Team L

SupernovaeMark Blount

Elizabeth BrooksBlaze CampbellSonia VazquezYanet Zavala

Goal To learn about stellar

evolution theory

To discover how elements spread across our galaxy after a supernova explosion.

To draw conclusions from supernova remnants that we studied, specifically Cassiopeia A (Cas A) and Tycho.

What is a supernova?

How are supernovae formed?

Stars make energy through fusion reactions in the core.

Internal structure has layers of chemicals like an onion.

Supernova explosion spreads the chemicals into space.

IntroductionSN 1987a - Type II

before supernova

supernova

Introduction Cont.

Why are supernovae remnants important?

The chemicals spread by SNRs are the building blocks of life anywhere in our universe.

Supernovae remnants Shells of gas that expand into space

Materials

DS9 computer program from NASA

Chandra X-ray Satellite archives

DS9 instruction handbook

Horizons Text book by: Michael

Seeds

Lecture Notes by M. Richards

NASA Chandra Education webpage

(http://chandra-ed.harvard.edu/activi

ties.html)

Procedures Use DS9 computer program to analyze

SNR data

Load, select, and examine SNR using

DS9

Qualitative Analysis

Quantitative Analysis

Procedures Cont. Calculate distance to supernova remnant

Use angular size of SNR and expansion speed over 10

years

Calculate date when supernova occurred

Calculate time that a knot takes to move a certain

distance

Determine size of remnant

Measure width of SNR in pixels and convert to light years

Calculate luminosity from flux

Examine radial intensity profile

Examine energy spectrum

24 dFL

Results

Cas A TychoDistance in light years (ly)

11,400 7,500

Date of explosion 1667 A.D. 1572 A.D.

Size of remnant6.16 pc18.57 ly

6.97 pc20.07 ly

Luminosity (ergs/sec) 4.54 x 1036 4.98 x 1036

Luminosity (Lsun) 1195 1311

Cas A Tycho

Conclusions Our results confirm the spread of the elements from a

supernova event.

Accuracy and precision play an important role in our

measurements and calculations because of the large

distances and small angles in astronomy.

Further Analysis

Long term monitoring of SNRs.

Determine rate of expansion

Detailed examination of the composition of

elements

QUESTIONS?

Thank you. . .

Dr. Daniel Larson, Dean of the Eberly College of Science

Dr. Mercedes Richards

Ms. Jody Markley

Ms. Annie Holmes

Mr. Craig Keiser

Ms. Skyra Blanchard

All UBMS Staff

This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory

Dr. W. Terrell Jones, Vice Provost for Educational Equity