Team L Supernovae Mark Blount Elizabeth Brooks Blaze Campbell Sonia Vazquez Yanet Zavala.
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Transcript of Team L Supernovae Mark Blount Elizabeth Brooks Blaze Campbell Sonia Vazquez Yanet Zavala.
![Page 1: Team L Supernovae Mark Blount Elizabeth Brooks Blaze Campbell Sonia Vazquez Yanet Zavala.](https://reader035.fdocuments.us/reader035/viewer/2022062518/56649eba5503460f94bc2293/html5/thumbnails/1.jpg)
Team L
SupernovaeMark Blount
Elizabeth BrooksBlaze CampbellSonia VazquezYanet Zavala
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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.
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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
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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
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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)
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Procedures Use DS9 computer program to analyze
SNR data
Load, select, and examine SNR using
DS9
Qualitative Analysis
Quantitative Analysis
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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
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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
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Cas A Tycho
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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
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QUESTIONS?
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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