Purdue University QuarkNet Center
Submitted by kcecire
on Friday, June 7, 2013 - 10:48
The Purdue University QuarkNet Center is a group of physicists and teachers who work together to learn about particle physics and how to bring what they learn to the classroom. Mentors Matthew Jones, Daniela Bortoletto, and David Sederberg lead the group along with lead teacher Marla Glover. In spring 2013, the Purdue center sent a physicist, a teacher, and cosmic ray detectors high into the atmosphere in hot air balloons to record the changes in flux. The group is also active in masterclasses and Marla Glover is a QuarkNet LHC fellow.
The Purdue center works on cosmic rays and CMS data.
1. There are four types of seismic waves: P wave (longitudinal), S wave (transverse), Love wave, and Rayleigh waves. P and S waves are body waves and go through the Earth. P waves arrive first. Love and Rayleigh waves are surface waves, Love waves are transverse and the Rayleigh waves are the most complex and the slowest.
5. Seismic waves are measured using seismometers, which record vibrations in the ground. One method is to use a drum with a marker attached to a spring-mass system. To go more old school, the ancient Chinese used a urn with water, that would spill over the mouths of dragons surrounding the urn. The amount of water indicates the relative strength of th seismic event. A more modern and advanced seismometer which uses magnets and coils are currently used to measure seismic activity at LIGO.
1. P and S waves interior waves. P--longitudinal, S transverse
Raleigh is a surface wave---rolling action on the transverse wave
Love is a suface wave that slides parallel to the surface.
2. P penatrates through all layers of the earth. Refracting at various layers based on density and elascitiy of the medium.
S penatrate only mantel. Reflecting or being absorbed by the outer core. So there is a shadow portion of the earth that will not observe the S waves
Raleigh and Love are both surface waves. So only felt on the surface but propagation is still governed by density and elascitiy of crust and surface features.
Four teachers attended Purdue's 2015 summer workshop which was held June 23-26. Our lead teacher (Marla Glover) was joined by two new teachers and one returning for a second year. As we have typically done when working with new teachers, the workshop focused on introducing particle physics concepts and the study of cosmic rays using the QuarkNet cosmic ray detector. This year we explored some ideas associated with probability and statistics and how these concepts might be taught using measurements made with the cosmic ray detector to provide concrete examples. In additon, teachers explored the activities on which the MasterClass workshop for high school students are based. This year we did not visit Fermilab, but did tour the nuclear reactor on the Purdue campus and the tandem Van de Graaff accelerator facility at Purdue's PRIME lab.
In March, Purdue hosted a MasterClass workshop in which 4 students from 2 schools participated. In addition to the analysis of data from the CMS experiment, the students were given tours of the silicon detector assembly labs at Purdue, at which components for the upgraded CMS Forward Pixel Detector are being assembled. Later in the spring, lead teacher Marla Glover hosted an additional MasterClass activity at her school in which 12 students from her school shared their findings with students from France.
This summer, Purdue hosted five teachers from Central Indiana for four days, followed by a tour of Fermilab. Almost all the teachers this year were new to QuarkNet so the workshop emphasized a basic introduction to fundamental particle physics, particle accelerators and cosmic ray physics. The cosmic ray detectors were used to study coincidence rates under various conditions and these rates were compared with the rate that would have been expected from purely random coincidences in independent counters. In this way the participants were able to deduce the presence of both cosmic rays and extended air showers and to measure the speed of cosmic rays. This year, data was collected using both the software interface originally developed at Purdue and the version on which development has continued at Fermilab. We also went through the CMS MasterClass exercises to illustrate the activities their students would undertake in Spring 2015. This year, we were fortunate to be visited by Nate Unterman, a QuarkNet fellow from the UIC group who observed the use of the two software interfaces and presented the activities his students have undertaken with the cosmic ray detector at his school. We were also visited by Prof. Neeti Parashar from the Calumet campus of Purdue University, who is starting a new QuarkNet center there. On Friday, the group toured the D0 detector and the MINOS detector at Fermilab.
Geographical distribution of CMS E-Lab uploaded posters and a brief inquiry into the aforementioned distribution and its varied nuances.
Our group elected to re-evaluate the conclusions reached by a previous group regarding the mass of a J/Psi particle based on muon +/- and muon ++/-- decays. The previous group concluded that the mass was either 3.05 GeV based on muon +- or 2.48 GeV based on muon ++/-- decay. Our evaluation is attached: http://www.i2u2.org/elab/cms/posters/display.jsp?name=adasf.data
Poster: Dimuon Analysis
Poster: Calculating Muon Velocity
Our group discovered a poster which evaluated the mass of a J/Psi particle to be approximately 3.05 GeV/c2. While this agrees with the accepted value of the mass of a J/Psi particle, the graphical representation used to reach this conclusion left much to be desired. We will be re-evaluating the CERN data using a smaller bin width and including data from the MasterClass website.