ATMOS Lecture 6. Atmospheric Pressure Pressure Profiles for Idealized Atmosphere
|
|
|
- Elfreda Nelson
- 6 years ago
- Views:
Transcription
1 ATMOS 5130 Lecture 6 Atmospheric Pressure Pressure Profiles for Idealized Atmosphere
2 Goal Understand how temperature, pressure and altitude are related in the atmosphere. Recall from last lecture Hypsometric Equation Δz = R &T ( g ln p - p. Allow for calculation of pressure at any height
3 Pressure Profiles for Idealized Atmosphere Constant Density Atmosphere Unrealistic Better representation of the ocean Atmosphere had the same mass as now, but had a constant density it would be only 8.3 km deep :1 :8 ρg Hydrostatic Equation 1 (3) 8 / dp = ρg / dz p z = p 9 ρgz Pressure decreases linearly with height
4 Pressure Profiles for Idealized Atmosphere Constant Density Atmosphere p z = p 9 ρgz Pressure is decreasing with height Density is constant SO, Temperature must decease with height p = ρr & T IDEAL GAS LAW p z = ρr & T z Substitute in Hydrostatic Equation Differentiate with respect to elevation p z = ρg := :8 = = C/km
5 Constant Density Atmosphere Autoconvective Lapse Rate p z = p 9 ρgz := :8 = = C/km = Γ BCDE When: Γ > Γ BCDE Density above greater than below! Density Inversion => Creates a mirage Above a very hot road, a layer of warm air whose density is lower than air above. The denser air slows light very slightly more than the less dense layer. So, one sees sky where the road should be, we often interpret this as a reflection caused by water on the road
6 Pressure Profiles for Idealized Atmosphere Constant Density
7 Pressure Profiles for Idealized Atmosphere Isothermal Atmosphere &1 &8 = ρg Hydrostatic Equation Again substitute in the ideal gas law, Solve dp dz = ρg = pg R & T 1 g dp = p R & T dz 1 / 1 dp = g p R & T / dz 9 ln p p 9 = gz R & T p z = p 9 exp z H Where: H = R &T 9 g
8 Scale Height p z = p 9 ρgz Scale Height (H): solve for z, when p(z) = 0, H = p 9 ρg substitute the Ideal Gas Law Constant Density Atmosphere Approximate scale heights for selected Solar System bodies Venus: 15.9 km Earth: 8.3 km Mars: 11.1 km Jupiter: 27 km Saturn: 59.5 km Titan: 40 km Uranus: 27.7 km Neptune: km Pluto: ~60 km H = R &T 9 g In other words: scale height is the increase in altitude for which the atmospheric pressure decreases by a factor of e -1 or about 37% of its original value.
9 Pressure Profiles for Idealized Atmosphere Constant Lapse Rate atmosphere T = T 9 Γz Normally Γ >0, temperature decreases with altitude When Γ >0, temperature increases with altitude INVERSION
10 Pressure Profiles for Idealized Atmosphere Constant Lapse Rate atmosphere T = T 9 Γz Take the hydrostatic equation and combine with Ideal Gas Law dp dz = ρg = pg R & (T 9 Γz) 1 p dp = g R & dz T 9 Γz 1 / 1 dp = g 8 dz / 1 5 p R & 9 T 9 Γz ln p p 9 = g R & Γ ln T 9 Γz T 9 p(z) = p 9 T 9 Γz T 9 Q
11 Pressure Profiles for Idealized Atmosphere Constant Lapse Rate atmosphere T = T 9 Γz Take the hydrostatic equation and combine with Ideal Gas Law dp dz = ρg = pg R & (T 9 Γz) 1 p dp = g R & dz T 9 Γz 1 / 1 dp = g 8 dz / 1 5 p R & 9 T 9 Γz ln p p 9 = g R & Γ ln T 9 Γz T 9 T(z) p(z) = p 9 T 9 Γz T 9 Q
12 Pressure Profiles for Idealized Atmosphere Constant Lapse rate atmosphere p(z) = p 9 T(z) T 9 Q Valid for Γ < 0 Exponent of the ratio is negative, so pressure still decreases with height Q is ratio of autoconvective to actual lapse rate So, what happens if Γ = Γ auto?
13 Pressure Profiles for Idealized Atmosphere Constant Lapse rate atmosphere p(z) = p 9 T(z) T 9 Q Valid for Γ < 0 Exponent of the ratio is negative, so pressure still decreases with height Q is ratio of autoconvective to actual lapse rate So, what happens if Γ = Γ auto? p(z) = p 9 =(8) = 5 - Pressure is linear function of z
14 20 15 Temperature vs. Altitude Γ=6.5 K/km Γ=0 z [km] 10 5 Γ=Γ auto T [K] Γ = 0 ; Isothermal Γ = 6.5 K/km; Constant Lapse Rate Γ = Γ auto ; Autoconvective; Constant Density = g/r d Fig. 4.4
15 20 15 Pressure vs. Altitude Γ=0 Γ=6.5 K/km z [km] 10 5 Γ=Γ auto Isothermal p z = p 9 exp z H p [hpa] Γ = 0 ; Isothermal Γ = 6.5 K/km; Constant Lapse Rate Γ = Γ auto ; Autoconvective Constant Density Constant Lapse Rate p(z) = p 9 T(z) T 9 Q Autoconvective p z = p 9 ρgz Fig. 4.4
16 20 Density vs. Altitude 15 z [km] 10 Γ=6.5 K/km 5 Γ=0 Γ=Γ auto ρ (kg/m 3 ) Γ = 0 ; Isothermal Γ = 6.5 K/km; Constant Lapse Rate Γ = Γ auto ; Autoconvective Constant Density Fig. 4.4
17 Piecewise Linear Temperature Profile Ultimate Approximation is model based on series of stacked layers Each layer exhibits a different constant lapse rate Generally speaking, if a layer is thin enough, then all the above methods give you about the same result. p YZ- = p Y T YZ- T Y Q [
18 10 Three Layers Piecewise Linear Profiles Layers Pressure [hpa] Pressure [hpa] Temperature [! C] Temperature [! C] Fig. 4.5
Lagrangian description from the perspective of a parcel moving within the flow. Streamline Eulerian, tangent line to instantaneous velocity field.
Chapter 2 Hydrostatics 2.1 Review Eulerian description from the perspective of fixed points within a reference frame. Lagrangian description from the perspective of a parcel moving within the flow. Streamline
Asteroids, Comets and NEOs. (Answers) Solar System Impacts. Author: Sarah Roberts
Asteroids, Comets and NEOs (Answers) Author: Sarah Roberts Asteroids, Comets and NEOs - Impact craters on the Earth 1. Using the data given below for real impact craters on the Earth, investigate the effect
ATMO/OPTI 656b Spring 08. Physical Properties of the Atmosphere
Physical Properties of the Atmosphere Thin as a piece of paper The atmosphere is a very thin layer above the solid Earth and its oceans. This is true of the atmospheres of all of the terrestrial planets.
ATMO/OPTI 656b Spring 09. Physical properties of the atmosphere
The vertical structure of the atmosphere. Physical properties of the atmosphere To first order, the gas pressure at the bottom of an atmospheric column balances the downward force of gravity on the column.
Planetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 17:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
The Outer Planets (pages )
The Outer Planets (pages 720 727) Gas Giants and Pluto (page 721) Key Concept: The first four outer planets Jupiter, Saturn, Uranus, and Neptune are much larger and more massive than Earth, and they do
Planetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 11:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
The Behaviour of the Atmosphere
3 The Behaviour of the Atmosphere Learning Goals After studying this chapter, students should be able to: apply the ideal gas law and the concept of hydrostatic balance to the atmosphere (pp. 49 54); apply
ATMO551a Fall Vertical Structure of Earth s Atmosphere
Vertical Structure of Earth s Atmosphere Thin as a piece of paper The atmosphere is a very thin layer above the solid Earth and its oceans. This is true of the atmospheres of all of the terrestrial planets.
Yes, inner planets tend to be and outer planets tend to be.
1. Planet Density Make some general comments about inner and outer planets density Inner Planets Density Outer Planets Density Is there a pattern or a trend in planet density? Yes, inner planets tend to
Key Concepts Solar System, Movements, Shadows Recall that Earth is one of many planets in the solar system that orbit the Sun.
Key Concepts Solar System, Movements, Shadows 4-3.1 Recall that Earth is one of many planets in the solar system that orbit the Sun. It is essential for students to know that Earth is a planet that orbits
Astronomy 111 Practice Midterm #2
Astronomy 111 Practice Midterm #2 Prof. Douglass Fall 2018 Name: If this were a real exam, you would be reminded of the Exam rules here: You may consult only one page of formulas and constants and a calculator
Astronomy Test Review. 3 rd Grade
Astronomy Test Review 3 rd Grade Match the vocabulary word to its definition. Outer Planets The path a planet takes around the sun. Inner Planets Orbit Sun The center of our solar system. Small, rocky
References: Parcel Theory. Vertical Force Balance. ESCI Cloud Physics and Precipitation Processes Lesson 3 - Stability and Buoyancy Dr.
References: ESCI 340 - Cloud Physics and Precipitation Processes Lesson 3 - Stability and Buoyancy Dr. DeCaria Glossary of Meteorology, 2nd ed., American Meteorological Society A Short Course in Cloud
TopHat quizzes for astro How would you represent in scientific notation? A 2.7 x 10 2 B 2.7 x 10 3 C 2.7 x 10 4 D 2.
TopHat quizzes for astro 111 Lecture week 1 1. If you multiply 2 x 10 4 by itself, what do you get? A. 4 x 10 4 B. 4 x 10 8 C. 2 x 10 4 D. 4 x 10 16 2. Jupiter's maximum distance from the sun is approximately
EART164: PLANETARY ATMOSPHERES
EART16: PLANETARY ATMOSPHERES Francis Nimmo Last Week How do planets form? They accrete from the solar nebula (dust+gas) They may subsequently migrate Where do atmospheres come from? Primary, secondary,
Atmospheric Thermodynamics
Atmospheric Thermodynamics Atmospheric Composition What is the composition of the Earth s atmosphere? Gaseous Constituents of the Earth s atmosphere (dry air) Constituent Molecular Weight Fractional Concentration
39th International Physics Olympiad - Hanoi - Vietnam Theoretical Problem No. 3 / Solution. Solution
Solution. For an altitude change dz, the atmospheric pressure change is : dp = ρgdz () where g is the acceleration of gravity, considered constant, ρ is the specific mass of air, which is considered as
Ionospheres of the Terrestrial Planets
Ionospheres of the Terrestrial Planets Stan Solomon High Altitude Observatory National Center for Atmospheric Research stans@ucar.edu Heliophysics Summer School Boulder, Colorado 28 July 2009 1 Outline
Formation of Planets and Earth Structure. Big Bang Theory. What is the shape of our solar system?
Formation of Planets and Earth Structure From work of Einstein and Hubble Big Bang Theory ~14 Ga All matter in one point Exploded Expanding still Food for thought What is the shape of our solar system?
Planetary atmospheres
Planetary atmospheres Planetary Sciences Chapter 4 Daphne Stam Netherlands Organisation for Scientific Research Outline What is an atmosphere? Pressure, density, and scale heights Origin of planetary atmospheres
ASTR 380 Possibilities for Life in the Outer Solar System
ASTR 380 Possibilities for Life in the Outer Solar System Possibility of Life in the Inner Solar System The Moon, Mercury, and the Moons of Mars Deimos NO LIFE NOW or EVER This is a 98% conclusion! Phobos
p = ρrt p = ρr d = T( q v ) dp dz = ρg
Chapter 1: Properties of the Atmosphere What are the major chemical components of the atmosphere? Atmospheric Layers and their major characteristics: Troposphere, Stratosphere Mesosphere, Thermosphere
A biological tour of the Solar System
A biological tour of the Solar System The story so far...! Cosmological: age, size and composition of the Universe.! Solar System: solar energy budget, physical composition of the planets.! Earth: the
Solar System Physics I
Department of Physics and Astronomy Astronomy 1X Session 2006-07 Solar System Physics I Dr Martin Hendry 6 lectures, beginning Autumn 2006 Lectures 4-6: Key Features of the Jovian and Terrestrial Planets
4 A(n) is a small, rocky object that orbits the sun; many of these objects are located in a band between the orbits of Mars and Jupiter.
Name Vocabulary Fill in the blank with the term that best completes the sentence., 6.11B 1 is the process in which energy is released as the nuclei of small atoms combine to form a larger nucleus., 6.11B
Which of the following planets are all made up of gas? When a planets orbit around the Sun looks like an oval, it s called a(n)
When a planets orbit around the Sun looks like an oval, it s called a(n) - ellipse - circle - axis - rotation Which of the following planets are all made up of gas? - Venus, Mars, Saturn and Pluto - Jupiter,
Outline. Aim. Gas law. Pressure. Scale height Mixing Column density. Temperature Lapse rate Stability. Condensation Humidity.
Institute of Applied Physics University of Bern Outline A planetary atmosphere consists of different gases hold to the planet by gravity The laws of thermodynamics hold structure as vertical coordinate
Inner and Outer Planets
Inner and Outer Planets SPI 0607.6.2 Explain how the relative distance of objects from the earth affects how they appear. Inner Planets Terrestrial planets are those that are closest to the Sun. Terrestrial
Unit 12 Lesson 1 What Objects Are Part of the Solar System?
Unit 12 Lesson 1 What Objects Are Part of the Solar System? The Solar System Earth, other planets, and the moon are part of a solar system. A solar system is made up of a star and the planets and other
GIANT PLANETS & PLANETARY ATMOSPHERES
GIANT PLANETS & PLANETARY ATMOSPHERES Problem Set 6 due Tuesday 25 October 2018 ASTRONOMY 111 FALL 2018 1 From last lecture INTERIOR TEMPERATURE OF A ROCKY PLANET! "# 'Λ "$ =! $ "$ + -! 1 "$ 3* + $ / "$
g (z) = 1 (1 + z/a) = 1 1 ( km/10 4 km) 2
1.4.2 Gravitational Force g is the gravitational force. It always points towards the center of mass, and it is proportional to the inverse square of the distance above the center of mass: g (z) = GM (a
Edmonds Community College Astronomy 100 Winter Quarter 2007 Sample Exam # 2
Edmonds Community College Astronomy 100 Winter Quarter 2007 Sample Exam # 2 Instructor: L. M. Khandro 1. Relatively speaking, objects with high temperatures emit their peak radiation in short wavelengths
Lecture 24: Saturn. The Solar System. Saturn s Rings. First we focus on solar distance, average density, and mass: (where we have used Earth units)
Lecture 24: Saturn The Solar System First we focus on solar distance, average density, and mass: Planet Distance Density Mass Mercury 0.4 1.0 0.06 Venus 0.7 0.9 0.8 Earth 1.0 1.0 1.0 Mars 1.5 0.7 0.1 (asteroid)
EATS Notes 1. Some course material will be online at
EATS 3040-2015 Notes 1 14 Aug 2015 Some course material will be online at http://www.yorku.ca/pat/esse3040/ HH = Holton and Hakim. An Introduction to Dynamic Meteorology, 5th Edition. Most of the images
The Earth s Hydrosphere. The volatile component of rocky planets (hydrospheres and atmospheres) Earth water reservoirs Rollins (2007)
The Earth s Hydrosphere Oceans The volatile component of rocky planets (hydrospheres and atmospheres) Planets and Astrobiology (2017-2018) G. Vladilo The Earth is the only planet of the Solar System with
Hydrostatics. ENGR 5961 Fluid Mechanics I: Dr. Y.S. Muzychka
1 Hydrostatics 2 Introduction In Fluid Mechanics hydrostatics considers fluids at rest: typically fluid pressure on stationary bodies and surfaces, pressure measurements, buoyancy and flotation, and fluid
Chapter 3 Energy Balance and Temperature. Astro 9601
Chapter 3 Energy Balance and Temperature Astro 9601 1 Topics to be covered Energy Balance and Temperature (3.1) - All Conduction (3..1), Radiation (3.. and 3...1) Convection (3..3), Hydrostatic Equilibrium
7. Our Solar System. Planetary Orbits to Scale. The Eight Planetary Orbits
7. Our Solar System Terrestrial & Jovian planets Seven large satellites [moons] Chemical composition of the planets Asteroids & comets The Terrestrial & Jovian Planets Four small terrestrial planets Like
ESE / GE 148a: Introduction to Climate
ESE / GE 148a: Introduction to Climate Organizational Details - I TA: Xianglei Huang: Xianglei (Luke) is a graduate student in Planetary Science and is working with Prof. Yuk Yung
1 Thermodynamics: some Preliminaries
1 Thermodynamics: some Preliminaries Beforewebegintoconsider thetransfer ofradiation through an atmosphere, let s consider the structure of an atmosphere with a little thermodynamics. This material hopefully
Earth Science. Unit 9: Our Place in the Universe
Earth Science Unit 9: Our Place in the Universe Lesson 8: The Outer Planets Make sure to have your study guide and a pencil and be ready to go when the timer dings! *If you choose not to participate, turn
ASTRONOMY SNAP GAME. with interesting facts
ASTRONOMY SNAP GAME with interesting facts Sun Sun The Sun is the largest object in the solar system The Sun's life expectancy is approximately 5 billion more years At its core, the Sun s temperature is
Chapter 3 Energy Balance and Temperature. Topics to be covered
Chapter 3 Energy Balance and Temperature Astro 9601 1 Topics to be covered Energy Balance and Temperature (3.1) - All Conduction (3..1), Radiation (3.. and31) 3...1) Convection (3..3), Hydrostatic Equilibrium
LEARNING ABOUT THE OUTER PLANETS. NASA's Cassini spacecraft. Io Above Jupiter s Clouds on New Year's Day, Credit: NASA/JPL/University of Arizona
LEARNING ABOUT THE OUTER PLANETS Can see basic features through Earth-based telescopes. Hubble Space Telescope especially useful because of sharp imaging. Distances from Kepler s 3 rd law, diameters from
On side wall labeled A: we can express the pressure in a Taylor s series expansion: x 2. + higher order terms,
Chapter 1 Notes A Note About Coordinates We nearly always use a coordinate system in this class where the vertical, ˆk, is normal to the Earth s surface and the x-direction, î, points to the east and the
Unit 6 Lesson 4 What Are the Planets in Our Solar System? Copyright Houghton Mifflin Harcourt Publishing Company
Unit 6 Lesson 4 What Are the Planets in Our Solar System? What other objects are near Earth in this part of space? Earth and millions of other objects make up our solar system. In Our Corner of Space A
AST 105 Intro Astronomy The Solar System
NEXT: TERRESTRIAL ATMOSPHERES Mercury AST 105 Intro Astronomy The Solar System Moon Venus Mars Earth Terrestrial Atmospheres: Which planet has the most atmosphere? Is it the largest? Closest? Fastest Rotator?
Inner and Outer Planets
Inner and Outer Planets Inner Planets Terrestrial planets are those that are closest to the Sun. Terrestrial planets are made mostly of rock and have similar characteristics to Earth. There are four terrestrial
Exercise 1: Vertical structure of the lower troposphere
EARTH SCIENCES SCIENTIFIC BACKGROUND ASSESSMENT Exercise 1: Vertical structure of the lower troposphere In this exercise we will describe the vertical thermal structure of the Earth atmosphere in its lower
Thermosphere Part-3. EUV absorption Thermal Conductivity Mesopause Thermospheric Structure Temperature Structure on other planets
Thermosphere Part-3 EUV absorption Thermal Conductivity Mesopause Thermospheric Structure Temperature Structure on other planets Thermosphere Absorbs EUV Absorption: Solar Spectrum 0.2 0.6 1.0 1.4 1.8
Learning Outcomes in Focus
Contextual strand: E&S 3 Learning Outcomes in Focus Students should be able to interpret data to compare the Earth with other planets and moons in the solar system, with respect to properties including
STUDENT RESOURCE 1.1 INFORMATION SHEET. Vocabulary
Vocabulary STUDENT RESOURCE 1.1 INFORMATION SHEET asteroids thousands of rocky objects that orbit the Sun Most asteroids orbit in a belt between the orbits of Mars and Jupiter. More than 9, asteroids have
Object Type Moons Rings Planet Terrestrial none none. Max Distance from Sun. Min Distance from Sun. Avg. Distance from Sun 57,910,000 km 0.
Mercury Mercury is the closest planet to the sun. It is extremely hot on the side of the planet facing the sun and very cold on the other. There is no water on the surface. There is practically no atmosphere.
2. Which of the following planets has exactly two moons? A) Venus B) Mercury C) Uranus D) Mars E) Neptune
Summer 2015 Astronomy - Test 2 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as
Name: Date: The masses of the various objects can be determined using the balance. Measure the masses and record the numbers in Table 7.2.
Name: Date: 7 Density 7.1 Introduction In this lab we will consider how to determine the average density of irregular shapes and what that density can tell us about the internal composition and structure
KENDRIYA VIDYALAYA, GANDHIGRAM, DINDIGUL
KENDRIYA VIDYALAYA, GANDHIGRAM, DINDIGUL Class: II A & B Month: December Subject: EVS Topic: Solar system and Earth directions Solar system: The sun is the center of our solar system. It is largest body
Sample Final Questions: Solutions Math 21B, Winter y ( y 1)(1 + y)) = A y + B
Sample Final Questions: Solutions Math 2B, Winter 23. Evaluate the following integrals: tan a) y y dy; b) x dx; c) 3 x 2 + x dx. a) We use partial fractions: y y 3 = y y ) + y)) = A y + B y + C y +. Putting
ATMOS 5130 Lecture 9. Enthalpy Conservation Property The Second Law and Its Consequences Entropy
ATMOS 5130 Lecture 9 Enthalpy Conservation Property The Second Law and Its Consequences Entropy CLASS Presentation Form group of 2 students Present ~20 minute presentation (~ 10 minute each person) Focus
Unit 2 Lesson 1 What Objects Are Part of the Solar System? Copyright Houghton Mifflin Harcourt Publishing Company
Unit 2 Lesson 1 What Objects Are Part of the Solar System? Florida Benchmarks SC.5.E.5.2 Recognize the major common characteristics of all planets and compare/contrast the properties of inner and outer
Name: Date: Hour: 179 degrees celsius. 5% of Earth A 70 pound person would weigh 27 pounds on Mercury.
Planet Exploration- http://www.kidsastronomy.com/solar_.htm Mercury 1 87.9 days 58.6 days 57 million Km 465 degrees celsius Minimum -184 degrees celsius 179 degrees celsius Moons Terrestrial or Gaseous?
ENVI.2030L - The Solar System
I. Physical characteristics of the solar system NAME ENVI.2030L - The Solar System The solar system consists of the sun and 9 planets. Table 2 lists a number of the properties and characteristics of the
Hydrostatic Equation and Thermal Wind. Meteorology 411 Iowa State University Week 5 Bill Gallus
Hydrostatic Equation and Thermal Wind Meteorology 411 Iowa State University Week 5 Bill Gallus Hydrostatic Equation In the atmosphere, vertical accelerations (dw/dt) are normally fairly small, and we can
Atmosphere, Ocean and Climate Dynamics Answers to Chapter 3
Atmosphere, Ocean and Climate Dynamics Answers to Chapter 3 1. Use the hydrostatic equation to show that the mass of a vertical column of air of unit cross-section, extendin from the round to reat heiht,
Chapter 15 & 16 Science Review (PATTERNS IN THE SKY, OUR SOLAR SYSTEM)
Chapter 15 & 16 Science Review (PATTERNS IN THE SKY, OUR SOLAR SYSTEM) The Milky Way the galaxy that contains our solar system Our solar system is a speck in the Milky Way galaxy Pluto is now considered
Name: (This only happens every four years or does it?)
Name: (This only happens every four years or does it?) Calendars: Then and Now Name: 1. What is a leap year? What do you already know about leap years? 2. List at least three questions about leap years
Overview of the Solar System
The Solar System Overview of the Solar System Basics Source: Nine Planets - A Multimedia Tour of the Solar System * By Bill Arnett The solar system consists of the Sun, the nine planets, about 90 satellites
The Earth s Hydrosphere. The volatile component of rocky planets (hydrospheres and atmospheres) Earth water reservoirs Rollins (2007)
The Earth s Hydrosphere Oceans The volatile component of rocky planets (hydrospheres and atmospheres) Planets and Astrobiology (2016-2017) G. Vladilo The Earth is the only planet of the Solar System with
Mercury Named after: Mercury, the fast-footed Roman messenger of the gods. Mean Distance from the Sun: 57,909,175 km (35,983,093.1 miles) or 0.
Mercury Named after: Mercury, the fast-footed Roman messenger of the gods. Mean Distance from the Sun: 57,909,175 km (35,983,093.1 miles) or 0.387 astronomical units Diameter: 4,879.4 km (3,031.92 miles)
Radiative equilibrium Some thermodynamics review Radiative-convective equilibrium. Goal: Develop a 1D description of the [tropical] atmosphere
![Radiative equilibrium Some thermodynamics review Radiative-convective equilibrium. Goal: Develop a 1D description of the [tropical] atmosphere](/thumbs/72/66535634.jpg "Radiative equilibrium Some thermodynamics review Radiative-convective equilibrium. Goal: Develop a 1D description of the [tropical] atmosphere")
Radiative equilibrium Some thermodynamics review Radiative-convective equilibrium Goal: Develop a 1D description of the [tropical] atmosphere Vertical temperature profile Total atmospheric mass: ~5.15x10
The Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure
The Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure RECAP Definition of an atmosphere: the gas surrounding a planet/satellite/comet/ Origin of the atmosphere. Three stages: I
TEKS Cluster: Space. identify and compare the physical characteristics of the Sun, Earth, and Moon
5.8 Earth and space. The student knows that there are recognizable patterns in the natural world and among the Sun, Earth, and Moon system. 5.8(C) 5.8(D) demonstrate that Earth rotates on its axis once
Astro 101 Lecture 12 The Jovian Planets
Astro 101 Lecture 12 The Jovian Planets 2-28-2018 Jupiter, Saturn, Uranus and Neptune ASTR-101 Section 004 Bulk Properties of Terrestrial and Jovian Planets All Jovian planets have strong magnetic fields
1. The Sun is a huge ball of very hot gas in space, which radiates heat and light in one direction.
PLEASE ANSWER YOUR QUESTIONS ON THIS PROVIDED QUESTION PAPER. EACH QUESTION IS FOLLOWED BY ANSWERS MARKED A AND B, OR A, B, C AND D. ONLY ONE ANSWER IS CORRECT. CHOOSE THE MOST CORRECT ANSWER AND CIRCLE
AOS 330: Physics of the Atmosphere and Ocean I Class Notes. G.W. Petty
AOS 330: Physics of the Atmosphere and Ocean I Class Notes G.W. Petty September 4, 2001 Chapter 1 Overview of the Atmosphere 1.1 Composition of the Terrestrial Atmosphere One may group the constituents
Observational Astronomy - Lecture 6 Solar System I - The Planets
Observational Astronomy - Lecture 6 Solar System I - The Planets Craig Lage New York University - Department of Physics craig.lage@nyu.edu March 23, 2014 1 / 39 The Sun and the Earth The Sun is 23,000
5. How did Copernicus s model solve the problem of some planets moving backwards?
MODELS OF THE SOLAR SYSTEM Reading Guide: Chapter 27.2 (read text pages 691-694) 1k. Recognize the cumulative nature of scientific evidence. 1n. Know that when an observation does not agree with an accepted
Chapter 3 Fluid Statics
Chapter 3 Fluid Statics 3.1 Pressure Pressure : The ratio of normal force to area at a point. Pressure often varies from point to point. Pressure is a scalar quantity; it has magnitude only It produces
PV = n R T = N k T. Measured from Vacuum = 0 Gauge Pressure = Vacuum - Atmospheric Atmospheric = 14.7 lbs/sq in = 10 5 N/m
PV = n R T = N k T P is the Absolute pressure Measured from Vacuum = 0 Gauge Pressure = Vacuum - Atmospheric Atmospheric = 14.7 lbs/sq in = 10 5 N/m V is the volume of the system in m 3 often the system
ρ x + fv f 'w + F x ρ y fu + F y Fundamental Equation in z coordinate p = ρrt or pα = RT Du uv tanφ Dv Dt + u2 tanφ + vw a a = 1 p Dw Dt u2 + v 2
Fundamental Equation in z coordinate p = ρrt or pα = RT Du uv tanφ + uw Dt a a = 1 p ρ x + fv f 'w + F x Dv Dt + u2 tanφ + vw a a = 1 p ρ y fu + F y Dw Dt u2 + v 2 = 1 p a ρ z g + f 'u + F z Dρ Dt + ρ
5.1 Fluid momentum equation Hydrostatics Archimedes theorem The vorticity equation... 42
Chapter 5 Euler s equation Contents 5.1 Fluid momentum equation........................ 39 5. Hydrostatics................................ 40 5.3 Archimedes theorem........................... 41 5.4 The
? 1. How old is Earth and the Moon? Warm-Up 145. The Moon: Earth s Traveling Companion Name:
The Moon: Earth s Traveling Companion Warm-Up 145 What is the Moon? What is important about it? How did the Moon end up where it is? The Moon and Earth were formed at the same time. This happened about
Fluid Statics. Pressure. Pressure
Pressure Fluid Statics Variation of Pressure with Position in a Fluid Measurement of Pressure Hydrostatic Thrusts on Submerged Surfaces Plane Surfaces Curved Surfaces ddendum First and Second Moment of
Assessment Vocabulary Instructional Strategies
Inner Planets and the similarities for each of the inner planets? (Mercury, Venus, Earth, and Mars - such as Size, atmosphere, moons/rings, ) What are the unique characteristics and details of each of
Our Sun. & the Planets. Sun and Planets.notebook. October 18, Our Sun (a quick review) Hydrogen is the main fuel source
Sun and Planets.notebook October 18, 2016 Our Sun Our Sun (a quick review) Average size main sequence star Hydrogen is the main fuel source In about 5 billion years it will become a & the Planets red giant
A medium-sized star. The hottest object found in our solar system.
A medium-sized star. The hottest object found in our solar system. It gives off heat, light, and energy. It affects the seasons, climate, and weather on Earth. The second smallest planet in our solar system.
Jovian (Jupiter like) Planets
Jovian (Jupiter like) Planets Jupiter Internal structure Heat source Moons & rings Terrestrial vs. Jovian - Size & Density Density (g/cm 3 ) Density (g/cm^3) 6 5 4 3 2 1 0 Mercury Venus Earth Mars Jupiter
ASTR 200 : Lecture 6 Introduction to the Solar System Pearson Education Inc., publishing as Addison-Wesley
ASTR 200 : Lecture 6 Introduction to the Solar System 1 2004 Pearson Education Inc., publishing as Addison-Wesley Comparative Planetology Studying the similarities among and differences between the planets
What's Up In Space? In the Center. Around the Sun. Around Earth. Space Facts! Places in Space
Non-fiction: What's Up In Space? What's Up In Space? Places in Space Space is an exciting place! Our solar system is in space. It is made up of the sun and the eight planets that travel around the sun.
Atmospheric Thermodynamics
Atmospheric Thermodynamics R. Wordsworth February 12, 2015 1 Objectives Derive hydrostatic equation Derive dry and moist adiabats Understand how the theory relates to observed properties of real atmospheres
The Standard Atmosphere
The Standard Atmosphere The Standard Atmosphere Some definitions Absolute altitude Geometric altitude Geopotential altitude Some physics The hydrostatic equation Construction of the standard atmosphere
A. The moon B. The sun C. Jupiter D. Earth A. 1 B. 2 C. 3 D. 4. Sky Science Unit Review Konrad. Here is a selection of PAT style questions.
Sky Science Unit Review Konrad Here is a selection of PAT style questions. Use the following information to answer the next question 1. 2. The source of light that allows astronimors to see Jupitor through
Lecture: Wave-induced Momentum Fluxes: Radiation Stresses
Chapter 4 Lecture: Wave-induced Momentum Fluxes: Radiation Stresses Here we derive the wave-induced depth-integrated momentum fluxes, otherwise known as the radiation stress tensor S. These are the 2nd-order
Comparing the Surfaces of the Moon and Earth
Chapter 4 Stars and the Solar System Chapter Science Investigation Comparing the Surfaces of the Moon and Earth two clear plastic shoe boxes, one with lid one cup of gravel two file folder labels or masking
ASTR 1050: Survey of Astronomy Fall 2012 PRACTICE Exam #2 Instructor: Michael Brotherton Covers Solar System and Exoplanet Topics
ASTR 1050: Survey of Astronomy Fall 2012 PRACTICE Exam #2 Instructor: Michael Brotherton Covers Solar System and Exoplanet Topics Instructions This exam is closed book and closed notes, although you may
EART164: PLANETARY ATMOSPHERES
EART164: PLANETARY ATMOSPHERES Francis Nimmo Last Week Radiative Transfer Black body radiation, Planck function, Wien s law Absorption, emission, opacity, optical depth Intensity, flux Radiative diffusion,
Lecture 19. Outline. Outline For Rest of Semester. Mercury. Discuss Quiz Mercury Venus
Lecture 19 iscuss Quiz Mercury Venus Outline Outline For Rest of Semester Oct. 29 th hapter 9 (Earth) Nov 3 rd and 5 th hapter 9 and hapter 10 (Earth and Moon) Nov. 10 th and 12 th hapter 11 (Mars, Venus,
Overview of the Solar System. Solar system contents one star, several planets, lots of debris.
Overview of the Solar System Solar system contents one star, several planets, lots of debris. Most of it is the Sun! 99.8% of the mass of the Solar System resides in the Sun. A hot ball of mostly hydrogen
ATMO 551a Homework 2 Solutions Fall r planet orbit
1. Pluto s orbit is far more eccentric than those of the major planets orbits: Aphelion: 7,375,927,931 km Perihelion: 4,436,824,613 km a. Determine the solar flux (watts/m 2 ) at each of these distances.
Project 3 Convection and Atmospheric Thermodynamics
12.818 Project 3 Convection and Atmospheric Thermodynamics Lodovica Illari 1 Background The Earth is bathed in radiation from the Sun whose intensity peaks in the visible. In order to maintain energy balance