Study Guides (390,000)
CA (150,000)
UTSC (10,000)
Final

ASTA01H3 Study Guide - Final Guide: Exoplanet, Nuclear Fission, Meteoroid


Department
Astronomy
Course Code
ASTA01H3
Professor
Kristen Menou
Study Guide
Final

This preview shows half of the first page. to view the full 2 pages of the document.
1. Volume of sphere:
=
4
3฀฀
3
2. Density:
=
3฀
4฀฀3
3. m = apparent magnitude, I = flux:
1
2
=
2
.
5฀฀10
1
2
4. Comparison of star brightness:
1
2
=
10
0
.
4
1
2
5. M = absolute magnitude, d = distance in parsecs:
=
5฀฀10
 −
5
6. Angular size:
2฀
฀฀
7. Speed of object in circular orbit:
=
2฀฀
8. Kepler’s 3rd law:
2
=
฀฀
or
2฀฀
2
to
2
=
4฀2
฀฀
3
9. Cooling rate:
฀฀฀฀
฀฀฀฀
฀฀฀฀฀฀
10. Comparison of planet mass:
฀฀฀฀฀฀฀
1
฀฀฀฀฀฀฀
2

฀฀฀฀฀฀
1
฀฀฀฀฀฀
2
3
RV method: the exoplanet pulls on the star and the two bodies orbit around their common centre-of-mass.
Measuring the Doppler shift of the starlight as it wobbles back-and-forth tells us about the presence of a
companion causing the star to wobble. Transit method: as the exoplanet’s orbit takes it between the star and
the observer, the exoplanet’s shadow causes the star to appear dimmer during the transit event.
Physical processes can shape a planet’s surface: impact cratering, erosion, plate tectonics, volcanism
Kepler's 1st law: Orbits of planets around sun are ellipses w/ sun at one focus, 2nd law: planets closer to sun
move faster, 3rd law: P (alpha) a; P = (a/1 AU)^(3/2) yrs
Meteoroid: body in space, Meteor: meteoroid enters atmosphere, Meteorite: meteor that hits ground
Asteroid: body orbiting sun, between Mars and Jupiter, Comet: ice and dust, near sun gas tail
Uranus (rotates on side) and Venus (rotates backwards): caused by large impacts
Nuclear fusion: elements of low atomic number fuse to form a heavier nucleus (exothermic)
Nuclear fission: heavy nucleus splits into parts releasing energy (exothermic)
Extrasolar planets: support solar nebula theory, Small planets: cold internally (cool faster) and geologically
inactive, Large planets: can be geologically active
Geological history of Earth: differentiation (separation of each planet’s materials into layers by density),
cratering and giant basin formation (heavy impacts), slow surface evolution (Earth’s crust is constantly
changing)
Condensation hypothesis: Earth/moon condensed from the same cloud of matter in the solar nebula
Capture hypothesis: moon formed elsewhere in the solar nebula and entered Earth’s orbit
Large-impact hypothesis: moon formed when planetesimal large as Mars smashed into proto-Earth (correct)
Drake’s equation (Civilizations in a galaxy): Nc = N* · fP · nHZ · fL · fI · Fs
N*: stars in galaxy, fP: fraction of stars having planets, nHZ: planets with water, fL: fraction of planets w/ life, fI:
fraction of intelligent life, Fs: fraction of star’s life during life is communicable.
Jupiter’s core: liquid hydrogen becomes metallic hydrogen under high pressure
Jupiter’s moons: Io, Europa (size of Earth’s moon), Ganymede, Callisto
Many moons are ‘captured’ asteroids
Callisto and Ganymede: look old heavily cratered and dark, interact w/ Jupiter’s magnetic field which
means they have mineral-rich water below their ice crusts
find more resources at oneclass.com
find more resources at oneclass.com
You're Reading a Preview

Unlock to view full version