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Study Guides for AST201H1 at University of Toronto St. George (UTSG)

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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 23: Main Sequence, Cosmic Distance Ladder, Edwin Hubble

OC25354552 Page
30 Mar 2019
0
The stars all have the same age and the stars are all at around the same distance. They are all at around the same distance. Step 1: use radar to deter
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 24: Graph Paper, Nucleosynthesis, Neutrino

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30 Mar 2019
0
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 22: Elliptical Galaxy, Disc Galaxy, Cosmic Distance Ladder

OC25354552 Page
21 Mar 2019
0
Irregular galaxies are a result of a collision of two galaxies (mergers. ) When its finish its star bursts, it will probably another disk galaxy. But i
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 20: Semi-Major And Semi-Minor Axes, Orbital Period, Vera Rubin

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17 Mar 2019
0
Johannes kepler: had worked from tycho bache"s data and came up with an accurate description of the motion of the planets. #1: planets orbit the sun in
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 19: Light Pollution

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18 Mar 2019
0
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 18: Angular Momentum, Degenerate Matter, Tablespoon

OC25354552 Page
10 Mar 2019
0
Topic: the afterlives of massive stars, neutron stars. The finale stage of a massive star"s life. When there is no more core fusion then gravity starts
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 15: AST201 lecture 13

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2 Mar 2019
0
Topic: lifecycle of a 1 solar mass star. The core expanding and cooling slows things down and stops fusion in the sun"s core from happening faster and
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 16: Neon Neon, Nucleon, Solar Mass

OC25354552 Page
1 Mar 2019
0
Talking about what happens to a star that is above 8 solar masses, and the difference between a low-mass star and high mass star. When all the helium i
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 12: AST 201 - lecture 12

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16 Feb 2019
0
Rule #1 = hotter is brighter if it is the same size. If a star is bluer than it is hotter, if it is redder than it is cooler. In our story, we have com
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 11: AST 201 - lecture 11

OC25354552 Page
16 Feb 2019
0
In the previous lecture we discussed how to find certain properties of stars without having to go send probes to the stars. We can find the chemical co
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 10: AST 201 - lecture 10

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7 Feb 2019
0
If you know a star"s distance and its brightness, you can figure out the luminosity of a star. You can figure out the temperature by the colour it is a
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 9: Stellar Parallax, Inverse-Square Law

OC25354552 Page
5 Feb 2019
0
We have information about our sun, mostly because we have sent probes to measure things or observe the sun. However, we have information about distant
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 8: AST 201 LECTURE 8

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1 Feb 2019
0
A star with a spectrum in the middle (close to where the green light area is) appear white. That is why there is no green stars in the sky. Historicall
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 7: Cygnus X-1, Photon, Astronomical Object

OC25354552 Page
30 Jan 2019
0
The black hole in the centre of our galaxy is actually much larger than cygnus x-1. Some elements tend to escape being devoured by black holes, and the
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 6: Cygnus X-1, Event Horizon, Escape Velocity

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29 Jan 2019
0
If you shrank the size of earth while keeping its mass the same means that the escape speed goes up. If you keep crushing the earth smaller and smaller
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 5: Gravitational Lens, Strong Gravity, Equivalence Principle

OC25354552 Page
25 Jan 2019
0
Equivalence principle: no experiment can distinguish a difference between gravity pulling things back to the surface of earth and acceleration. We feel
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture Notes - Lecture 1: Vera Rubin, Spiral Galaxy, Orbital Speed

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19 Jan 2019
0
One patch of the night sky can have numerous galaxies. If you are looking at things in the sky, it actually means you are looking back in time, as ligh
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 4: AST201 - lecture 4

OC25354552 Page
20 Jan 2019
0
Objects will move with a constant speed and direction unless acted on by an external. You feel gravity every day, every other force you feel (wind, pus
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 2: LIGHT

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19 Jan 2019
0
How can you tell if a train has moved: you can be looking out the window, seeing if the landscape moves. If there are no windows, you can hear the trai
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UTSGAST201H1Bryan Gaensler, C. Barth Netterfield, Ilana MacDonaldWinter

AST201H1 Lecture 3: Relativity part 2

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15 Jan 2019
0
Time dilation: when someone is moving relative to you, their clock will seem to be running slower. Not only does time slow down, but also length. Thing
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UTSGAST201H1Ian SheltonFall

AST201H1- Midterm Exam Guide - Comprehensive Notes for the exam ( 14 pages long!)

OC105000614 Page
5 Oct 2017
0
Wavelength is the distance between two wave peaks. Frequency is the number of times per second that a wave vibrates up and down. This is like water, th
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UTSGAST201H1Bryan GaenslerWinter

[AST201H1] - Midterm Exam Guide - Ultimate 10 pages long Study Guide!

OC115122010 Page
6 Feb 2017
74
Ast101 lecture 3: time dilation and the twin paradox. The speed of light: light always travels at c (in a vacuum, slightly slower in air, no object wit
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UTSGAST201H1Michael ReidFall

[AST201H1] - Midterm Exam Guide - Ultimate 239 pages long Study Guide!

OC755883239 Page
5 Oct 2016
42
Ast201 - the sun: part 1 (chp 5. 1-5. 4) Can"t for diagonal or across our line of sight) for rotation- faster the object is rotating, the broader the w
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UTSGAST201H1Bryan GaenslerWinter

AST201H1 Midterm: Exam Study Notes

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18 May 2018
0
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UTSGAST201H1Bryan GaenslerFall

AST201H1 Midterm: AST201 Midterm study notes

OC11643159 Page
16 Feb 2017
5
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UTSGAST201H1Michael ReidWinter

AST201H1 Study Guide - Midterm Guide: Natural Resources Defense Council, Positron

OC5017118 Page
3 Mar 2016
55
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UTSGAST201H1AllWinter

AST201H1 Midterm: AST201 Test 1 Lecture notes

OC64961311 Page
22 Feb 2016
79
> trick question: if light behaves like a ball, then it would have speed of. 200mph + c in #2 (however this doesn"t make sense in real life since #6: s
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UTSGAST201H1Stefan MochnackiWinter

AST201H1 Study Guide - Midterm Guide: Length Contraction, Special Relativity, Dark Matter

OC4389462 Page
17 Oct 2015
49
Astronomy midterm review sketch of look back time : the further you look, the further in time you are looking. Dark energy and dark matter: it was firs
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UTSGAST201H1Michael ReidWinter

AST201H1 Study Guide - Midterm Guide: Spacetime, Positron, Spectroscopy

OC17104068 Page
16 Apr 2014
92
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UTSGAST201H1Michael ReidWinter

AST201H1 Study Guide - Midterm Guide: Neutrino, Superbubble

OC17104063 Page
16 Apr 2014
75
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UTSGAST201H1Michael ReidWinter

AST201H1 Study Guide - Midterm Guide: Weightlessness, Gravitational Time Dilation, Electromagnetic Spectrum

OC1652638 Page
10 Feb 2014
58
S2. 1 einstein"s revolution special relativity: an object is travelling relative to sth, no object can travel faster than the speed of light. 2 people
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UTSGAST201H1Michael ReidWinter

AST201H1 Study Guide - Midterm Guide: Helium Flash, Red Giant, Net Force

OC3292914 Page
30 Mar 2013
42
Cosmological redshift the expansion of the universe stretches out all the photons within it, shifting them to longer, redder wavelengths: tells us how
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