Tuesday, September 11, 2012


Please comment with any topic ideas you have for SciMaTech meetings. This can be anything regarding Science, Math, or Technology, and is not limited to our normal formal symposium-style meetings, but is limited by resources and law.

Some presented:

  • Java
  • Paul Hewitt

As some of you know, last year SciMaTech sponsored several spring wind events, the topics of those being fractals, computer anatomy, and bridge building. These events are very fun and a good way to gain members  to attend our meetings and learn with us, but do take some time and preparation. If you have any ideas regarding to spring wind events, or you would like to run one for SciMaTech, please let us know. (Note: to appeal to the general public, these should probably be more interactive activities, although normal lectures are welcomed too)

Spring wind event ideas:
  • Catapults and Trebuchets

Thursday, August 30, 2012


Post comments here with any questions, comments, concerns, or otherwise involving this meeting. Discussion is encouraged, and how we learn more about the universe. Here are the notes on the subject, to remind you of what was gone over (or was supposed to have been).

Elementary Particles/Nucleosynthesis

Dark Energy/Dark Matter

Quantum effects when the universe was small lead to irregularties in the distribution of matter and energy in the cosmos. These irregularities, through gravitational interaction amongst themselves, coalesce into galaxies.
Spiral/Bar Galaxies
Have the most star formation.
Irregular Galaxies
Totally depends
Elliptical Galaxies
Oldest galaxies, usually the result of collisions between spiral/bar galaxies.
Dark matter
Most of the matter in a galaxy is invisible to our instruments, only detectable by its influence.

Stellar Evolution

Fusion, gravitational force of star’s mass overcome electromagnetic force of star’s electrons, forcing atomic nuclei together, fusing them.
Main Sequence
Stellar Classes
O, B, A, F, G, K, M, going from largest to smallest, and hottest to coolest.

O = ultraviolet, burn hydrogen very quickly, strong He, Si, O, N, C lines. 1/3,000,000, millions of times more powerful than sun.
B = blue, He, H, Mg, Si lines, 1/800
A = white, strong H lines, Fe, Mg, Si, Ca lines, 1/160, common in night sky
F = white/yellow, H and ionized metal lines (Ca). 1/33
G = yellow, like our sun. weak H lines, strong Ca lines. 1/16.
K = orange, almost no hydrogen, mostly metals. 1/8. Giants-dwarves.
M = red, no hydrogen. Most common main sequence stars. Red Giants.
Towards the end of their lives, stars will have burned most of their hydrogen and they will begin to collapse. At a certain pressure and temperature, the star will begin to fuse Helium, thus preventing further collapse. Helium only provides about a tenth of the energy of normal
Supernova/Hypernova - multiple types:
Type 1a: A white dwarf that accretes enough matter onto its surface that it exceeds the Chandrasekhar limit, or about 1.38 solar masses, and the white dwarf starts to collapse. This ignites carbon fusion in the white dwarf, which releases large amounts of energy, and it increases the luminosity of the white dwarf by a factor of billions.
Type 1b: Large stars that have shed most of their outer layers of hydrogen and their cores collapse, producing a supernova.
Type 1c: Same as 1b, except that it doesn’t show helium spectra either.
Type II: Traditional supernova. Large star, generally above 8 solar masses, finally runs out of fusion fuel, and its core catastrophically collapses into a neutron star or a black hole. This collapse stops very suddenly when the neutron star forms, causing massive rebound and supernova.
Pair-Instability: 130 solar masses to 250 solar masses, the gamma rays produced by the star are so energetic that when they interact with nuclei, they condense into a positron and an electron. This reduces the expansionary pressure, which causes the outer layers of the star to collapse, which makes even more energetic gamma rays, which results in more pair production, and the cycle continues until the entire star is blown apart, leaving nothing left.

Accretion of the Gas Disk around a star.
Types of planets
Terrestrial planets
silicon, oxygen, iron/nickel.
Jovian planets
hydrogen, helium, water, ammonia, hydocarbons

Stellar Evolution
Big Bang
Main Sequence
Proto Stars
Galactic formation
Death of Stars
White Dwarves
Black Dwarves
Black holes

Neutron Stars

End of the Universe.