Midterm 1 Review Office Hours Midterm 1 on Sept. 28th Mon 12-1pm - - PowerPoint PPT Presentation

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Midterm 1 Review Office Hours Midterm 1 on Sept. 28th Mon 12-1pm - - PowerPoint PPT Presentation

Jan 30, 2023 293 likes •828 views

Midterm 1 Review Office Hours Midterm 1 on Sept. 28th Mon 12-1pm Zane will cover Chapters 1-5 and lecture material Tues 1:30-3pm me Tues 5-6pm Randall Chapter 10 Reading Assignment due Monday,

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Fall 2018: Chapter 5 ASTR/PHYS 1060: The Universe

Midterm 1 Review

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Midterm 1 on Sept. 28th will cover Chapters 1-5 and lecture material Chapter 10 Reading Assignment due Monday, October 1st & Chapter 11 Reading Assignment due Friday, October 5th (in Canvas) Are your grades in Canvas correct??? Office Hours Mon 12-1pm Zane Tues 1:30-3pm me Tues 5-6pm Randall Wed 3-4pm Randall Thurs 11:45a-12:45pm Zane Fri 12-1pm me me: INSCC 320 Zane/Randall: JFB 325

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Fall 2018: Midterm 1 Review ASTR/PHYS 1060: The Universe

Exam Format

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50-60 min time limit: 10:45-11:35/45am Multiple Choice Questions 60-75% of total score Short Answer Questions 40-25% of total score may require calculations, but calculators not needed (or allowed)

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Fall 2018: Midterm 1 Review ASTR/PHYS 1060: The Universe

Chapter 1: Scales and How to Think Like a Scientist

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Scale by light-speed

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Scientific Method

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Scientific Notation

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106 = 1,000,000 5x109 = 5,000,000,000 2x102 x 3x103 = = one million = five billion 6x105 = 600,000 = six hundred thousand Calculator / Computer shorthand: 2e-7 = 2x10-7 = 0.0000002 (on exams and assignments, use the correct notation, not this shorthand)

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Fall 2018: Midterm 1 Review ASTR/PHYS 1060: The Universe

To conclude (or really, begin):

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Because light travels at a finite speed, looking far away is looking into the past 1011 Suns light 102-5 yr old There are ~100 billion stars in our Galaxy, the Milky Way We are made of stardust Nearby galaxies light 106+ yr old There are ~100 billion galaxies in the visible universe Distant galaxies light 109+ yr old

Gemini Planet Imager HR 8799

Most stars host planets (although mostly uninhabitable by our standards)

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Chapter 2: Celestial Sphere and Phases of the Moon

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It’s all just geometry and timing

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top view side view top view

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Important Points & Planes

  • n the Celestial Sphere

Project stars and planets on a sphere surrounding the Earth It is fictitious, but convenient for locating objects in the sky

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If you’re 30 degrees north of the equator:

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Max altitude of the Sun determined by where we are on Earth and where the Earth is in its orbit

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Seasonal Poetry

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The two reasons we have seasons Are both due to the Earth’s tilt, When our nearest pole Points toward Sol Its light shines to the hilt And stays in the sky Like a too-long deployed spy At risk of committing treason!

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Hey you, what’s your sign?

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Astrology is bunk!

(HINT: This will be an exam question.)

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Earth’s axis wobbles like a top: called Precession

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Why star rise/set times change

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About how many degrees does the Earth move in its orbit each day?

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Moon phases are easy to figure out once you have the right mental picture

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The apparent size of Venus correlates with its phase

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Eclipses

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http://www.graphicine.com/asa-smiths-illustrated-astronomy-eclipses/ courtesy of your fellow student Megan Clasper

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Fall 2018: Chapter ASTR/PHYS 1060: The Universe

The reason it’s two-faced is known, but how that happened is not!

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proto-Earth Mars-sized protoplanet

http://www.slate.com/blogs/bad_astronomy/2014/07/01/ the_moon_s_two_faces_why_are_they_so_different.html

Theory 1) two proto-Moons formed from collision, which later “gently” coalesced Theory 2) the Moon formed very close to the Earth, became tidally locked soon thereafter, and the heat from the Earth “evaporated” crust on the near side, which preferentially condensed on the cooler far side The Moon’s crust is thicker on the far side than the near side!

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Chapter 3: Laws of Motion and Gravity

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Epicycles

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https://en.wikipedia.org/wiki/Apparent_retrograde_motion Retrograde motion of Mars in 2005. Credit astrophotographer Tunc Tezel https://physics.weber.edu/schroeder/ua/ BeforeCopernicus.html

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Kepler’s 3 Laws

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1st Law: Orbits are elliptical 2nd Law: equal areas in equal times 3rd Law: period depends on distance (Period of Planet [in years])2 = (Average Distance of Planet from Star [in AU])3

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Newton’s 3 Laws

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1) Law of Inertia: Objects at rest stay at rest, objects in motion stay in motion (Galileo figured this one out) 2) Motion is changed by unbalanced forces acceleration = force / mass 3) Forces always come in pairs and those pairs are always equal in strength but opposite in direction

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Gravity and Orbits

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17500 miles/hr

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Not zero gravity. All objects are in free fall.

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Escape Velocity

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For Earth vesc ~ 25,000 miles/hour

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Chapter 4: Light and Telescopes

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Light is “quantized” Its energy is proportional to frequency

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Electromagnetic Spectrum

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xkcd.com

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Telescope Resolution

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Making Images

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Charged Coupled Devices (CCDs) Filters

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Andromeda Galaxy - Our Nearest Neighbor

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Chapter 5: Star and Planet Formation and Exoplanets

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Life Cycle of Gas and Stars

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Thermal Pressure Turbulence Magnetic Fields

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Any small net spin of the collapsing cloud is amplified as it becomes smaller

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Conservation of Angular Momentum: L = m v r

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Sun 99.85%

Outer Planets 0.134% Terrestrial Planets 0.001%

Mass Distribution in the Solar System

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Inner versus outer planets

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How to find planets

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  • Detect them directly
  • Detect their influence on their star
  • Image the planet
  • Detect its atmosphere in a spectrum




  • Measure light blocked from the star when

the planet eclipses it

  • Measure the star’s motion due to the

planet’s gravity

Direct Imaging Transit Method Radial Velocity Method

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Doppler Shift of Light

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λobserved − λemitted λemitted = ∨ c

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Transit Method

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Starlight is blocked by the planet, reducing the amount of light detected from the star

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Fall 2018: Midterm 1 Review ASTR/PHYS 1060: The Universe

Happy Studying!

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