EPSC 201 Wednesday September 11, 2013.docx

4 Pages
111 Views
Unlock Document

Department
Earth & Planetary Sciences
Course
EPSC 201
Professor
Anthony Williams- Jones
Semester
Fall

Description
Wednesday, September 11, 2013 Understanding Planet Earth EPSC 201 The Big Bang • The universe started off with a bang- from big bang theory everything is supposed to unfold- eventually get to galaxies and stars • Big bang is perceived as a singularity • Universe was infitiely small and hot- it evolved there after by expanding fairly rapidly • Whole of the universe was compressed into a small volume- started to evolve and things expanded extremely rapidly, the first few fractions of a second, it was supposed to be over very quickly • Matter was started to be seen- matter is extremely hot • Anti- matter were destroying themselves- we wouldn’t have been here if matter hadn’t won • Slow to large expansion • Electron- negatively charged particle- very small • Positron- positively charged- if they interact matter will be annihilated • Doppler Effect- change of frequency of a wave • Electromagnetic spectrum- long wave length to short wave length • Light moves in wa • Larger particles begin to form once the universe starts cooling- 3 minutes • Hydrogen has 1 proton and when becomes an atom will have one electron • Deuterium Part of the hydrogen family because it has a proton and neutron- has double the mass • Building larger nuclei • Build them by nucleosynthesis • Nuclear reaction has occurred. 2 protons hit and form 1 proton and 1 neutron through nuclear fusion creating particles with a huger mass • Equal number of protons and neutrons- helium • Colliding subatomic particles, to form progressively larger nuclei • Forming nuclei of atoms / relatively light atoms • 300 thousand years- 6000 degrees • The rate at which the universe is cooling is slowly down immensely • Particles are slowing down and expanding • Electrons now start to get captured by nuclei • First atoms begin to form • Decoupling from energy to matter – 300 thousand to 380 thousand • Light energy from the mass • Light energy is bouncing off protons, electrons, becoming scattered • Scattering stops because of atoms have been created and atoms are not scattering the light • 380,000- last scattering occurs • Atoms are not absorbing the thermal radiation, therefore we can detect the radiation • Cosmic Microwave Background Information • When light hits water molecules the light gets scattered so the object the light is trying to display becomes destroyed • Black lines represent the continuous absorbing of hydrogen • Parts of the universe that are dense will become more dense and vice versa • At some point it will become dense enough that stars will be able to form • Denser parts will be hotter in the nebula. You keep on sucking in matter and the parts become much more dense. • Universe is dominantly hydrogen and a little bit helium • Heating up as they become denser and then nuclear fusion can occur when it gets hot enough. Pulling a cloud in- temperatures increasing
More Less

Related notes for EPSC 201

Log In


OR

Join OneClass

Access over 10 million pages of study
documents for 1.3 million courses.

Sign up

Join to view


OR

By registering, I agree to the Terms and Privacy Policies
Already have an account?
Just a few more details

So we can recommend you notes for your school.

Reset Password

Please enter below the email address you registered with and we will send you a link to reset your password.

Add your courses

Get notes from the top students in your class.


Submit