Newton s Laws of Motion and Gravity ASTR 2110 Sarazin. Space Shuttle
|
|
- Lindsay Norman
- 6 years ago
- Views:
Transcription
1 Newton s Laws of Motion and Gravity ASTR 2110 Sarazin Space Shuttle
2 Discussion Session This Week Friday, September 8, 3-4 pm Shorter Discussion Session (end 3:40), followed by: Intro to Astronomy Department for Potential Astronomy or Astronomy-Physics Majors (if not interested in majors, no need to stay)
3 Welcome Party Friday, September 8, 4:30-6 pm Food and drinks. Meet the Astronomy Department and NRAO McCormick Observatory Will walk interested students over to Department after Discussion Session. Walk or rides provided up O Hill
4 Isaac Newton ( )
5 Newton s 1 st Law F = 0 v = constant a = 0 Unless subject to a force, an object will continue to move at a constant velocity Objects at rest stay at rest Objects in motion maintain same speed and direction
6 F = 0 a = 0 F a? Newton s 2 nd Law F = ma = m d v dt = d dt p m mass (total amount of matter in object) p m v momentum a = F m equation of motion
7 Newton s 3 rd Law Is physics just too tough? N atoms ~ N forces = N atoms (N atoms 1)/2 ~ 10 48!! F = F F12 F 21 Every force produces an equal and opposite force
8 Momentum: d p i dt p tot = = j Conservation Laws Closed system F ij i p i d p tot = F ij = 1 " dt i, j 2 % $ F ij + F ji ' = 1 # i, j j,i & 2 i, j p tot = constant, momentum is conserved ( F ij + F ) ji = 0
9 Center of Mass p tot = v CM r CM i i i m i vi m i vi m i ri = constant i m i = constant m i moves at constant velocity i
10 Conservation Laws Energy: Object of mass m moving in a force field m d v dt = F Now, do dot product with v mv d v dt = v F = F d r dt v d v dt = 1 d v 2 = 1 2 dt 2 2 v d v dt 1 2 m d v2 = F d r Now, integrate both sides dt dt 1 2 mv2 = F d r + constant dt
11 Conservation Laws Energy: 1 2 mv2 = Define: F d r + constant KE 1 2 mv2 kinetic energy PE F d r potential energy E = KE + PE = constant Total energy is conserved
12 Conservation Laws Angular Momentum: L r p angular momentum Assume: F ij r ij Central force F 12 r 12 F21 d L tot dt = i d dt ( r i p ) i
13 Conservation Laws Angular Momentum: r 12 d L tot dt = = = i i i, j d dt ( r i p ) i v i m i vi + r i F i ( ) r i F i, j F 12 F21 = 1 2 i, j r i F i, j + r j F j,i ( )
14 Conservation Laws Angular Momentum: r 12 d L tot dt = 1 2 i, j r i F i, j + r j F j,i ( ) F 12 F21 but F j,i = F i, j d L tot = 1 ( r i r ) j F i, j = 1 dt 2 i, j 2 F ij r ij Central force i, j r ij F i, j d L tot dt = 0, L tot = constant
15 Conservation Laws Something for nothing? Conservation Laws Momentum Energy Angular Momentum çè Symmetries of nature çè All places are the same Space is homogeneous çè All times are the same çè All directions are the same Space is isotropic
16 Turning now to gravity
17 No force move in straight line Planet orbits curved (ellipses) must be a force acting Prob. 2.1 in homework a cent = v2 r Force due to Sun What is force? Planetary Motions êr Force toward Sun Sun force planet
18 Lunar Motion Moon s orbit curved must be a force Force due to Earth: What is force?
19 Lunar Motion Moon force force
20 Gravity Gravity is force in motion of Moon Gravity is force in planetary motion
21 Galileo and Gravity Galileo also studied gravity on Earth Pre-Galileo: Heavy objects fall faster Objects fall at a constant speed Galileo: Objects fall at a constant acceleration All objects fall with the same acceleration (no air friction)
22 Properties of Gravity Newton s 2 nd Law: a = F/m = g = constant Can only be true for everything if F m Force on object proportional to its mass Newton s 3 rd Law: F 21 m 2 force on 2 due to 1 F 12 = - F 21 F 12 m 2 force on 1 due to 2 m 1 m F F Force due to object proportional to its mass
23 Properties of Gravity Force is proportional both to mass of source and mass of object being affected F 12 m 1 F 12 m 2 F 12 m 1 x m 2
24 Properties of Gravity Compare acceleration of Moon, apple Acceleration of Moon much smaller. Distance to Moon much greater. Assume F = m 1 m 2 f(d) decreasing function of distance d
25 Properties of Gravity Assume F = m 1 m 2 f(d) decreasing func. d Moon = 3.84 x 10 5 km, d Earth = 6378 km v Moon = 2πd Moon /P Moon, P moon =27.3 d a Moon = v Moon2 /d Moon =0.272 cm/s 2 a Earth = g = 981 cm/s 2 = 3600 a Moon =60 2 a Moon d Moon = 60 d Earth F α d -2
26 Newton s Law of Gravity F 12 = - G m 1 m 2 / d 2 d d = distance m 1 m F F G = constant of nature = 6.67 x 10-8 cm 3 / gm / s 2 = 6.67 x m 2 / kg / s 2
27 Newton s Law of Gravity F 12 = G m 1m 2 r 12 2 PE = G m 1m 2 r 12 ê r d m 1 m F F m 1 a1 = G m 1 m 2 r 12 2 ê r
28 Newton s Law of Gravity m 1 a1 = G m 1 m 2 r 12 2 ê r d m 1 m F F Inertia Three Roles for Mass ma Gravity Source m 2 active Gravity Effect m 1 passive Why mass? Inertia and passive gravity terms cancel why?
29 Spherical Object F = G M(r)m r 2 ê r M(r) mass interior to r r m
30 One Body Solvable N-Body (N 3) Two Body N-Body Problem Fixed mass Generally, no analytic solution. Solve numerically on a computer Six Equations, but total momentum conserved è Only 3 independent equations, same as 1-body 2-Body Problem = 1-Body Problem in CM frame, solvable. m
31 2-Body Problem v r v 1 r 1 m 1 CM r 2 m 2 v 2 = r μ r = r 2 r 1 r 1 = v = v 2 v 1 v 1 = m 2 m 1 + m 2 r r 2 = m 2 m 1 + m 2 v v 2 = m 1 m 1 + m 2 r m 1 m 1 + m 2 v µ m 1m 2 m 1 + m 2 "reduced mass"
32 2-Body Problem v r v 1 r 1 m 1 CM r 2 m 2 v 2 = r μ KE = 1 2 µv2 PE = G m 1 m 2 r E = KE + PE = constant L = µ r v = constant
33 Newton Derived Kepler s Law Derived, generalized, corrected Kepler s laws Treat Solar System as a series of 2-body problems (Sun and each planet), since most of gravity is from the Sun
34 Kepler s 2 nd Law Equal areas in equal times d A = 1 2 r perpendicular component of d s = 1 2 r d s = 1 2 r v dt r d A = 1 2m = 1 2m da dt = constant [ r (mv) ]dt = 1 2m L dt = constant dt r p ( )dt True for any central force (not just gravity) ds = v dt
35 Kepler s 3 nd Law P 2 α a 3 Do for a circular orbit m a = F (1-body) µ a = F (2-body) m 1 m 2 m 1 + m 2 " $ # v2 r v 2 = G(m 1 + m 2 ) r v = 2πr P P 2 =! # " % ' e r = G m 1m 2 & r 2 2πr P 4π 2 a 3 G(m 1 + m 2 ) $ & % 2 Not quite Kepler, depends on mass! er v = G(m 1 + m 2 ) r = v 2 4π 2 r 2 = G(m 1 + m 2 ) P 2 r
36 Kepler s 1 st Law Orbits ellipses, Sun at focus Use conservation of L and E L planar orbit, L ( ) r = L2 G m 1 m 2 µ 1+ ecosθ e = 1+ 2EL 2 G 2 m 1 2 m 22 µ 1 cosθ +1 e <1 1+ ecosθ > 0 r remains finite (bound) e 1 1+ ecosθ 0 r (unbound) e <1 E < 0 Conic section
37 Kepler s 1 st Law Energy Eccentricity Shape Bound? E < 0 e < 1 Ellipse (circle) Bound (can t get apart) E = 0 e = 1 Parabola Just unbound E > 0 e > 1 Hyperbola Unbound Why does energy determine orbit? Conserved Unbound è r è PE è 0 E = KE = ½ m v 2 0
38 ( r = L2 G m 1 m 2 µ ) 1+ ecosθ r = ( ) a 1 e2 1+ ecosθ Kepler s 1 st Law Compare to previous equation for ellipse Only for ellipse E = 1 2 G m 1 m 2 a = constant (bound orbit) PE = G m 1 m 2 r Odd: E = 1 2 PE??
39 Consider A Virial Theorem No static gravitational equilibrium since force always attractive KE > 0 da dt = i m i v i r i (Why? Trust me.) i m ia i r ( i + m ivi v i ) " = m iv 2 i + F i r % $ ' # & i = 2KE + F i r i
40 Virial Theorm Now, consider average of da/dt over a long time da dt = A(t) t So either A(t) A(0) t da dt da dt t + A(0) as t mean value thm of calculus 0 or A(t) A v i r i so either v or r not bound! So, da dt 0 over a long time
41 Virial Theorm da dt 2 KE = = 2 KE + = + = i i, j pairs F i r i i F i r i G m i m j ri r j r i r 3 j ( ) G m i m j ri r j r i r 3 j ( ) 0 over a long time r i Do by pairs i,j r i + G m m j i r j r i r j r 3 i ( ) r j
42 Virial Theorm 2 KE = pairs G m i m j r i r 3 j " #( r i r j ) r i r i r j ( ) r j $ % = G m i m j r i r ( r 3 i r ) 2 j = pairs j pairs G m i m j r i r j 2 KE = PE KE = 1 2 PE E = KE + PE = constant E = E E = 1 2 PE = KE
43 Electromagnetism and Light ASTR 2110 Sarazin Laser Guide Star at Telescope
44 Four Forces in Nature Strong (Nuclear) Force: ~10 1 Electromagnetic Force: ~10-2 α = e 2 /ħc 1/137 Weak (Nuclear) Force: ~10-18 Gravity: ~10-40 But gravity applies to everything, always attractive
45 Electromagnetic Forces E electric field B magnetic field # F = q E v B & % + ( $ c ' q charge F 12 = q q 1 2 ê r 2 r Coulomb s Law
46 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field Coulomb s Law or Gauss s Law
47 Static Electricity
48 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field charges E
49 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field No magnetic charges (magnetic monopoles) charges E no magnetic charges B
50 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field No magnetic charges (magnetic monopoles) Moving charges (currents) make magnetic fields Ampere s Law
51 Electromagnets
52 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field No magnetic charges (magnetic monopoles) Moving charges (currents) make magnetic fields charges E no magnetic charges currents B
53 Maxwell s Equations Complete theory of electricity and magnetism Electric charges make electric field No magnetic charges (no magnetic monopoles) Moving charges (currents) make magnetic fields Changing magnet fields make electric fields Faraday s Law
54
Today. Laws of Motion. Conservation Laws. Gravity. tides
Today Laws of Motion Conservation Laws Gravity tides Newton s Laws of Motion Our goals for learning: Newton s three laws of motion Universal Gravity How did Newton change our view of the universe? He realized
More informationChapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity. Copyright 2009 Pearson Education, Inc.
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity How do we describe motion? Precise definitions to describe motion: Speed: Rate at which object moves speed = distance time
More informationAdios Cassini! Crashed into Saturn 9/15/17 after 20 years in space. https://saturn.jpl.nasa.gov/mission/grand-finale/overview/
Adios Cassini! Crashed into Saturn 9/15/17 after 20 years in space https://saturn.jpl.nasa.gov/mission/grand-finale/overview/ Laws of Motion Conservation Laws Gravity tides Today Why are astronauts weightless
More informationNewton s Laws and the Nature of Matter
Newton s Laws and the Nature of Matter The Nature of Matter Democritus (c. 470-380 BCE) posited that matter was composed of atoms Atoms: particles that can not be further subdivided 4 kinds of atoms: earth,
More information4.1 Describing Motion. How do we describe motion? Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity 4.1 Describing Motion Our goals for learning: How do we describe motion? How is mass different from weight? How do we describe
More informationChapter 5 Centripetal Force and Gravity. Copyright 2010 Pearson Education, Inc.
Chapter 5 Centripetal Force and Gravity v Centripetal Acceleration v Velocity is a Vector v It has Magnitude and Direction v If either changes, the velocity vector changes. Tumble Buggy Demo v Centripetal
More informationThe Cosmic Perspective Seventh Edition. Making Sense of the Universe: Understanding Motion, Energy, and Gravity. Chapter 4 Lecture
Chapter 4 Lecture The Cosmic Perspective Seventh Edition Making Sense of the Universe: Understanding Motion, Energy, and Gravity 2014 Pearson Education, Inc. Making Sense of the Universe: Understanding
More informationAstro Lecture 12. Energy and Gravity (Cont d) 13/02/09 Habbal Astro Lecture 12 1
Astro 110-01 Lecture 12 Energy and Gravity (Cont d) 13/02/09 Habbal Astro110-01 Lecture 12 1 Energy due to movement of Kinetic Energy: object E k = ½ m v 2 13/02/09 Habbal Astro110-01 Lecture 12 2 Gravitational
More informationHow do we describe motion?
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity How do we describe motion? Precise definitions to describe motion: Speed: Rate at which object moves example: speed of
More informationObservational Astronomy - Lecture 4 Orbits, Motions, Kepler s and Newton s Laws
Observational Astronomy - Lecture 4 Orbits, Motions, Kepler s and Newton s Laws Craig Lage New York University - Department of Physics craig.lage@nyu.edu February 24, 2014 1 / 21 Tycho Brahe s Equatorial
More information4.3 Conservation Laws in Astronomy
4.3 Conservation Laws in Astronomy Our goals for learning: Why do objects move at constant velocity if no force acts on them? What keeps a planet rotating and orbiting the Sun? Where do objects get their
More informationChapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity. Copyright 2012 Pearson Education, Inc.
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity 1 4.1 Describing Motion: Examples from Everyday Life Our goals for learning: How do we describe motion? How is mass different
More informationLecture: October 1, 2010
Lecture: October 1, 2010 How long would it take to walk to Alpha Centauri? Announcements: Next Observatory Opportunity: Wednesday October 6 Phases of Matter the phases solid liquid gas plasma depend on
More information4.1 Describing Motion
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity 4.1 Describing Motion Our goals for learning: How do we describe motion? How is mass different from weight? How do we describe
More information5. Universal Laws of Motion
5. Universal Laws of Motion If I have seen farther than others, it is because I have stood on the shoulders of giants. Sir Isaac Newton (164 177) Physicist Image courtesy of NASA/JPL Sir Isaac Newton (164-177)
More informationUniversal gravitation
Universal gravitation Physics 211 Syracuse University, Physics 211 Spring 2015 Walter Freeman February 22, 2017 W. Freeman Universal gravitation February 22, 2017 1 / 14 Announcements Extra homework help
More informationChapter 13. Gravitation
Chapter 13 Gravitation e = c/a A note about eccentricity For a circle c = 0 à e = 0 a Orbit Examples Mercury has the highest eccentricity of any planet (a) e Mercury = 0.21 Halley s comet has an orbit
More informationHow do we describe motion?
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity 4.1 Describing Motion: Examples from Everyday Life Our goals for learning: How do we describe motion? How is mass different
More informationIsaac Newton & Gravity
Isaac Newton & Gravity Isaac Newton was born in England in 1642 the year that Galileo died. Newton would extend Galileo s study on the motion of bodies, correctly deduce the form of the gravitational force,
More informationFinding Extrasolar Planets. I
ExtraSolar Planets Finding Extrasolar Planets. I Direct Searches Direct searches are difficult because stars are so bright. How Bright are Planets? Planets shine by reflected light. The amount reflected
More informationAgenda Announce: 4.1 Describing Motion. Tests. How do we describe motion?
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity Agenda Announce: Stony Brook talk this Friday on Precision Cosmology Project Part I due in one week before class: one paragraph
More informationBasic Physics. Isaac Newton ( ) Topics. Newton s Laws of Motion (2) Newton s Laws of Motion (1) PHYS 1411 Introduction to Astronomy
PHYS 1411 Introduction to Astronomy Basic Physics Chapter 5 Topics Newton s Laws Mass and Weight Work, Energy and Conservation of Energy Rotation, Angular velocity and acceleration Centripetal Force Angular
More information9/13/ Describing Motion: Examples from Everyday Life. Chapter 4: Making Sense of the Universe Understanding Motion, Energy, and Gravity
9/13/17 Lecture Outline 4.1 Describing Motion: Examples from Everyday Life Chapter 4: Making Sense of the Universe Understanding Motion, Energy, and Gravity Our goals for learning: How do we describe motion?
More informationGravitation and the Motion of the Planets
Gravitation and the Motion of the Planets 1 Guiding Questions 1. How did ancient astronomers explain the motions of the planets? 2. Why did Copernicus think that the Earth and the other planets go around
More informationUniversal Gravitation
Universal Gravitation Newton s Law of Universal Gravitation Every particle in the Universe attracts every other particle with a force that is directly proportional to the product of their masses and inversely
More informationUnderstanding Motion, Energy & Gravity
Speed, Velocity & Acceleration Understanding Motion, Energy & Gravity Chapter 4 speed: distance traveled per unit time (e.g., m/s, mph, km/ hr) velocity: speed & direction acceleration: change in velocity
More informationKepler, Newton, and laws of motion
Kepler, Newton, and laws of motion First: A Little History Geocentric vs. heliocentric model for solar system (sec. 2.2-2.4)! The only history in this course is this progression: Aristotle (~350 BC) Ptolemy
More informationOutline for Today: Newton s Law of Universal Gravitation The Gravitational Field Orbital Motion Gravitational Potential Energy. Hello!
PHY131H1F - Class 13 Outline for Today: Newton s Law of Universal Gravitation The Gravitational Field Orbital Motion Gravitational Potential Energy Under the Flower of Kent apple tree in the Woolsthorpe
More informationCopyright 2008 Pearson Education, Inc., publishing as Pearson Addison-Wesley.
Chapter 13. Newton s Theory of Gravity The beautiful rings of Saturn consist of countless centimeter-sized ice crystals, all orbiting the planet under the influence of gravity. Chapter Goal: To use Newton
More informationUnderstanding Motion, Energy & Gravity
Speed, Velocity & Acceleration Understanding Motion, Energy & Gravity Chapter 4 speed: distance traveled per unit time (e.g., m/s, mph, km/ hr) velocity: speed & direction acceleration: change in velocity
More informationF = ma. G mm r 2. S center
In the early 17 th century, Kepler discovered the following three laws of planetary motion: 1. The planets orbit around the sun in an ellipse with the sun at one focus. 2. As the planets orbit around the
More informationLecture 16. Gravitation
Lecture 16 Gravitation Today s Topics: The Gravitational Force Satellites in Circular Orbits Apparent Weightlessness lliptical Orbits and angular momentum Kepler s Laws of Orbital Motion Gravitational
More informationHow do we describe motion?
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity If I have seen farther than others, it is because I have stood on the shoulders of giants. Sir Isaac Newton (1642 1727)
More informationLecture 1a: Satellite Orbits
Lecture 1a: Satellite Orbits Meteorological Satellite Orbits LEO view GEO view Two main orbits of Met Satellites: 1) Geostationary Orbit (GEO) 1) Low Earth Orbit (LEO) or polar orbits Orbits of meteorological
More informationGravitation and the Waltz of the Planets
Gravitation and the Waltz of the Planets Chapter Four Guiding Questions 1. How did ancient astronomers explain the motions of the planets? 2. Why did Copernicus think that the Earth and the other planets
More informationGravitation and the Waltz of the Planets. Chapter Four
Gravitation and the Waltz of the Planets Chapter Four Guiding Questions 1. How did ancient astronomers explain the motions of the planets? 2. Why did Copernicus think that the Earth and the other planets
More informationToday. Events. Energy. Gravity. Homework Due Next time. Practice Exam posted
Today Energy Gravity Events Homework Due Next time Practice Exam posted Autumn is here! Autumnal equinox occurred at 11:09pm last night night and day very nearly equal today days getting shorter Moon is
More information2010 Pearson Education, Inc. Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity 4.1 Describing Motion: Examples from Daily Life Some of the topics we will explore: How do we describe motion? (Speed,
More informationHow do we describe motion?
Chapter 4 Making Sense of the Universe: Understanding Motion, Energy, and Gravity How do we describe motion? Precise definitions to describe motion: Speed: Rate at which object moves $ speed = distance!#"units
More informationMidterm 3 Thursday April 13th
Welcome back to Physics 215 Today s agenda: rolling friction & review Newtonian gravity Planetary orbits Gravitational Potential Energy Physics 215 Spring 2017 Lecture 13-1 1 Midterm 3 Thursday April 13th
More informationBasics of Kepler and Newton. Orbits of the planets, moons,
Basics of Kepler and Newton Orbits of the planets, moons, Kepler s Laws, as derived by Newton. Kepler s Laws Universal Law of Gravity Three Laws of Motion Deriving Kepler s Laws Recall: The Copernican
More informationChapter 13. Universal Gravitation
Chapter 13 Universal Gravitation Planetary Motion A large amount of data had been collected by 1687. There was no clear understanding of the forces related to these motions. Isaac Newton provided the answer.
More informationFirst exam next Wednesday. Today in class Review: Motion, Gravity. Gravity and Orbits. Review: Motion. Newton s Laws of Motion. Gravity and Orbits
Review: s of First exam next Wednesday Today in class Review:, Gravity Gravity and Gravity and Review: s of Review: Gravity and Newton s laws of motion Review: s of 1. Momentum (qualitative) 2. Force and
More informationLecture Fall 2005 Astronomy 110 1
Lecture 9 + 10 Fall 2005 Astronomy 110 1 Isaac Newton and the birth of Physics If I have seen farther than others, it is because I have stood on the shoulders of giants. Sir Isaac Newton (1642 1727) Nature
More informationCopyright 2009, August E. Evrard.
Unless otherwise noted, the content of this course material is licensed under a Creative Commons BY 3.0 License. http://creativecommons.org/licenses/by/3.0/ Copyright 2009, August E. Evrard. You assume
More informationAstro 210 Lecture 8 Feb 4, 2011
Astro 210 Lecture 8 Feb 4, 2011 Announcements HW2 due apologies for the erratum HW3 available, due next Friday HW1 Q8 bonus still available register your iclicker; link on course webpage Planetarium: shows
More informationPhysics Lecture 03: FRI 29 AUG
Physics 23 Jonathan Dowling Isaac Newton (642 727) Physics 23 Lecture 03: FRI 29 AUG CH3: Gravitation III Version: 8/28/4 Michael Faraday (79 867) 3.7: Planets and Satellites: Kepler s st Law. THE LAW
More informationDownloaded from
Chapter 8 (Gravitation) Multiple Choice Questions Single Correct Answer Type Q1. The earth is an approximate sphere. If the interior contained matter which is not of the same density everywhere, then on
More informationNewton s Gravitational Law
1 Newton s Gravitational Law Gravity exists because bodies have masses. Newton s Gravitational Law states that the force of attraction between two point masses is directly proportional to the product of
More informationSaint Lucie County Science Scope and Sequence
Course: Honors Physics 1 Course Code: 2003390 UNIT 4 TOPIC of STUDY: Newton s Laws of Motion and the Law of Gravity STANDARDS: 10: Energy, 12: Motion ~Net force produces motion ~There are four fundamental
More informationOutline for Today: Newton s Law of Universal Gravitation The Gravitational Field Orbital Motion Gravitational Potential Energy
PHY131H1F - Class 13 Outline for Today: Newton s Law of Universal Gravitation The Gravitational Field Orbital Motion Gravitational Potential Energy Under the Flower of Kent apple tree in the Woolsthorpe
More informationMore examples: Summary of previous lecture
More examples: 3 N Individual Forces Net Force 5 N 37 o 4 N Summary of previous lecture 1 st Law A net non zero force is required to change the velocity of an object. nd Law What happens when there is
More informationThe Hertzsprung Russell Diagram. The Main Sequence
The Hertzsprung Russell Diagram H R diagram plots stellar luminosity against surface temperature Luminosity ranges 10-4 10 4 L. Temperature ranges by a factor of 10 increases to the left spectral sequence
More informationMotion. Argument: (i) Forces are needed to keep things moving, because they stop when the forces are taken away (evidence horse pulling a carriage).
1 Motion Aristotle s Study Aristotle s Law of Motion This law of motion was based on false assumptions. He believed that an object moved only if something was pushing it. His arguments were based on everyday
More informationLecture 9 Chapter 13 Gravitation. Gravitation
Lecture 9 Chapter 13 Gravitation Gravitation UNIVERSAL GRAVITATION For any two masses in the universe: F = Gm 1m 2 r 2 G = a constant evaluated by Henry Cavendish +F -F m 1 m 2 r Two people pass in a hall.
More informationLecture Outline. Chapter 13 Gravity Pearson Education, Inc. Slide 13-1
Lecture Outline Chapter 13 Gravity Slide 13-1 The plan Lab this week: exam problems will put problems on mastering for chapters without HW; will also go over exam 2 Final coverage: now posted; some sections/chapters
More information11 Newton s Law of Universal Gravitation
Physics 1A, Fall 2003 E. Abers 11 Newton s Law of Universal Gravitation 11.1 The Inverse Square Law 11.1.1 The Moon and Kepler s Third Law Things fall down, not in some other direction, because that s
More informationWelcome back to Physics 211. Physics 211 Spring 2014 Lecture Gravity
Welcome back to Physics 211 Today s agenda: Newtonian gravity Planetary orbits Gravitational Potential Energy Physics 211 Spring 2014 Lecture 14-1 1 Gravity Before 1687, large amount of data collected
More informationChapter 4. Motion and gravity
Chapter 4. Motion and gravity Announcements Labs open this week to finish. You may go to any lab section this week (most people done). Lab exercise 2 starts Oct 2. It's the long one!! Midterm exam likely
More informationFORCE. The 4 Fundamental Forces of Nature
FORCE - Force a push or pull. Results only from interaction with another object. Without interaction, forces cannot be present. - Measured in Newtons (N) 1 Newton is the amount of force required to give
More informationCIRCULAR MOTION AND UNIVERSAL GRAVITATION
CIRCULAR MOTION AND UNIVERSAL GRAVITATION Uniform Circular Motion What holds an object in a circular path? A force. String Friction Gravity What happens when the force is diminished? Object flies off in
More informationWelcome back to Physics 215. Review gravity Oscillations Simple harmonic motion
Welcome back to Physics 215 Review gravity Oscillations Simple harmonic motion Physics 215 Spring 2018 Lecture 14-1 1 Final Exam: Friday May 4 th 5:15-7:15pm Exam will be 2 hours long Have an exam buddy
More informationWelcome back to Physics 215
Welcome back to Physics 215 Today s agenda: More rolling without slipping Newtonian gravity Planetary orbits Gravitational Potential Energy Physics 215 Spring 2018 Lecture 13-1 1 Rolling without slipping
More informationPulsars ASTR2110 Sarazin. Crab Pulsar in X-rays
Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other
More informationFEYNMAN SIMPLIFIED 1A: PROBLEM SET ANSWERS
FEYNMAN SIMPLIFIED 1A: PROBLEM SET ANSWERS EVERYONE S GUIDE TO THE FEYNMAN LECTURES ON PHYSICS BY ROBERT L. PICCIONI, PH.D. This Book This ebook contains problems to help readers of Feynman Simplified:
More information1. Which of the following correctly lists our cosmic address from small to large?
1. Which of the following correctly lists our cosmic address from small to large? (a) Earth, solar system, Milky Way Galaxy, Local Group, Local Super Cluster, universe (b) Earth, solar system, Milky Way
More information1 Summary of Chapter 2
General Astronomy (9:61) Fall 01 Lecture 7 Notes, September 10, 01 1 Summary of Chapter There are a number of items from Chapter that you should be sure to understand. 1.1 Terminology A number of technical
More informationClassical mechanics: conservation laws and gravity
Classical mechanics: conservation laws and gravity The homework that would ordinarily have been due today is now due Thursday at midnight. There will be a normal assignment due next Tuesday You should
More information9/12/2010. The Four Fundamental Forces of Nature. 1. Gravity 2. Electromagnetism 3. The Strong Nuclear Force 4. The Weak Nuclear Force
The Four Fundamental Forces of Nature 1. Gravity 2. Electromagnetism 3. The Strong Nuclear Force 4. The Weak Nuclear Force The Universe is made of matter Gravity the force of attraction between matter
More informationPHYSICS. Chapter 13 Lecture FOR SCIENTISTS AND ENGINEERS A STRATEGIC APPROACH 4/E RANDALL D. KNIGHT Pearson Education, Inc.
PHYSICS FOR SCIENTISTS AND ENGINEERS A STRATEGIC APPROACH 4/E Chapter 13 Lecture RANDALL D. KNIGHT Chapter 13 Newton s Theory of Gravity IN THIS CHAPTER, you will learn to understand the motion of satellites
More informationNewton's Laws of Motion
Newton's Laws of Motion 1 Newton's Laws of Motion: First Law Law of Inertia An object at rest remains at rest unless acted upon by an outside force. - provides a qualitative definition of force. 2 An object
More informationAstr 2320 Tues. Jan. 24, 2017 Today s Topics Review of Celestial Mechanics (Ch. 3)
Astr 2320 Tues. Jan. 24, 2017 Today s Topics Review of Celestial Mechanics (Ch. 3) Copernicus (empirical observations) Kepler (mathematical concepts) Galileo (application to Jupiter s moons) Newton (Gravity
More informationA) Yes B) No C) Impossible to tell from the information given.
Does escape speed depend on launch angle? That is, if a projectile is given an initial speed v o, is it more likely to escape an airless, non-rotating planet, if fired straight up than if fired at an angle?
More informationStudents' Alternate Conceptions in Introductory Physics
Students' Alternate Conceptions in Introductory Physics The following is a list of preconceptions and misconceptions that high school physics teachers and college professors have recognized in their students.
More informationThe beginnings of physics
The beginnings of physics Astronomy 101 Syracuse University, Fall 2018 Walter Freeman October 9, 2018 Astronomy 101 The beginnings of physics October 9, 2018 1 / 28 Announcements No office hours this week
More informationChapter 13 Gravity Pearson Education, Inc. Slide 13-1
Chapter 13 Gravity Slide 13-1 The plan Lab this week: there will be time for exam problems Final exam: sections posted today; some left out Final format: all multiple choice, almost all short problems,
More informationAtomic Physics 3 ASTR 2110 Sarazin
Atomic Physics 3 ASTR 2110 Sarazin Homework #5 Due Wednesday, October 4 due to fall break Test #1 Monday, October 9, 11-11:50 am Ruffner G006 (classroom) You may not consult the text, your notes, or any
More informationApples and Planets. PTYS Feb 2008
Apples and Planets PTYS206-2 28 Feb 2008 List of Symbols F, force a, acceleration (not semi-major axis in this lecture) v, velocity M, mass of Sun m, mass of planet d, general distance r,radius of circle,
More informationWiley Plus Reminder! Assignment 1
Wiley Plus Reminder! Assignment 1 6 problems from chapters and 3 Kinematics Due Monday October 5 Before 11 pm! Chapter 4: Forces and Newton s Laws Force, mass and Newton s three laws of motion Newton s
More informationStellar Interiors ASTR 2110 Sarazin. Interior of Sun
Stellar Interiors ASTR 2110 Sarazin Interior of Sun Test #1 Monday, October 9, 11-11:50 am Ruffner G006 (classroom) You may not consult the text, your notes, or any other materials or any person Bring
More informationGravitation and Newton s Synthesis
Lecture 10 Chapter 6 Physics I 0.4.014 Gravitation and Newton s Synthesis Course website: http://faculty.uml.edu/andriy_danylov/teaching/physicsi Lecture Capture: http://echo360.uml.edu/danylov013/physics1spring.html
More informationMaking Sense of the Universe: Understanding Motion, Energy, and Gravity Pearson Education, Inc.
Making Sense of the Universe: Understanding Motion, Energy, and Gravity 4.1 Describing Motion: Examples from Daily Life Our goals for learning: How do we describe motion? How is mass different from weight?
More informationThe Heliocentric Model of Copernicus
Celestial Mechanics The Heliocentric Model of Copernicus Sun at the center and planets (including Earth) orbiting along circles. inferior planets - planets closer to Sun than Earth - Mercury, Venus superior
More informationHere are some internet links to instructional and necessary background materials:
The general areas covered by the University Physics course are subdivided into major categories. For each category, answer the conceptual questions in the form of a short paragraph. Although fewer topics
More informationMonday, October 10, 2011
the shuttle blasts off Then comes the tremendous pressure of three G s and the sudden release into weightlessness as the ship leaves the gravitational field behind -from The Arizona Republic 1 Chapter
More informationLecture 8. Kepler's IInd: Angular Momentum
Lecture 8 Gravity and Orbits Angular Momentum Deducing the Law of Gravity Escape Orbits Orbits: common misconceptions Feb 3, 2006 Astro 100 Lecture 8 1 Kepler's IInd: Angular Momentum Kepler's IInd: (motion
More informationWelcome back to Physics 215
Welcome back to Physics 215 Today s agenda: Gravity 15-2 1 Current assignments HW#15 due Monday, 12/12 Final Exam, Thursday, Dec. 15 th, 3-5pm in 104N. Two sheets of handwritten notes and a calculator
More informationEvents. Notable. more gravity & orbits Tides. Homework Due Next time; Exam review (Sept. 26) Exam I on Sept. 28 (one week from today)
Today more gravity & orbits Tides Events Homework Due Next time; Exam review (Sept. 26) Exam I on Sept. 28 (one week from today) Notable Fall equinox (Sept. 22 - tomorrow at 4:02PM) Escape Velocity M r
More informationComments about HW #1 Sunset observations: Pick a convenient spot (your dorm?) Try to get 1 data point per week Keep a lab notebook with date, time,
Comments about HW #1 Sunset observations: Pick a convenient spot (your dorm?) Try to get 1 data point per week Keep a lab notebook with date, time, weather, comments Mark down bad weather attempts Today:
More informationChapter 1. Basic Concepts. 1.1 Trajectories
Chapter 1 Basic Concepts 1.1 Trajectories We shall be concerned in this course with the motion of particles. Larger bodies will (with a few exceptions) be made up of collections of particles. We will find
More informationAST1100 Lecture Notes
AST1100 Lecture Notes 5 The virial theorem 1 The virial theorem We have seen that we can solve the equation of motion for the two-body problem analytically and thus obtain expressions describing the future
More informationOccam s Razor: William of Occam, 1340(!)
Reading: OpenStax, Chapter 2, Section 2.2 &2.4, Chapter 3, Sections 3.1-3.3 Chapter 5, Section 5.1 Last time: Scales of the Universe Astro 150 Spring 2018: Lecture 2 page 1 The size of our solar system,
More informationPHYS 106 Fall 2151 Homework 3 Due: Thursday, 8 Oct 2015
PHYS 106 Fall 2151 Homework 3 Due: Thursday, 8 Oct 2015 When you do a calculation, show all your steps. Do not just give an answer. You may work with others, but the work you submit should be your own.
More informationCircular Motion. Gravitation
Circular Motion Gravitation Circular Motion Uniform circular motion is motion in a circle at constant speed. Centripetal force is the force that keeps an object moving in a circle. Centripetal acceleration,
More informationA force is could described by its magnitude and by the direction in which it acts.
8.2.a Forces Students know a force has both direction and magnitude. P13 A force is could described by its magnitude and by the direction in which it acts. 1. Which of the following could describe the
More informationDescribing Motion. Newton Newton s Laws of Motion. Position Velocity. Acceleration. Key Concepts: Lecture 9
Key Concepts: Lecture 9 Newton Newton s Laws of Motion More on Kepler s Laws Describing Motion Position Velocity Rate of change of position (speed & direction) 80 km/hr Acceleration 40 km/hr Rate of change
More informationChapter 9 Circular Motion Dynamics
Chapter 9 Circular Motion Dynamics Chapter 9 Circular Motion Dynamics... 9. Introduction Newton s Second Law and Circular Motion... 9. Universal Law of Gravitation and the Circular Orbit of the Moon...
More informationChapter 9 Lecture. Pearson Physics. Gravity and Circular Motion. Prepared by Chris Chiaverina Pearson Education, Inc.
Chapter 9 Lecture Pearson Physics Gravity and Circular Motion Prepared by Chris Chiaverina Chapter Contents Newton's Law of Universal Gravity Applications of Gravity Circular Motion Planetary Motion and
More informationNotes on Planetary Motion
(1) Te motion is planar Notes on Planetary Motion Use 3-dimensional coordinates wit te sun at te origin. Since F = ma and te gravitational pull is in towards te sun, te acceleration A is parallel to te
More informationChapter 12 Gravity. Copyright 2010 Pearson Education, Inc.
Chapter 12 Gravity Units of Chapter 12 Newton s Law of Universal Gravitation Gravitational Attraction of Spherical Bodies Kepler s Laws of Orbital Motion Gravitational Potential Energy Energy Conservation
More information