The document discusses planetary atmospheres and their evolution. It aims to understand the origin and evolution of Earth's atmosphere by studying other atmospheres in the solar system. These atmospheres can be in different evolutionary stages or on objects of different sizes and distances from the sun. The document provides overviews of the basic properties and composition of different planetary atmospheres. It discusses concepts like scale height, adiabatic lapse rate, and potential temperature which are important for understanding the structure and dynamics of atmospheres. The goal is to interpret data from spacecraft and telescopes on other atmospheres to learn about how Earth's atmosphere has changed over time.
Particle Emission from the Sun and fluid flow in a Nozzleelangovan. physics
Gemechu Chala Debela is doing his Post Graduate studies at Wollega University, Ethiopia. He published his presentation here about Particle Emission. It will be useful to the Post Graduate and research scholars.
The mass of_the_mars_sized_exoplanet_kepler_138_b_from_transit_timingSérgio Sacani
Artigo da revista Nature, descreve o trabalho de astrônomos para medir o tamanho e a massa de um exoplaneta parecido com Marte, além de caracterizar por completo o sistema planetário da estrela Kepler-138.
Particle Emission from the Sun and fluid flow in a Nozzleelangovan. physics
Gemechu Chala Debela is doing his Post Graduate studies at Wollega University, Ethiopia. He published his presentation here about Particle Emission. It will be useful to the Post Graduate and research scholars.
The mass of_the_mars_sized_exoplanet_kepler_138_b_from_transit_timingSérgio Sacani
Artigo da revista Nature, descreve o trabalho de astrônomos para medir o tamanho e a massa de um exoplaneta parecido com Marte, além de caracterizar por completo o sistema planetário da estrela Kepler-138.
Magnetic interaction of_a_super_cme_with_the_earths_magnetosphere_scenario_fo...Sérgio Sacani
Solar eruptions, known as Coronal Mass Ejections (CMEs), are
frequently observed on our Sun. Recent Kepler observations of super
ares
on G-type stars have implied that so called super-CMEs, possessing kinetic
energies 10 times of the most powerful CME event ever observed on the Sun,
could be produced with a frequency of 1 event per 800-2000 yr on solar-
like slowly rotating stars. We have performed a 3D time-dependent global
magnetohydrodynamic simulation of the magnetic interaction of such a CME
cloud with the Earth's magnetosphere. We calculated the global structure
of the perturbed magnetosphere and derive the latitude of the open-closed
magnetic eld boundary. We also estimated energy
uxes penetrating the
Earth's ionosphere and discuss the consequences of energetic particle
uxes
on biological systems on early Earth.
3d modeling of_gj1214b_atmosphere_formation_of_inhomogeneous_high_cloouds_and...Sérgio Sacani
Uma equipe de cientistas da Universidade de Washington e da Universidade de Toronto foram os primeiros a simular nuvens exóticas em 3D na atmosfera de um exoplaneta.
O objeto em questão, é o GJ 1214b, um exoplaneta chamado de mini-Netuno que foi descoberto, seis anos atrás pelos astrônomos no Harvard-Smithsonian Center for Astrophysics.
Também conhecido como Gliese 1214b, esse mundo tem cerca de 2.7 vezes o diâmetro da Terra e uma massa quase 7 vezes maior que a massa do nosso planeta. Ele está localizado a cerca de 52 anos-luz de distância na constelação de Ophiuchus.
O planeta orbita a estrela anã vermelha, GJ 1214, a cada 38 horas, a uma distância de 1.3 milhões de milhas.
De acordo com estudos prévios, o planeta tem uma atmosfera rica em água ou hidrogênio com extensas nuvens.
“Deve existir altas nuvens ou uma névoa orgânica na atmosfera – como nós observamos em Titã. Sua temperatura atmosférica excede o ponto de fusão da água”, disse o Dr. Benjamin Charnay, um dos membros da equipe da Universidade de Washington.
Magnetic interaction of_a_super_cme_with_the_earths_magnetosphere_scenario_fo...Sérgio Sacani
Solar eruptions, known as Coronal Mass Ejections (CMEs), are
frequently observed on our Sun. Recent Kepler observations of super
ares
on G-type stars have implied that so called super-CMEs, possessing kinetic
energies 10 times of the most powerful CME event ever observed on the Sun,
could be produced with a frequency of 1 event per 800-2000 yr on solar-
like slowly rotating stars. We have performed a 3D time-dependent global
magnetohydrodynamic simulation of the magnetic interaction of such a CME
cloud with the Earth's magnetosphere. We calculated the global structure
of the perturbed magnetosphere and derive the latitude of the open-closed
magnetic eld boundary. We also estimated energy
uxes penetrating the
Earth's ionosphere and discuss the consequences of energetic particle
uxes
on biological systems on early Earth.
3d modeling of_gj1214b_atmosphere_formation_of_inhomogeneous_high_cloouds_and...Sérgio Sacani
Uma equipe de cientistas da Universidade de Washington e da Universidade de Toronto foram os primeiros a simular nuvens exóticas em 3D na atmosfera de um exoplaneta.
O objeto em questão, é o GJ 1214b, um exoplaneta chamado de mini-Netuno que foi descoberto, seis anos atrás pelos astrônomos no Harvard-Smithsonian Center for Astrophysics.
Também conhecido como Gliese 1214b, esse mundo tem cerca de 2.7 vezes o diâmetro da Terra e uma massa quase 7 vezes maior que a massa do nosso planeta. Ele está localizado a cerca de 52 anos-luz de distância na constelação de Ophiuchus.
O planeta orbita a estrela anã vermelha, GJ 1214, a cada 38 horas, a uma distância de 1.3 milhões de milhas.
De acordo com estudos prévios, o planeta tem uma atmosfera rica em água ou hidrogênio com extensas nuvens.
“Deve existir altas nuvens ou uma névoa orgânica na atmosfera – como nós observamos em Titã. Sua temperatura atmosférica excede o ponto de fusão da água”, disse o Dr. Benjamin Charnay, um dos membros da equipe da Universidade de Washington.
Materials Required· Computer and internet access· Textbook· AbramMartino96
Materials Required
· Computer and internet access
· Textbook
· Scientific calculator
· Spreadsheet software like Excel
· Digital camera
· Printer or drawing software
· Save this worksheet and use it as your report template
Time Required: Between 3-3.5 hours, note that depending if you use Excel (or similar), your time will be shortened.
Introduction
Figure 1: JP Stellar Revolution
The life cycle of the stars is one of the most fascinating studies of astronomy.Stars are the building blocks of galaxies and by looking at their age, composition and distribution we can learn a great deal about the dynamics and evolution of that galaxy. Stars manufacture the heavier elements including carbon, nitrogen and oxygen which in turn will determine the characteristics of the planetary systems that form around them. It is the mass of the star which will determine its life cycle and this all depends on the amount of matter that is available in its nebula. Each star will begin with a limited amount of hydrogen in their cores. This lifespan is proportional to (f M) / (L), where f is the fraction of the total mass of the star, M, available for nuclear burning in the core and L is the average luminosity of the star during its main sequence lifetime. The larger the mass, the shorter the lifespan ending in a beautiful supernova, the smaller the mass, the longer the lifespan ending as a quiet brown dwarf (Fig. 1).
Main Sequence Stars
Figure 2: https://imagine.gsfc.nasa.gov/
For this lab we will focus on stars similar to our own Sun (up to 1.4MassSun ), main sequence stars. A star that is similar in size to our Sun will take approximately 50 million years to mature from the beginning of their collapse to becoming an “adult” star. Our Sun, after reaching this mature phase, will stay on the main sequence of the HR-diagram for approximately 10 billion years (Fig. 2). Stars like our Sun are fueled by the nuclear fusion of hydrogen forming into helium at their cores. It is this outflow of energy that provides the outward pressure necessary to keep the star from collapsing under its own weight. And in turn, this energy determines the luminosity of the stars.
Death of Our Sun
Figure 3. NGC 6543
When a low mass star like our Sun has exhausted its supply of hydrogen in its core, then there will no longer be a source of heat to support the core against the pull of gravity. Hydrogen will continue to burn in a shell around the core and the star will evolve into the phase of a red giant, growing in diameter. The core of the star will collapse under the pull of gravity until it reaches a high enough density, and it will begin to burn helium and make carbon. This phase will last about 100 million years eventually exhausting the helium and then becoming a red supergiant, growing more in diameter. This is a more brief phase and last only a few tens of thousands of years and the star loses mass by expelling a strong wind. The star eventually loses the mass in its envelope, leav ...
Materials Required· Computer and internet access· Textbook· AbramMartino96
Materials Required
· Computer and internet access
· Textbook
· Scientific calculator
· Spreadsheet software like Excel
· Digital camera
· Printer or drawing software
· Save this worksheet and use it as your report template
Time Required: Between 3-3.5 hours, note that depending if you use Excel (or similar), your time will be shortened.
Introduction
Figure 1: JP Stellar Revolution
The life cycle of the stars is one of the most fascinating studies of astronomy.Stars are the building blocks of galaxies and by looking at their age, composition and distribution we can learn a great deal about the dynamics and evolution of that galaxy. Stars manufacture the heavier elements including carbon, nitrogen and oxygen which in turn will determine the characteristics of the planetary systems that form around them. It is the mass of the star which will determine its life cycle and this all depends on the amount of matter that is available in its nebula. Each star will begin with a limited amount of hydrogen in their cores. This lifespan is proportional to (f M) / (L), where f is the fraction of the total mass of the star, M, available for nuclear burning in the core and L is the average luminosity of the star during its main sequence lifetime. The larger the mass, the shorter the lifespan ending in a beautiful supernova, the smaller the mass, the longer the lifespan ending as a quiet brown dwarf (Fig. 1).
Main Sequence Stars
Figure 2: https://imagine.gsfc.nasa.gov/
For this lab we will focus on stars similar to our own Sun (up to 1.4MassSun ), main sequence stars. A star that is similar in size to our Sun will take approximately 50 million years to mature from the beginning of their collapse to becoming an “adult” star. Our Sun, after reaching this mature phase, will stay on the main sequence of the HR-diagram for approximately 10 billion years (Fig. 2). Stars like our Sun are fueled by the nuclear fusion of hydrogen forming into helium at their cores. It is this outflow of energy that provides the outward pressure necessary to keep the star from collapsing under its own weight. And in turn, this energy determines the luminosity of the stars.
Death of Our Sun
Figure 3. NGC 6543
When a low mass star like our Sun has exhausted its supply of hydrogen in its core, then there will no longer be a source of heat to support the core against the pull of gravity. Hydrogen will continue to burn in a shell around the core and the star will evolve into the phase of a red giant, growing in diameter. The core of the star will collapse under the pull of gravity until it reaches a high enough density, and it will begin to burn helium and make carbon. This phase will last about 100 million years eventually exhausting the helium and then becoming a red supergiant, growing more in diameter. This is a more brief phase and last only a few tens of thousands of years and the star loses mass by expelling a strong wind. The star eventually loses the mass in its envelope, leav ...
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Aerodynamics Part I of 3 describes aerodynamics of wings and bodies in subsonic flight.
For comments please contact me at solo.hermelin@gmail.com.
For more presentations on different subjects visit my website at http://www.solohermelin.com.
Fighter Aircraft Performance, Part I of two, describes the parameters that affect aircraft performance.
For comments please contact me at solo.hermelin@gmail.com.
For more presentations on different subjects visit my website at http://www.solohermelin.com.
Magma oceans and enhanced volcanism on TRAPPIST-1 planets due to induction he...Sérgio Sacani
Low-mass M stars are plentiful in the Universe and often host small, rocky planets detectable with current instrumentation.
These stars host magnetic fields, some of which have been observed to exceed a few hundred gauss. Recently, seven small
planets have been discovered orbiting the ultra-cool M dwarf TRAPPIST-1, which has an observed magnetic field of 600 G. We
suggest electromagnetic induction heating as an energy source inside these planets. If the stellar rotation and magnetic dipole
axes are inclined with respect to each other, induction heating can melt the upper mantle and enormously increase volcanic
activity, sometimes producing a magma ocean below the planetary surface. We show that induction heating leads the four
innermost TRAPPIST-1 planets, one of which is in the habitable zone, either to evolve towards a molten mantle planet, or to
experience increased outgassing and volcanic activity, while the three outermost planets remain mostly unaffected.
Hollow earth, contrails & global warming calculations lectureMarcus 2012
http://marcusvannini2012.blogspot.com/
http://www.marcusmoon2022.org/designcontest.htm
Shoot for the moon and if you miss you'll land among the stars...
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.
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.
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.
Encryption in Microsoft 365 - ExpertsLive Netherlands 2024Albert Hoitingh
In this session I delve into the encryption technology used in Microsoft 365 and Microsoft Purview. Including the concepts of Customer Key and Double Key Encryption.
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:
Smart TV Buyer Insights Survey 2024 by 91mobiles.pdf91mobiles
91mobiles recently conducted a Smart TV Buyer Insights Survey in which we asked over 3,000 respondents about the TV they own, aspects they look at on a new TV, and their TV buying preferences.
UiPath Test Automation using UiPath Test Suite series, part 3DianaGray10
Welcome to UiPath Test Automation using UiPath Test Suite series part 3. In this session, we will cover desktop automation along with UI automation.
Topics covered:
UI automation Introduction,
UI automation Sample
Desktop automation flow
Pradeep Chinnala, Senior Consultant Automation Developer @WonderBotz and UiPath MVP
Deepak Rai, Automation Practice Lead, Boundaryless Group and UiPath MVP
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
Welocme to ViralQR, your best QR code generator.ViralQR
Welcome to ViralQR, your best QR code generator available on the market!
At ViralQR, we design static and dynamic QR codes. Our mission is to make business operations easier and customer engagement more powerful through the use of QR technology. Be it a small-scale business or a huge enterprise, our easy-to-use platform provides multiple choices that can be tailored according to your company's branding and marketing strategies.
Our Vision
We are here to make the process of creating QR codes easy and smooth, thus enhancing customer interaction and making business more fluid. We very strongly believe in the ability of QR codes to change the world for businesses in their interaction with customers and are set on making that technology accessible and usable far and wide.
Our Achievements
Ever since its inception, we have successfully served many clients by offering QR codes in their marketing, service delivery, and collection of feedback across various industries. Our platform has been recognized for its ease of use and amazing features, which helped a business to make QR codes.
Our Services
At ViralQR, here is a comprehensive suite of services that caters to your very needs:
Static QR Codes: Create free static QR codes. These QR codes are able to store significant information such as URLs, vCards, plain text, emails and SMS, Wi-Fi credentials, and Bitcoin addresses.
Dynamic QR codes: These also have all the advanced features but are subscription-based. They can directly link to PDF files, images, micro-landing pages, social accounts, review forms, business pages, and applications. In addition, they can be branded with CTAs, frames, patterns, colors, and logos to enhance your branding.
Pricing and Packages
Additionally, there is a 14-day free offer to ViralQR, which is an exceptional opportunity for new users to take a feel of this platform. One can easily subscribe from there and experience the full dynamic of using QR codes. The subscription plans are not only meant for business; they are priced very flexibly so that literally every business could afford to benefit from our service.
Why choose us?
ViralQR will provide services for marketing, advertising, catering, retail, and the like. The QR codes can be posted on fliers, packaging, merchandise, and banners, as well as to substitute for cash and cards in a restaurant or coffee shop. With QR codes integrated into your business, improve customer engagement and streamline operations.
Comprehensive Analytics
Subscribers of ViralQR receive detailed analytics and tracking tools in light of having a view of the core values of QR code performance. Our analytics dashboard shows aggregate views and unique views, as well as detailed information about each impression, including time, device, browser, and estimated location by city and country.
So, thank you for choosing ViralQR; we have an offer of nothing but the best in terms of QR code services to meet business diversity!
Builder.ai Founder Sachin Dev Duggal's Strategic Approach to Create an Innova...Ramesh Iyer
In today's fast-changing business world, Companies that adapt and embrace new ideas often need help to keep up with the competition. However, fostering a culture of innovation takes much work. It takes vision, leadership and willingness to take risks in the right proportion. Sachin Dev Duggal, co-founder of Builder.ai, has perfected the art of this balance, creating a company culture where creativity and growth are nurtured at each stage.
Accelerate your Kubernetes clusters with Varnish CachingThijs Feryn
A presentation about the usage and availability of Varnish on Kubernetes. This talk explores the capabilities of Varnish caching and shows how to use the Varnish Helm chart to deploy it to Kubernetes.
This presentation was delivered at K8SUG Singapore. See https://feryn.eu/presentations/accelerate-your-kubernetes-clusters-with-varnish-caching-k8sug-singapore-28-2024 for more details.
2. A principal reason for studying planetary atmospheres is
to try to understand the origin and evolution of the
earth’s atmosphere. Of course, in trying to understand
the workings of our solar system or even the evolution
of the earth as a body, the earth’s atmosphere is
essentially irrelevant since its mass is negligible. For
that matter, the mass of the earth is only a small
fraction of the mass of the sun. So we are considering
a thin skin of gravitationally bound gas attached to a
speck of matter in a dynamic and, in the
past, violent, system. Therefore, it is a formidable
problem.
However, it is in that thin skin of gas and on that speck
of matter that we live, and therefore, it is interesting to
us.
3. It is also clear now that the earth’s gaseous envelope is
changing and has changed. In fact it is abundantly
clear that the present atmosphere barely resembles the
original residual gas left when the earth formed.
Because of this it is also important to study the other
atmospheres in the solar system, since they are either
different end states or in different stages of atmospheric
evolution. They may all have had roughly similar
materials as sources, but either these atmospheres are
on objects of a very different size or at a very different
distance from the sun. Since, we can not carry out
many experiments to see how the earth’s atmosphere is
evolving, Interpreting the data on other
atmospheres, given to us by Spacecraft and telescope
data, is crucial and is one goal of this theme.
4. Basic Properties of Atmospheres
Composition
Size
Equilibrium T
Scale Height
Adiabatic Lapse Role
Mixing in Troposphere
Radiation Absorption
Absorption Cross Section
Heating by Absorption
Chapman Layer
Ozone Production:
Stratosphere
Thermospheric Structure
Ionospheres
Green House Effect
Atmospheric Evolution
Water:
Venus, Earth, Mars
Loss by Escape
Isotope Ratios
CO2 cycle:
Earth, Venus, Mars
Atmospheric Circulation
Coriolis Effect
Local Circulation
Boundary Layer
Global Circulation
Zonal Belts
Cloud Formation
Topical Problems in Planetary
Atmospheres
Overview of Solar System
6. Type Name Mass Escape p T*
(eV/u) (bar) (K)
Collisionless Mercury 0.053 0.093
Moon 0.012 0.029
Other moons
T*: for Jovian they are Teq ; for the terrestrial
they are mean surface temperatures; for icy
satellites they are the subsolar T
1eV = 1.16x104 K
1 bar = 105 Pa = 105 N/m2.
7. Molecular
Sun
H (H2) 0.86
He 0.14
O 0.0014
C 0.0008
Ne 0.0002
N 0.0004
Jupiter Saturn Uranus Neptune
H2 0.898 0.963 0.825 0.80
He 0.102 0.0325 0.152 0.19
CH4 0.003 0.0045 0.023 0.015
NH3 0.0026 0.0001 <10-7 <6x10-7
9. Pressure is the weight of a column of gas: force
per unit area
p = mg N (column density: N)
Thickness if frozen: Hs
p(bar) Hs(m) Ma/Mp
(10-5)
Mars 0.008 2 0.049
Earth 1 10 0.087
Titan 1.5 100 6.8
Venus 90 1000 9.7
How big might Mars atmosphere have been (in bars) based
on its size? How big might the earth’s have been?
10. p, T, n (density) Equation of State
Conservation of Species
Continuity Equation: Diffusion and Flow
Sources / Sinks: Volcanoes
Escape (top)
Condensation/ Reaction (surface)
Chemical Rate Equations
Conservation of Energy
Heat Equation: Conduction, Convection, Radiation
Sources: Sun and Internal
Sinks: Radiation to Space, Cooling to Surface
Radiation transport
Conservation of Momentum
Pressure Balance
Flow
Rotating: Coriolis
Atomic and Molecular Physics
Solar Radiation: Absorption and Emission
Heating; Cooling; Chemistry
Solar Wind: Aurora
11. Equilibrium Temperature
Heat In = Heat Out
or
Source (Sun) = Sink (IR Radiation to Space)
Planetary body with radius a it absorbs energy over
an area pa2
Cooling: IR radiation out
If the planetary body is rapidly rotating or has
winds
rapidly transporting energy, it radiates energy
from all of its area 4pa2
12. Fraction of radiation absorbed in atmosphere vs. wavelength
Principal absorbing species indicated
13. Source=Absorb
Area heat flux amount absorbed
pa2 x [F / Rsp
2] x [1-A]
A = Bond Albedo: total amount reflected
(Complicated)
Solar Flux 1AU: F =1370W/m2
Rsp= distance from sun to planet in AU
Loss=Emitted (ideal radiator)
Area radiated flux
4pa2 x T4
= Stefan-Boltzman Constant= 5.67x10-8 J/(m2 K4 s)
Fig. Radiation/ Albedo
14. Bond Albedo, A, is
fraction of sunlight
reflected to space:
Surface, clouds, sc
attered
15. Set Equal
Heat In = Heat Out
Te = [ (F / Rsp
2) (1-A) / 4 ]1/4
Rsp A Te Ts
Mercury 0.39 0.11 435 440
Venus 0.72 0.77 227 750
Earth 1 0.3 256 280
Mars 1.52 0.15 216 240
Jupiter 5.2 0.58 98 134*
If the radiation was slow but evaporation was fast,
like in a comet, describe the loss term that would the
IR loss.
Fig. Sub T
17. Pressure vs. Altitude
Hydrostatic Law
Force Up = Force Down
p- A=area
---------------------------------------------
Draw forces Δz
---------------------------------------------
p+ mg = (ρ A Δz) g
Result:
Net Force= 0 = - (Δp A) - (ρ A Δz) g
where p = p-- - p+
18. dp/dz = - g
Now Use Ideal Gas Law
p = nkT (k=1.38 x 10-23 J/K) =kT/m
or
p = (R/Mr)T [Gas constant: R=Nak =8.3143 J/(K mole)
with Mr the mass in grams of a mole]
substitute for
dp/dz = - p(mg/kT)= -p/H
H is an effect height=
Gravitational Force/ Thermal Energy
Same result for a ballistic atmosphere
19. Pressure vs. Altitude
p = po exp( - ∫ dz / H)
(assuming T constant)
p = po exp( - z / H)
or
Density vs. Altitude
= 0 exp( - z / H)
Scale Height: H
H = kT/mg (or H = RT / Mr g)
Mr g(m/s2) Ts(K) H(km)
Venus CO2 44 8.88 750 16
Earth N2 ,O2 29 9.81 288 8.4
Mars CO2 44 3.73 240 12
Titan N2 , CH4 28 1.36 95 20
Jupiter H2 2 26.2 128 20
Note: did not use Te , used Ts for V,E,M
20. Pressure: p
p = weight of a column of gas (force per unit area)
1bar = 106 dyne/cm2=105 Pascal=0.987atmospheres
Pascal=N/m2 ; Torr=atmosphere/760= 1.33mbars
Venus 90 bars
Titan 1.5 bars
Earth 1 bar
Mars 0.008 bar
Column Density: N
p = m g N
Surface of earth: N 2.5 x 1025 molecules/cm2.
What would N be at the surface of Venus?
If the atmosphere froze (like on Triton),
how deep would it be?
n(solid N2) 2.5 x 1022 /cm3
N/n = 10m
21. PARTIAL PRESSURES
Lower Atmosphere
Mixing dominates: use m or Mr
Upper atmosphere
Diffusive separation
Partial Pressure (const T)
p = pi(z) = poi exp[ - z/Hi ]
Hi = kT/ mig
Fig. Density vs. z
25. Convection Dominates Adiabatic Lapse Rate
In the troposphere
Radiation Dominates Greenhouse Effect
In the troposphere and stratosphere
Conduction Dominates Thermal Conductivity
In the thermosphere
Fig. T vs. z
27. Imagine gas moving up or down adiabatically: no
heat in or out of the volume
Energy = Internal energy + Work
dq = cvdT + p dV
(energy per mass of a volume of gas V = 1 / )
Adiabatic = no heat in or out: dq = 0
cv dT = - p dV
Ideal gas law [p = nkT = (R/Mr)T ]
pV = (R/Mr)T
28. Differentiate
p dV + dp V = (R/Mr) dT
or
cv dT = - (R/Mr) dT + V dp
(cv +R/Mr) dT = dp /
cp (dT/dz) = (dp/dz) /
Apply Hydrostatic Law
(dp/dz) = - g
29. (dT/dz) = -g / cp = - d
Heating at surface + Slow vertical motion.
T= [Ts - d z]
T falls off linearly with altitude
cp (erg/gm/K) d (deg/km)
Venus 8.3 x 106 11
Earth 1.0 x 107 10
Mars 8.3 x 106 4.5
Jupiter 1.3 x 108 20
30. cp = Cp / m = cv + (R/Mr)
= Cv + k
m
CvT = heat energy of a molecule
Atom = Cv = (3/2)k ; kinetic energy only
3-degrees of freedom each with k/2
N2: One would think that there are
6-degrees of freedom: 3 + 3
or 3 (CM) + 2 (ROT) + 1 (VIB)
Cv = 3k
31. But potential energy of internal vibrations
needed.
Cv 3.5 k = 4.8 x 10-16 ergs/K
1 mass unit = 1.66x 10-24 gm
cv 1.0 x 107 (ergs/gm/K)
fortuitous as Cp 3.5
Define = Cp/Cv
Using the above - 1 = k/Cv
or ( - 1) / = k/ Cp = k/(mcp)
32. Now have p(z) with T dependence.
Use (dT/dz) = -g / cp and dp/dz = - ρ g and p = nkT
dp/p = - mgdz/kT = [m cp/k] dT/T = x dT/T
x = /(-1)
=cp/cv
1/x = ~0.2 for N2 ; ~0.17 for CO2 ; ~0 for large molecule
(~5/3, 7/3, 4/3 for mono, dia and ployatomic gases)
Solve and rearrange
(p/po) = (T/To)x
using T= [Ts - d z]
p(z) = po[1 - z/(xH)]x --> po exp(-z/H) for x small
33. = T (po/p)1/x
Adiabatic Entropy = Constant
Gas can move freely along constant lines
Using dq = T dS where S is entropy
Can show S = cp ln + const
34. Things you should know
Te and how is it obtained
The average albedo
The hydrostatic law for an atmosphere
The atmospheric scale height
The adiabatic lapse rate
Potential Temperature