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Buckhannon, WV, United States

West Virginia Wesleyan College is a regionally accredited private, coeducational, liberal arts college in Buckhannon, West Virginia, United States. It has an enrollment of about 1,400 students from 35 U.S. states and 26 countries. The school was founded in 1890 by the West Virginia Conference of the United Methodist church. The college assumed its current name on Tuesday June 5, 1906 . U.S. News & World Report considers West Virginia Wesleyan a regional college and ranks it 12th in the South and ranks it second in the South in the "Great Schools at Great Prices" category. In 2014, U.S. News & World Report again ranked West Virginia Wesleyan College as a 1st Tier College, and 14th on the list of Best Colleges in the South. West Virginia Wesleyan College is accredited by the Commission on Institutions of Higher Education of the North Central Association of Colleges and Schools.Wesleyan was listed as one of the "Best Southeastern Colleges" by the Princeton Review in 2005, 2006, 2007, 2008, 2009, 2010, and 2011 and a "Best-Value College" in 2006 and 2007. Wesleyan is one of 150 schools to receive that distinction .Wesleyan continues to serve as a residential, liberal arts college. The primary majors are elementary and secondary education, business, and natural science. Wikipedia.

Delaney T.,West Virginia Wesleyan College | Kassim N.E.,U.S. Navy | Rudnick L.,University of Minnesota | Perley R.A.,U.S. National Radio Astronomy Observatory
Astrophysical Journal

Characterizing the ejecta in young supernova remnants is a requisite step toward a better understanding of stellar evolution. In Cassiopeia A the density and total mass remaining in the unshocked ejecta are important parameters for modeling its explosion and subsequent evolution. Low frequency (<100 MHz) radio observations of sufficient angular resolution offer a unique probe of unshocked ejecta revealed via free-free absorption against the synchrotron emitting shell. We have used the Very Large Array plus Pie Town Link extension to probe this cool, ionized absorber at 9″ and 18.″5 resolution at 74 MHz. Together with higher frequency data we estimate an electron density of 4.2 cm-3 and a total mass of 0.39 M with uncertainties of a factor of 2. This is a significant improvement over the 100 cm-3 upper limit offered by infrared [S III] line ratios from the Spitzer Space Telescope. Our estimates are sensitive to a number of factors including temperature and geometry. However using reasonable values for each, our unshocked mass estimate agrees with predictions from dynamical models. We also consider the presence, or absence, of cold iron- and carbon-rich ejecta and how these affect our calculations. Finally we reconcile the intrinsic absorption from unshocked ejecta with the turnover in Cas A's integrated spectrum documented decades ago at much lower frequencies. These and other recent observations below 100 MHz confirm that spatially resolved thermal absorption, when extended to lower frequencies and higher resolution, will offer a powerful new tool for low frequency astrophysics. © 2014. The American Astronomical Society. All rights reserved.. Source

Moore J.H.,West Virginia Wesleyan College
Proceedings of the Annual Hawaii International Conference on System Sciences

Technological advances, market shifts in the recording industry, and aesthetic elements have converged to make recording and releasing a self-produced album financially feasible for the independent jazz musician. A critical step in the process of completing such a project involves the utilization of one ore more e-government services offered by the U.S. Copyright Office and the Library of Congress. This observational value assessment compares and contrasts these services with similar and related e-services in the private sector. © 2015 IEEE. Source

Isensee K.,University of Minnesota | Olmschenk G.,University of Minnesota | Rudnick L.,University of Minnesota | Delaney T.,West Virginia Wesleyan College | And 5 more authors.
Astrophysical Journal

We present a three-dimensional analysis of the supernova remnant Cassiopeia A using high-resolution spectra from the Spitzer Space Telescope. We observe supernova ejecta both immediately before and during the shock-ejecta interaction. We determine that the reverse shock of the remnant is spherical to within 7%, although the center of this sphere is offset from the geometric center of the remnant by 810kms-1. We determine that the velocity width of the nucleosynthetic layers is 1000kms-1 over 4000 arcsec2 regions, although the velocity width of a layer along any individual line of sight is <250kms-1. Si and O, which come from different nucleosynthetic layers in the progenitor star, are observed to be coincident in velocity space in some directions, but segregated by up to 500kms-1 in other directions. We compare these observations of the nucleosynthetic layers to predictions from supernova explosion models in an attempt to constrain such models. Finally, we observe small-scale, corrugated velocity structures that are likely caused during the supernova explosion itself, rather than hundreds of years later by dynamical instabilities at the remnant's reverse shock. © 2012. The American Astronomical Society. All rights reserved. Source

Allen G.E.,Massachusetts Institute of Technology | Chow K.,Weston High School | Delaney T.,West Virginia Wesleyan College | Filipovic M.D.,University of Western Sydney | And 3 more authors.
Astrophysical Journal

An analysis of Chandra ACIS data for two relatively bright and narrow portions of the northwestern rim of G266.2-1.2 (a.k.a. RX J0852.0-4622 or Vela Jr.) reveal evidence of a radial displacement of 2.40 ± 0.56 arcsec between 2003 and 2008. The corresponding expansion rate (0.42 ± 0.10 arcsec yr-1 or 13.6% ± 4.2% kyr-1) is about half the rate reported for an analysis of XMM-Newton data from a similar, but not identical, portion of the rim over a similar, but not identical, time interval (0.84 ± 0.23 arcsec yr-1). If the Chandra rate is representative of the remnant as a whole, then the results of a hydrodynamic analysis suggest that G266.2-1.2 is between 2.4 and 5.1 kyr old if it is expanding into a uniform ambient medium (whether or not it was produced by a Type Ia or Type II event). If the remnant is expanding into the material shed by a steady stellar wind, then the age could be as much as 50% higher. The Chandra expansion rate and a requirement that the shock speed be greater than or equal to 1000 km s-1 yields a lower limit on the distance of 0.5 kpc. An analysis of previously published distance estimates and constraints suggests G266.2-1.2 is no further than 1.0 kpc. This range of distances is consistent with the distance to the nearer of two groups of material in the Vela Molecular Ridge (0.7 ± 0.2 kpc) and to the Vel OB1 association (0.8 kpc). © 2015. The American Astronomical Society. All rights reserved.. Source

DeLaney T.,West Virginia Wesleyan College | Rudnick L.,University of Minnesota | Stage M.D.,Mount Holyoke College | Smith J.D.,University of Toledo | And 8 more authors.
Astrophysical Journal

We used the Spitzer Space Telescope's Infrared Spectrograph to map nearly the entire extent of Cassiopeia A between 5 and 40μm. Using infrared and Chandra X-ray Doppler velocity measurements, along with the locations of optical ejecta beyond the forward shock, we constructed a three-dimensional model of the remnant. The structure of Cas A can be characterized into a spherical component, a tilted thick disk, and multiple ejecta jets/pistons and optical fast-moving knots all populating the thick disk plane. The Bright Ring in Cas A identifies the intersection between the thick plane/pistons and a roughly spherical reverse shock. The ejecta pistons indicate a radial velocity gradient in the explosion. Some ejecta pistons are bipolar with oppositely directed flows about the expansion center while some ejecta pistons show no such symmetry. Some ejecta pistons appear to maintain the integrity of the nuclear burning layers while others appear to have punched through the outer layers. The ejecta pistons indicate a radial velocity gradient in the explosion. In three dimensions, the Fe jet in the southeast occupies a "hole" in the Si-group emission and does not represent "overturning," as previously thought. Although interaction with the circumstellar medium affects the detailed appearance of the remnant and may affect the visibility of the southeast Fe jet, the bulk of the symmetries and asymmetries in Cas A are intrinsic to the explosion. © 2010. The American Astronomical Society. All rights reserved. Source

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