees Fahrenheit, leading to climate swings from ice ages to planet-wide tropical conditions. Now, a seventh rapidly acting force is changing climate—modern human civilization. What evidences of climate change are observed today, and what is likely to happen to our children and generations beyond as a result of human activity in the recent past and today? What can we do to minimize the impacts of the changes to come?
This presentation briefly describes the term - climate change and what we know and what we don't know. The intention was to understand the ideology of the term, framing of the term and politics behind this.
En la siguiente presentación se realizo un extracto muy especifico desde el punto de vista de la Astronomía, dando a conocer nuestro sistema solar o universo, los planetas, las lunas mas características de nuestro universo y algo mas de nuestro planeta, también viendo las características especificas de cada planeta o luna mas representativas y por eso la denominación viajando por el universo.
En la presente se muestra un poco mas sobre una de las lunas que tiene Saturno, cual es en este caso Titan es importante por sus características atmosféricas pues esta compuesto por Metano, nitrógeno y argón mayoritariamente, también que es de mucho interés para NASA quien esta realizando un seguimiento exhaustivo mediante un sofisticado equipo que órbita Saturno Cassini Huygens
Site of asteroid impact changed the history of life on Earth: the low probabi...Sérgio Sacani
Sixty-six million years ago, an asteroid approximately 9km in diameter hit the hydrocarbon- and
sulfur-rich sedimentary rocks in what is now Mexico. Recent studies have shown that this impact at
the Yucatan Peninsula heated the hydrocarbon and sulfur in these rocks, forming stratospheric soot
and sulfate aerosols and causing extreme global cooling and drought. These events triggered a mass
extinction, including dinosaurs, and led to the subsequent macroevolution of mammals. The amount
of hydrocarbon and sulfur in rocks varies widely, depending on location, which suggests that cooling
and extinction levels were dependent on impact site. Here we show that the probability of signifcant
global cooling, mass extinction, and the subsequent appearance of mammals was quite low after an
asteroid impact on the Earth’s surface. This signifcant event could have occurred if the asteroid hit the
hydrocarbon-rich areas occupying approximately 13% of the Earth’s surface. The site of asteroid impact,
therefore, changed the history of life on Earth.
09-28-17 Lifelong Learning Lecture: Jim HaynesEllsworth1835
"Natural and Human Causes of Climate Change: What Scientists Know and How They Know It"
Presented by James M. Haynes, PhD, Interim Provost and Vice President for Academic Affairs, Professor of Environmental Science and Ecology
For eons, six slowly, often intermittently acting natural forces have changed the Earth's temperature within a range of +7 degrees Fahrenheit, leading to climate swings from ice ages to planet-wide tropical conditions. Now, a seventh rapidly acting force is changing climate—modern human civilization. What evidences of climate change are observed today, and what is likely to happen to our children and generations beyond as a result of human activity in the recent past and today? What can we do to minimize the impacts of the changes to come?
This presentation briefly describes the term - climate change and what we know and what we don't know. The intention was to understand the ideology of the term, framing of the term and politics behind this.
En la siguiente presentación se realizo un extracto muy especifico desde el punto de vista de la Astronomía, dando a conocer nuestro sistema solar o universo, los planetas, las lunas mas características de nuestro universo y algo mas de nuestro planeta, también viendo las características especificas de cada planeta o luna mas representativas y por eso la denominación viajando por el universo.
En la presente se muestra un poco mas sobre una de las lunas que tiene Saturno, cual es en este caso Titan es importante por sus características atmosféricas pues esta compuesto por Metano, nitrógeno y argón mayoritariamente, también que es de mucho interés para NASA quien esta realizando un seguimiento exhaustivo mediante un sofisticado equipo que órbita Saturno Cassini Huygens
Saturn´s Moon Titan shows many incredible features as; only liquid bodies observed in the solar other than Earth, huge seas of hydrocarbons, only moon with a thick atmosphere and also are similar to Earth in that it is dominated by nitrogen, methane and argon. Surface features consistent with erosion and however, it seems highly doubtful it is a good candidate for life.
La razón principal para el estudio de atmósferas planetarias es tratar de entender el origen y evolución de la atmósfera de la tierra. Por supuesto, en el intento de comprender el funcionamiento de nuestro sistema solar o incluso la evolución de la Tierra como un organismo, la atmósfera de la tierra es esencialmente irrelevante, ya que su masa es despreciable.
The international Cassini-Huygens spacecraft was launched on October 15, 1997 and had a marathon 7-year 2-billion mile journey to the distant planet Saturn. The 23-foot tall, 14-foot wide, 6-ton spacecraft is the largest most sophisticated outer planet spacecraft ever built, and is in its third year of operation in orbit around the planet Saturn. Cassini-Huygens has been returning extraordinary data about the entire Saturn system: the spectacular rings; the numerous icy satellites with a variety of unique surface features; the giant planet itself; a huge magneto-sphere teeming with particles that interact with the rings and moons; and the intriguing moon Titan, which is slightly larger than the planet Mercury, and whose hazy atmosphere is denser than that of Earth. This talk will be an overview of the Cassini-Huygens mission to Saturn with a summary of the top science returns of its first three years in orbit.
The Minnesota Space Grant Consortium, run out of the Department of Aerospace Engineering and Mechanics at the University of Minnesota, hosts Trina Ray of NASA JPL on January 22, 2008.
El presente estudio tuvo como finalidad aplicar una metodología simple y eficaz para diferentes análisis de suelos hiperaridos, el cual nos sirvió para poder hacer una demostración de la presencia de vida en este tipo de suelos análogos al planeta marte. Esta aplicación se realizo en el desierto de La Joya-Arequipa, Perú y en el desierto de Atacama, Chile.
Variables Meteorológicas en el Desierto de la Joya - Perú.Renée Condori Apaza
El presente trabajo de investigación es uno más de los realizados por un grupo multidisciplinario de profesionales que están realizando estudios desde el punto de vista búsqueda de vida en lugares análogos al Planeta Marte a nivel mundial en desiertos como; Atacama-Chile, La Joya-Perú, Mojave-USA y en otros lugares similares.
Esto quiere decir estudios, químicos, microbiológicos, geología y geofisica de los desiertos, climatología de los lugares de interés y sistemas de navegación y telecomunicaciones, entre otros.
Earth’s atmosphere is slightly warmer than what it should be due to direct solar heating because of a mild case of greenhouse effect…
The ground is heated by visible and (some) infrared light from the Sun.
The heated surface emits infrared light.
The majority of Earth’s atmosphere (N2 and O2) are not good greenhouse gas.
The small amount of greenhouse gases (H2O, CO2) traps (absorb and re-emit) the infrared radiation, increasing the temperature of the atmosphere…
The Origin of the Earth’s Atmosphere: Still Many UncertaintiesEzioAang
About 4.5 billion years ago, Earth formed out of nebula of gases and dust that were to become the solar system
Small objects--called planetoids-- accreted or combined together to build larger objects…such as planets
The early atmosphere would have been similar to the Sun--mainly hydrogen and helium, but this atmosphere was lost quickly for two reasons:
(1) The gravity of the modest size earth was not strong enough to prevent such light gases from escaping to space. Particularly since the early earth was hot!
(2) It appears that around 30 million years after the earth’s formation, it was struck by a large object…the size of Mars. The result: the origin of the moon and loss of earth’s early H, He atmosphere.
The surface of the earth during this period was extremely hot with numerous volcanoes
The earth was under near constant bombardment by objects of varying sizes
Slowly, the earth started to cool down and the second atmosphere began to form.
A new atmosphere was established by the outgasing of volcanoes…the mixture of gases was probably similar to those of today’s volcanoes:
H20 vapor (roughly 80%)
CO2 (roughly 10%)
N2 (few percent)
Small amounts of CO, HCL, HS (Hydrogen Sulfide), SO2, CH4 (Methane), Ammonia (NH3), and other trace gases.
Virtually no oxygen in that second atmosphere.
Thus, no ozone layer, so ultraviolet radiation flooded the earth’s surface.
With a huge influx of water vapor and the cooling of the planet, clouds and earth’s oceans formed.
At that time the sun was about 30% weaker than today…why didn’t the earth freeze over?
The apparent reason: so much CO2 so there was a very strong greenhouse effect.
In the first two billion years of the planet’s evolution, the atmosphere acquired a small amount of oxygen, probably by the splitting of water (H20) molecules by solar radiation.
The evidence of this oxygen is suggested by minor rust in some early rocks.
The oxygen also led to the establishment of an ozone layer that reduced UV radiation at the surface.
With the rise of photosynthetic bacteria (cyanobacteria) and early plants, oxygen levels began to rise rapidly as did indications of rust in rocks
Between 2.5 billion years ago to about 500 bya, 02 rose to near current levels.
While O2 was increasing, CO2 decreased due to several reasons:
(1) In photosynthesis CO2 is used to produce organic matter, some of which is lost to the system (e.g., drops to the bottom of the ocean or is buried)
(2) chemical weathering, which removes CO2
Sulfur compounds were taken out of the atmosphere as acid rain and were deposited on the ground as sulfates.
N2 gas increased slowly but progressively since it was relatively inert.
Current composition of the atmosphere was established approximately a billion years ago.
With lower CO2 levels the earth became more susceptable to ice ages when solar radiation decreases due to orbital variations,
It appears that around 750-550 million years ago the earth cooled down and became nearly entirely glaciated.
Climate Change
Investigation
Manual
ENVIRONMENTAL SCIENCE
CLIMATE CHANGE
Overview
In this lab, students will carry out several activities aimed at
demonstrating consequences of anthropogenic carbon emissions,
climate change, and sea level rise. To do this, students will model
how certain gases in Earth’s atmosphere trap heat and then how
different colors and textures of surfaces reflect differing amounts
of sunlight back into space. They will create models of sea level
rise resulting from melting of sea ice and glacial ice and examine
the effects of this potential consequence of climate change.
Students will critically examine the model systems they used in
the experiments.
Outcomes
• Explain the causes of increased carbon emissions and their likely
effect on global climate.
• Discuss positive and negative climate feedback.
• Distinguish between glacial ice melt and oceanic ice melt.
Time Requirements
Preparation ..................................................................... 15 minutes
Activity 1: Modeling the Greenhouse Effect ................... 30 minutes
Activity 2: Modeling Albedo ........................................... 40 minutes
Activity 3: Sea Ice, Glacial Ice, and Sea Level Rise ....... 30 minutes
2 Carolina Distance Learning
Key
Personal protective
equipment
(PPE)
goggles gloves apron
follow
link to
video
photograph
results and
submit
stopwatch
required
warning corrosion flammable toxic environment health hazard
Made ADA compliant by
NetCentric Technologies using
the CommonLook® software
Table of Contents
2 Overview
2 Outcomes
2 Time Requirements
3 Background
9 Materials
9 Safety
9 Preparation
10 Activity 1
11 Activity 2
12 Activity 3
13 Graphing
13 Submission
13 Disposal and Cleanup
14 Lab Worksheet
Background
For the last 30 years, controversy has
surrounded the ideas of global warming/climate
change. However, the scientific concepts behind
the theory are not new. In the 1820s, Joseph
Fourier was the first to recognize that, given
the earth’s size and distance from the sun,
the planet’s surface temperature should be
considerably cooler than it was. He proposed
several mechanisms to explain why the earth
was warmer than his calculations predicted,
one of which was that the earth’s atmosphere
might act as an insulator. Forty years later,
John Tyndall demonstrated that different
gases have different capacities to absorb
infrared radiation, most notably methane (CH4),
carbon dioxide (CO2), and water vapor (H2O),
all of which are present in the atmosphere. In
1896, Svante Arrhenius developed the first
mathematical model of the effect of increased
CO2 levels on temperature. His model predicted
that a doubling of the amount of CO2 in the
atmosphere would produce a 5–6 °C increase
in temperature globally. Based on the level of
CO2 production in the late 19th century, he
predicted that this change would take place
over thousands of years, if at ...
The universe began about 14.4 billion years ago.
The Big Bang Theory states that, in the beginning, the universe was all in one place.
To know more, see the presentation.
Exposición en el seminario Internacional del Colegio de Ingenieros del Perú-Consejo Departamental Arequipa, sobre parte de una investigación en el ecosistema acuático marino del puerto de Ilo, respecto a la contaminación por metales pesados y utilizando la tecnica analitica de espectrofotometria de absorcion atómica y respectiva evaluación con estándares de ECAs-Perú y USEPA.
El presente proyecto es un prototipo que se viene desarrollando en la ciudad de Ilo por parte de un grupo multidisciplinario, como un aporte en la mejora y salud de personas que trabajan segregando residuos sólidos, vemos que este proyecto también se puede aplicar en diferentes escenarios de la industria previo entrenamiento respectivo.
Diseño y Estructura de un Brazo Robot Seleccionador de ObjetosRenée Condori Apaza
La presentación es la primera etapa sobre diseño y estructura del brazo seleccionador de objetos el cual se enfocara en la selección de residuos sólidos con el fin del cuidado de la salud pública y obtención de materia prima para próximo uso como se explico en el presente evento. producido por EPISI UNAM- ILO.
Se presenta una breve resumen de la investigación científica que se viene desarrollando con información preliminar de los estudios de los ecosistema acuático marinos del puerto de Ilo en conmemoración de un aniversario mas de la Escuela Profesional de Ingeniería Ambiental EPIAM-ILO.
Ponencia sobre el día del Agua que fue realizado por el Colegio de Ingenieros del Perú - Arequipa. Proyecto que se realizó y que se viene realizando para conocer la calidad del agua de mar y del ecosistema marino en el puerto de Ilo
La presentación es una descripción y la importancia de la Ingeniería Química en nuestro planeta y en el dia a dia de nuestra población, en cuanto a las necesidades. el proceso industrial y protección de los recursos y el medio ambiente. Desarrollado en el evento organizado por el Colegio de Ingenieros del Perú - Arequipa, Capitulo de Ingenieria Quimica.
Presentación que se desarrollo para la población estudiantil y publico en general en la ciudad de Huarmey y por invitación de la SubGerencia de Gestión Ambiental del Municipio Provincial de Huarmey, en favor de concientizar y brindar educación ambiental a la población, gracias por esta oportunidad.
Investigación y tecnología del agua (Continentales y Marino Costeros)Renée Condori Apaza
La presente es una breve descripción de lo que se viene realizando en la Universidad Nacional de Moquegua para conocer como estamos en cuanto a la calidad de agua en los diferentes ecosistemas acuáticos y como9 esto sirve como una herramienta para tomar decisiones en las mejoras futras de mano con la sociedad en esta ciudad de Moquegua.
La presente presentación es el trabajo realizado por un grupo de trabajo de Escuela Profesional de Ingeniería Ambiental de la Universidad Nacional de Moquegua, se desarrollo muestreo y monitoreo en el distrito de Ichuña en Sánchez Cerro Moquegua, Perú. Fue realizar análisis de metales pesados en los manantiales de Humalzo, Totorani y Mauri.
En este trabajo detallamos como es el comportamiento del evento del niño y la niña en la parte sur de nuestro planeta y como es que influye directamente dentro del cambio climático en las ultimas décadas con mayor fuerza, donde se manifiesta con graves daños a la población y en la economía. Tenemos que empezar a respetar y cuidar la naturaleza nuestro único hogar por ahora accesible el planeta tierra.
CLIMATOLOGÍA EN LA FRANJA DESÉRTICA DE ILO-PERU (METEOROLÓGIA Y CLIMA)Renée Condori Apaza
Estudio de parámetros meteorológicos en la franja desértica de la ciudad de Ilo-Perú, la diferencia de micro climas en dos puntos distintos (Lomas de Ilo y Algarrobal). La investigación fue desarrollada por un grupo de investigación de Ingeniería Ambiental de la Universidad Nacional de Moquegua. Por un periodo de dos meses(Octubre a Diciembre de 2017) donde podemos ver el cambio extremo que existe en ambos lugares. Los pobladores de la ciudad de Ilo y moquegua mencionan que las lomas de Ilo hace 50 años atrás eraun lugar donde era prospera la agricultura y ganadería, también que había pequeñas lagunas, un verdadero ecosistema para nuestros tiempos.
Breve explicación de Cambio Climático; de donde proviene, porque se da y las consecuencias. También desde el punto de vista de la Ingeniería Ambiental como se realiza la aplicación de la encomia ambiental en la valoración en la minimizacion de CO2 o como retribuir por la contaminación atmosférica.
En esta presentación tenemos el análisis de la Teoría de Gaia establecida por el científico Lovelock el cual nos brinda antecedentes y datos de como el cambio climático se da y viene dando en nuestro planeta Tierra, siendo los compuestos que mas directamente se relacionan con este fenómeno, el aumento del CO2 y los cambios bruscos delos estados del agua el cual es un termo regulador de temperatura en nuestro planeta.
Aquí se hace un análisis sobre el calentamiento global en nuestro planeta o lo que se conoce como aumento de la temperatura en la tierra, según postulado del Dr. Hansen y sus dos puntos de vista las causas. Como parte de la Ingeniería Ambiental nosotros lo analizamos y en parte estamos de acuerdo que la fuente antropológica lo que hace es acelerar los cambios en nuestro clima tal como lo estamos viviendo ahora.
Importancia de las Pampas de la Joya como análogo a MarteRenée Condori Apaza
En el presente documento se da a conocer la importancia del Desierto de la Joya para realizar estudios sobre un ambiente similar al Planeta Marte, como se inicio y quienes actúan en este trabajo que viene realizándose desde el 2004 a la fecha.
La siguiente presentación es un resumen sobre el área de estudio que concierne al desierto de la Joya en Arequipa -Perú.Con imagenes panorámicas y es ecosistema presente en el área,también la climatología y estudios que se realizaron y se continúan haciendo en el desierto de la Joya, Todo esto gracias al grupo multidisciplinario conformado por investigadores nacionales e internacionales.
Esta presentación la realice en un forum organizado por el distrito de torata, en el cual se muestra las diferentes formas de contaminación ambiental y como la minería de alguna manera como empresa económicamente activa es buena y como también pueden dañar nuestro medio ambiente si no llevan un control adecuado en sus procesos y mejora del hábitat donde se desarrollan. También se ve que es útil la presencia de un laboratorio de control ambiental para una vigilancia adecuada del medio ambiente.
En esta presentación se detalla el trabajo realizado en laboratorio y campo sobre la importancia de horas frió en semillas de frutos para obtener buenos plantones, tambien se logra demostrar como y cuando es bueno o no usar el AG3, el cual es el Ácido Giberelico una hormona que sirve para ayudar al buen desarrollo de los plantones y primordial en monitoreo de temperaturas y humedad relativa para un buen tratamiento de horas frió en semillas de frutas como es el presente estudio.
La siguiente presentación tiene por objetivo informar en forma breve sobre un plan de manejo ambiental y muy especifico lo que es Mitigacion, el cual es primordial para un buen manejo de antes durante y después de una obra o proyecto donde siempre debe tenerse un cuidado con el hábitat o medio ambiente donde vivimos.
La presente trata sobre Monitoreo Ambiental del Aire, un resumen de la atmósfera de nuestro planeta, parámetros que se miden en el aire y la ley vigente en nuestro país con parámetros que se deben medir para una mejor calidad de vida, también se muestran equipos que se usan para tomar data de diferentes agentes presentes en nuestra atmósfera y en especial el equipo con el que trabajamos para medir material particulado como PM10 Y PM2.5
Observability Concepts EVERY Developer Should Know -- DeveloperWeek Europe.pdfPaige Cruz
Monitoring and observability aren’t traditionally found in software curriculums and many of us cobble this knowledge together from whatever vendor or ecosystem we were first introduced to and whatever is a part of your current company’s observability stack.
While the dev and ops silo continues to crumble….many organizations still relegate monitoring & observability as the purview of ops, infra and SRE teams. This is a mistake - achieving a highly observable system requires collaboration up and down the stack.
I, a former op, would like to extend an invitation to all application developers to join the observability party will share these foundational concepts to build on:
A tale of scale & speed: How the US Navy is enabling software delivery from l...sonjaschweigert1
Rapid and secure feature delivery is a goal across every application team and every branch of the DoD. The Navy’s DevSecOps platform, Party Barge, has achieved:
- Reduction in onboarding time from 5 weeks to 1 day
- Improved developer experience and productivity through actionable findings and reduction of false positives
- Maintenance of superior security standards and inherent policy enforcement with Authorization to Operate (ATO)
Development teams can ship efficiently and ensure applications are cyber ready for Navy Authorizing Officials (AOs). In this webinar, Sigma Defense and Anchore will give attendees a look behind the scenes and demo secure pipeline automation and security artifacts that speed up application ATO and time to production.
We will cover:
- How to remove silos in DevSecOps
- How to build efficient development pipeline roles and component templates
- How to deliver security artifacts that matter for ATO’s (SBOMs, vulnerability reports, and policy evidence)
- How to streamline operations with automated policy checks on container images
PHP Frameworks: I want to break free (IPC Berlin 2024)Ralf Eggert
In this presentation, we examine the challenges and limitations of relying too heavily on PHP frameworks in web development. We discuss the history of PHP and its frameworks to understand how this dependence has evolved. The focus will be on providing concrete tips and strategies to reduce reliance on these frameworks, based on real-world examples and practical considerations. The goal is to equip developers with the skills and knowledge to create more flexible and future-proof web applications. We'll explore the importance of maintaining autonomy in a rapidly changing tech landscape and how to make informed decisions in PHP development.
This talk is aimed at encouraging a more independent approach to using PHP frameworks, moving towards a more flexible and future-proof approach to PHP development.
Transcript: Selling digital books in 2024: Insights from industry leaders - T...BookNet Canada
The publishing industry has been selling digital audiobooks and ebooks for over a decade and has found its groove. What’s changed? What has stayed the same? Where do we go from here? Join a group of leading sales peers from across the industry for a conversation about the lessons learned since the popularization of digital books, best practices, digital book supply chain management, and more.
Link to video recording: https://bnctechforum.ca/sessions/selling-digital-books-in-2024-insights-from-industry-leaders/
Presented by BookNet Canada on May 28, 2024, with support from the Department of Canadian Heritage.
Elevating Tactical DDD Patterns Through Object CalisthenicsDorra BARTAGUIZ
After immersing yourself in the blue book and its red counterpart, attending DDD-focused conferences, and applying tactical patterns, you're left with a crucial question: How do I ensure my design is effective? Tactical patterns within Domain-Driven Design (DDD) serve as guiding principles for creating clear and manageable domain models. However, achieving success with these patterns requires additional guidance. Interestingly, we've observed that a set of constraints initially designed for training purposes remarkably aligns with effective pattern implementation, offering a more ‘mechanical’ approach. Let's explore together how Object Calisthenics can elevate the design of your tactical DDD patterns, offering concrete help for those venturing into DDD for the first time!
Generative AI Deep Dive: Advancing from Proof of Concept to ProductionAggregage
Join Maher Hanafi, VP of Engineering at Betterworks, in this new session where he'll share a practical framework to transform Gen AI prototypes into impactful products! He'll delve into the complexities of data collection and management, model selection and optimization, and ensuring security, scalability, and responsible use.
LF Energy Webinar: Electrical Grid Modelling and Simulation Through PowSyBl -...DanBrown980551
Do you want to learn how to model and simulate an electrical network from scratch in under an hour?
Then welcome to this PowSyBl workshop, hosted by Rte, the French Transmission System Operator (TSO)!
During the webinar, you will discover the PowSyBl ecosystem as well as handle and study an electrical network through an interactive Python notebook.
PowSyBl is an open source project hosted by LF Energy, which offers a comprehensive set of features for electrical grid modelling and simulation. Among other advanced features, PowSyBl provides:
- A fully editable and extendable library for grid component modelling;
- Visualization tools to display your network;
- Grid simulation tools, such as power flows, security analyses (with or without remedial actions) and sensitivity analyses;
The framework is mostly written in Java, with a Python binding so that Python developers can access PowSyBl functionalities as well.
What you will learn during the webinar:
- For beginners: discover PowSyBl's functionalities through a quick general presentation and the notebook, without needing any expert coding skills;
- For advanced developers: master the skills to efficiently apply PowSyBl functionalities to your real-world scenarios.
The Art of the Pitch: WordPress Relationships and SalesLaura Byrne
Clients don’t know what they don’t know. What web solutions are right for them? How does WordPress come into the picture? How do you make sure you understand scope and timeline? What do you do if sometime changes?
All these questions and more will be explored as we talk about matching clients’ needs with what your agency offers without pulling teeth or pulling your hair out. Practical tips, and strategies for successful relationship building that leads to closing the deal.
UiPath Test Automation using UiPath Test Suite series, part 4DianaGray10
Welcome to UiPath Test Automation using UiPath Test Suite series part 4. In this session, we will cover Test Manager overview along with SAP heatmap.
The UiPath Test Manager overview with SAP heatmap webinar offers a concise yet comprehensive exploration of the role of a Test Manager within SAP environments, coupled with the utilization of heatmaps for effective testing strategies.
Participants will gain insights into the responsibilities, challenges, and best practices associated with test management in SAP projects. Additionally, the webinar delves into the significance of heatmaps as a visual aid for identifying testing priorities, areas of risk, and resource allocation within SAP landscapes. Through this session, attendees can expect to enhance their understanding of test management principles while learning practical approaches to optimize testing processes in SAP environments using heatmap visualization techniques
What will you get from this session?
1. Insights into SAP testing best practices
2. Heatmap utilization for testing
3. Optimization of testing processes
4. Demo
Topics covered:
Execution from the test manager
Orchestrator execution result
Defect reporting
SAP heatmap example with demo
Speaker:
Deepak Rai, Automation Practice Lead, Boundaryless Group and UiPath MVP
Key Trends Shaping the Future of Infrastructure.pdfCheryl Hung
Keynote at DIGIT West Expo, Glasgow on 29 May 2024.
Cheryl Hung, ochery.com
Sr Director, Infrastructure Ecosystem, Arm.
The key trends across hardware, cloud and open-source; exploring how these areas are likely to mature and develop over the short and long-term, and then considering how organisations can position themselves to adapt and thrive.
SAP Sapphire 2024 - ASUG301 building better apps with SAP Fiori.pdfPeter Spielvogel
Building better applications for business users with SAP Fiori.
• What is SAP Fiori and why it matters to you
• How a better user experience drives measurable business benefits
• How to get started with SAP Fiori today
• How SAP Fiori elements accelerates application development
• How SAP Build Code includes SAP Fiori tools and other generative artificial intelligence capabilities
• How SAP Fiori paves the way for using AI in SAP apps
Assuring Contact Center Experiences for Your Customers With ThousandEyes
Planetary Atmospheres II
1. Planetary Atmospheres II
Planets and Planetary
Systems
RENEE CONDORI APAZA, JULIO
VALDIVIA SILVA, Christopher P.
McKay
The Advanced Studies Laboratories
2. What is an atmosphere?, What is its structure?
Temperature of a planet, neglecting effects of
atmosphere (“no-greenhouse temperatures”)
Generic atmospheric structure
Global climate change
Earth
Venus
Mars
3. • Planetary atmospheres as a balancing act:
– Gravity vs. thermal motions of air molecules
– Heating by Sun vs. heat radiated back into space
– Weather as a way to equalize pressures at different places on a
planet’s surface
• Atmospheres of terrestrial planets are very different now
from the way they were born
– Formation: volcanoes, comets
– Destruction: escape, incorporation into rocks, oceans
– Huge changes over a billion years or less
• Prospect of human-induced global warming on Earth needs
to be taken seriously
4. • Earth diameter
~ 12,000 km
• Top of troposphere
~ 12 km
• Thickness of
atmosphere divided
by Earth diameter = 1 /
1000
5. • About 10 km thick
• Consists mostly of
molecular nitrogen (N2)
and oxygen (O2)
• Fractions:
– 78% Nitrogen
– 21% Oxygen
– 0.04% CO2
7. Mathematically: p nkT. Units: energy per unit volume or force per unit area
n number density (molecules per cubic cm),
T temperature (deg Kelvin), k Boltzmann constant, Units of kT : energy
8. • Pressure and density
decrease with altitude
because the weight of
overlying layers is less
• Earth’s pressure at sea
level is
– 1.03 kg per sq. meter
– 14.7 lbs per sq. inch
– 1 bar
10. h
P
h
0
P0
/e
• Pressure, density fall off exponentially with altitude
• Higher temperature T larger “scale height” h0
• Stronger gravity g shorter “scale height” h0
13. • Create pressure that determines whether liquid water
can exist on surface
• Absorb and scatter light
• Create wind, weather, and climate
• Interact with solar wind to create a magnetosphere
• Can make planetary surfaces warmer through
greenhouse effect
16. Conclusion: for Venus and Earth, at least, something else is
going on! (not just radiation into space.
17. • Ionization: Removal of
an electron
• Dissociation: Destruction
of a molecule
• Scattering: Change in
photon’s direction
• Absorption: Photon’s
energy is absorbed
18.
19.
20. • carbon dioxide CO2
• water vapor H20
• methane CH4
• others too (NO2, ....)
• More greenhouse gases in atmosphere can
lead to higher surface temperatures.
21.
22.
23.
24. • What would happen to Earth’s temperature if
Earth’s surface were less reflective?
a) It would go up.
b) It would go down.
c) It wouldn’t change
• This is one of the factors exacerbating global
warming.
– As more arctic ice melts in summer, arctic
ocean absorbs more light, temperature
rises
25.
26. • Ultraviolet light
can break up
O2 molecules,
allowing ozone
(O3) to form
• Without plants
to release O2,
there would be
no ozone in
stratosphere to
absorb UV
light
27. • Ultra-violet light from Sun dissociates oxygen
molecules O2 to produce O in stratosphere
• O combines with O2 to form O3 (ozone)
• Ozone in stratosphere absorbs harmful ultraviolet
light from Sun, providing land-based life with a
protective shield
• Manmade aerosols (chlorofluorocarbons, CFCs)
can inhibit ozone formation
• Result: “Ozone hole”
29. ?
• Why is ozone hole much deeper and larger in
the Antarctic than in the arctic?
– During winter, clouds form in the Antarctic ozone
layer.
– Chemical reactions on ice particles in the clouds
activate ozone destroying substances.
– In spring, these substances take part in chemical
reactions that destroy ozone.
• Arctic: warmer than Antarctic (fewer ice
clouds), more irregular air circulation
30. • Huge changes took place over the 4.6 billion
years since planets formed!
• Early atmospheres didn’t resemble current
ones at all
• Question: why are atmospheres of Venus,
Earth, Mars so different?
35. Moon Mercury
• Very sensitive measurements show Moon and
Mercury have extremely thin atmospheres
• Gas comes from impacts that eject surface atoms
36. • Why are they so different?
• Were they always this different from each other?
37. First Atmosphere: Primordial elements
Composition - Probably H2, He
Today these gases are relatively rare on Earth compared to other
places in the universe.
Were probably lost to space early in Earth's history because
Earth's gravity is not strong enough to hold lightest gases
Earth still did not have a differentiated core (solid inner/liquid
outer core) which creates Earth's magnetic field
(magnetosphere = Van Allen Belt) which deflects solar wind.
Magnetosphere protects any atmosphere from the solar wind.
Once the core differentiated, gases could be retained.
38. Gases similar to those from
modern volcanoes (H2O, CO2,
SO2, CO, S2, Cl2, N2, H2) and NH3
(ammonia) and CH4 (methane)
No free oxygen (O2 not found in
volcanic gases)
Ocean Formation - As Earth
cooled, H2O produced by
outgassing could exist as liquid
CO2 could then dissolve in
ocean, be sequestered in
marine sediments
39. Today, atmosphere is ~21% free oxygen. How did oxygen reach this level?
Oxygen Production
Photochemical dissociation - breakup of water molecules by ultraviolet light
Produced O2 levels 1-2% current levels
At these levels O3 (Ozone) could form to shield Earth surface from UV
Photosynthesis: CO2 + H2O + sunlight = organic compounds + O2 -
produced by cyanobacteria, and eventually higher plants - supplied the rest
of O2 to atmosphere.
Oxygen Consumers
Chemical Weathering - through oxidation of surface materials (early
consumer)
Respiration (much later)
Burning of Fossil Fuels (much, much later)
Once rocks at the surface were sufficiently oxidized, more oxygen could remain
free in the atmosphere
40. The Carbon Dioxide Cycle 1. Atmospheric CO2
dissolves in rainwater
2. Rain erodes minerals
which flow into ocean
3. Minerals combine with
carbon to make rocks
on ocean floor
4. Subduction carries
carbonate rocks down
into mantle
5. Rocks melt in mantle
and outgas CO2 back
into atmosphere
through volcanoes
41. Cooling allows CO2 to build up in atmosphere
Heating causes rain to reduce CO2 in atmosphere
42. • The first photosynthesis
–Consumes CO2,
release O2
43. Chemical building blocks of life could not have formed in the
presence of atmospheric oxygen. Chemical reactions that yield
amino acids are inhibited by presence of very small amounts of
oxygen.
Oxygen prevents growth of the most primitive living bacteria
such as photosynthetic bacteria, methane-producing bacteria
and bacteria that derive energy from fermentation.
Conclusion - Since today's most primitive life forms are
anaerobic (don’t need oxygen), the first forms of cellular life
probably had similar metabolisms.
Today these anaerobic life forms are restricted to anoxic (low
oxygen) habitats such as swamps, ponds, and lagoons.
44.
45. Potential source of the Earth's ocean water is
comet-like balls of ice.
Enter atmosphere at rate of about 20/second.
Four billion years of such bombardment would
give enough water to fill the oceans to their
present volume.
Possible problems with isotope ratios. Under
active research.
46. Solar Brightening
• Sun very gradually grows brighter with time, increasing
the amount of sunlight warming planets
47. Changes in Axis Tilt
• Greater tilt makes more extreme seasons, while smaller
tilt keeps polar regions colder.
48. Changes in Reflectivity
• Higher reflectivity tends to cool a planet, while lower
reflectivity leads to warming
49. Changes in Greenhouse Gases
• Increase in greenhouse gases leads to warming, while a
decrease leads to cooling
50. • Global temperatures
have tracked CO2
concentration for last
500,000 years
• Antarctic air bubbles
indicate current CO2
concentration is
highest in at least
500,000 years
51. • Most of CO2 increase has happened in last 50 years!
55. Increased Glacier retreat
since the early 1990s
Area of seasonally frozen
ground in NH has decreased
by 7% from 1901 to 2002
IPCC Report 2007
56.
57. CO2, CH4, N2O Concentrations
- far exceed pre-industrial
values
- increased markedly since
1750
due to human activities
Relatively little variation
between last Ice Age and
the current
industrial era
IPCC Report 2007
61. Impacts are worse
Already more flood and drought prone
Larger share of the economy is in climate sensitive
sectors
Lower capacity to adapt
Lack of financial, institutional and technological
capacity
Climate change is likely to impact disproportionately
upon the poorest countries
.. and the poorest people within countries
Net economic effects expected to be negative in most
developing countries
62.
63.
64. • No evidence for plate
tectonics on Venus
– No mid-ocean rifts
– No subduction trenches
• Volcanos spread evenly
across surface instead of
at plate boundaries, as on
Earth.
• Lithosphere not broken
into plates; probably
because heat at surface
slightly softens the
lithosphere
67. • Venus has far fewer impact craters than Moon & Mercury, but more than
Earth.
– The dense atmosphere protects it from smaller impacts
• Geologic activity (volcanic resurfacing) has erased much of the evidence
• Surface age is only about a billion years.
• Rather uniform age implies that Venus was "resurfaced" by lava flows
during a recent, relatively short period
• This differs profoundly from Earth's crustal history. What is it telling us?
– Could Venus' present crust only have formed that recently?
– Could there have been a growing crust before 1 billion years ago that
"turned over" as heat built up underneath, to lead to a new era of major
lava flows?
– Why?
68. • Geomorphological evidence (*lots* of it)
– River and flood channels, alluvial fans, slumps, canyons, ...
• One more piece of evidence: shape of ocean basins
69. • Evidence of previous
era when liquid water
was plentiful
• Today: Evidence for ice
mixed with soil in top
meter of ground
70. • Mars has not had
widespread surface
water for 3 billion
years
• Greenhouse effect
probably kept
surface warmer
before that
• Somehow Mars
lost most of its
atmosphere
71. One possible scenario
• Magnetic field may have preserved early Martian
atmosphere .
• Solar wind may have stripped atmosphere after field
decreased because of interior cooling (no more molten
core)
72. Shortly after Mars formed, its surface temperature was ~ equal to its blackbody
temperature (around -55 C).
As volcanoes dumped CO2 and H2O vapor into atmosphere, greenhouse effect
increased temperature above 0 C (freezing) so liquid water could exist.
Liquid water was present, so rocks could efficiently remove CO2 from atmosphere.
Two competing effects determined amount of CO2 in atmosphere: volcanoes
adding CO2, and rocks absorbing CO2. Result: moderate level of CO2 .
Greenhouse effect could keep surface T > 0 C, as long as volcanoes kept erupting.
Eventually Mars' core cooled and solidified (Mars is small). Volcanic activity
subsided. Magnetic field went away, solar wind particles eroded atmosphere.
Once rate of eruptions tapered off, CO2 in the atmosphere started to fall.
As the atmosphere thinned out, the greenhouse effect weakened. Eventually the
average surface temperature dropped, and surface water froze.
73. Balancing act between injection and removal of
CO2 from atmosphere
Role of liquid water in sequestering CO2
Venus too hot
Mars too cold
Earth just right
What is evidence for these scenarios? How
could you test them?