Phys 1810 Lecture 11: Office hours Allen 514

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Phys 1810 Lecture 11: Office hours Allen 514 (Image unknown origin) Office hours Allen 514 Monday (today) between 3-4pm This Class Telescopes Overview of planets READ BEFORE COMING TO CLASS Solar System Chapt 6 formation of the moon 8.8 exoplanets Chapt 15 Topics include scale, objects terrestrial vs jovian planetary system formation including (differentiation) Mars Earth – climate change planetary system formation including differentiation ALL NOTES COPYRIGHT JAYANNE ENGLISH Does everyone have the password?

Hubble Deep Field Light Gathering Power 2. Diffraction-limited Resolution 3. “Seeing”

3. Seeing

Mountaintop Sites build high to get above most of the atmosphere summary Recall column build high to get above most of the atmosphere

Highlights of Previous Class: summary Recall column - Resolution is effected by atmospheric seeing. - Atmospheric transmission filters electromagnetic radiation. Seeing is less affected at longer wavelengths. Near IR ground-based observations can be as high resolution as optical observations on the HST. The atmosphere filters electromagnetic radiation to us ground based folk

Can observe at wavelengths that the Earth’s atmosphere blocks. Above the atmosphere far infrared view quite different Optical Far Infrared Can observe at wavelengths that the Earth’s atmosphere blocks.

Which wavelength range(s) do you plan to observe at? Why? Review: Imagine that you and your neighbours are part of an international consortium planning to build a telescope to study very powerful, energetic supernova explosions. Discuss the following details of your plans: Which wavelength range(s) do you plan to observe at? Why? Will it be a space-based or ground-based observatory? Why? Will these choices give you high or low resolution? Why? Results of discussion (which is a synthesis of the material recently covered): the wavelength regime for objects with a lot of energy: Gamma-ray, X-ray, UV. Multi-wavelength observations are good too since Gamma-rays and X-rays are absorbed by dust that might be in between the earth and the SN. Supernova remnants (SNR) are discovered at radio wavelengths for example. space-based telescopes are necessary for the high energy wavelengths like gamma-ray and x-ray since they are affected by the atmosphere being opaque for those wavelengths. Space-based is good for optical observations due to seeing. ground-based for the radio telescopes since seeing doesn’t affect the longer wavelengths of IR and beyond. it is also good to go to high energy regime since the resolution is higher with shorter wavelength. (Note – there is no one right answer, as one can see from the multi-wavelength discussion.)

Afternoon class, see Lecture 9 for Doppler Shift

Planets in Our Solar System. Now we have fundamentals: Major force: gravity  motion EM radiation: how it tells us about matter (elements, particles) and energy (temperature, magnetic fields) and forces (gravity) Detect radiation: telescopes and instruments  COSMIC TOPICS

Solar System Overview: Planet Definitions Classical Planet Orbits sun. Massive enough that its own gravity has caused its shape to be nearly spherical. It’s “cleared the neighbourhood” around its orbit of other bodies. either by colliding with (sweeping up) the debris, or gravitationally kicking the debris out of its path (slingshot effect). This leaves us with 8 planets.

Solar System Overview: Planet Definitions Dwarf Planet Orbits the sun. Massive enough that is own gravity has caused its shape to be spherical. Is not a satellite of another body. (Has not cleared its neighbourhood.) Exact wording is at http://www.iau.org/public_press/news/detail/iau0602/ . See International Astronomical Union Resolution 5A. Examples: Pluto Eris (1.3 * Pluto’s mass) Ceres (in the asteroid belt) Objects at Neptune and beyond are called Trans-Neptune Objects (TNO) and those TNO that are similar to Pluto are called plutoids.

revolve & rotate in the same direction as other planets? Solar System Overview: What does the class already know about the classical planets? For each planet: revolve & rotate in the same direction as other planets? primarily composed of rock or of gas? # Earth Masses, # Earth radii small or large? (i.e. closer to Earth size or Jupiter size?) in outer region or inner region of solar system? hot or cold? surface T in Kelvin Lots of moons? Any other details are welcome  (eg. Does it have rings? B field?) If a planet spins in the same direction as its orbit, its spin is called “prograde”. If a planet spins in the opposite direction to its orbital motion, that spin is called “retrograde”. See contributed notes from planet teams and do your own research to supplement these powerpoint presentations.

Solar System Overview: Add to this table Temperature & Magnetic field. (Not kg, km but Earth mass and radii) How do we know these things? we’ll do that after we talk about the classical planets so we don’t run out of time for our competition. The first 8 are planets. Note the second column.

Keplerian Rotation Curve. Solar System Overview Keplerian Rotation Curve.

Solar System Overview The density in kg/m If the density of an object is less than that of water, then it will float. The density in kg/m 1000 for water; if less than this, floats in water. 2000-3000 for rocks; 8000 for iron Note 2nd last column & density of Earth. Ask yourself which planets have densities like rocks/iron? Float on water? 3

How do we know these characteristics? Check the notes that you wrote in class for deriving: distance diameter or orbital radius mass density Wrote notes on overhead in class.