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Office: LD 156-S, 278-9244
Class: IT 160, Monday and Wednesday from 12:00 - 1:15
Is the University open/closed today?
4 questions, multiple choice, review your notes from the past four lectures
Know the history of Foucault, Galileo, Kepler, Brahe, Copernicus
Know the numbers/info regarding galaxies, and stars in galaxies
Know the motion of Earth's path around Sun (ecliptic plane, perihelion = closest to the sun, etc.) and the seasons
Know about the Moon's motion around the Earth and the phases of the Moon
4 questions, multiple choice, review your notes from last week, know:
The metric prefix names for various powers of ten
Dividing two numbers and obtaining the "order of magnitude"
The number of stars in a galaxy and the number of stars in the observable universe
The speed-of-light in the metric units (3 x 10^8 meters/second)
I post this early, just to keep it on everybody's radar screen: 5 Bonus Points are available to all students if the following condition is met: 80% class participation in filling out the official IUPUI Online Course Evaluation (near the end of semester).
Syllabus (PDF). Please print and keep with your notes.
Master Schedule (PDF). Please print and keep with your notes.
These documents may be changed/updated during the semester. Please check that you have the latest versions.
A solar eclipse only occurs if the New Moon is about within half a degree of the ecliptic plane (defined by the orbit path of Earth as it travels around the Sun). The Moon's orbital path, around the Earth, is (unfortunately) inclined by about 5 degrees to the ecliptic. Thus, there are only two opportunities each moonth (punning) when the Moon passes through the ecliptic. These points are called the nodes (ascending, descending). The Moon passing through a node is not sufficient, it must pass through the node during the New Moon lunar phase.
About twice a year, during an approximately 45 day window (based upon the orbital speeds of the Earth and Moon), the New Moon is close enough to a node that a solar eclipse can occur. Further complicating the motion, the Moon's orbital plane precesses relative to the ecliptic. Hence, the nodes precess around the ecliptic, completing one rotation about every 18.6 years. In addition, because the Moon's path around Earth is elliptical, during many solar eclipses the angular diameter of the Moon is not large enough to fully cover the Sun. Only when the New Moon is near a node and near perigee (i.e. closest to the Earth), does totality occur. On average, it takes about 400 years for totality to occur again at the same geographical location.
Many thanks to Ryan Bertram, who introduced me to this YouTube video (courtesy of Rob Bryanton, Canadian author) that discusses the ten possible dimensions of our universe.
Many thanks to Tim McCormick, who introduced me to this webpage that models early solar system formation.
Department of Physics, IUPUI - Updated on Jan 16, 2019 at 2:15 PM EST