Genealogical Plagiarism and the Library Community

Plagiarism is regarded as an academic crime, but can affect hobbies that rely on research and information sharing such as genealogy. The issue is well-known within the genealogy community. However, information professionals who aid genealogists in their research may not know enough about the issue. How can the library field respond constructively to the issue of uncontrolled plagiarism in genealogy? While the genealogy community condemns plagiarism and offers resources to correct it, current library practices concentrate on services and not on plagiarism education in the genealogy context, concentrating more on copyright and legal problems. The library field can help professionals respond to uncontrolled plagiarism in genealogy by studying the issue. Recommendations for further action include more research on the information-seeking behaviors of genealogists, training information professionals to give both copyright and plagiarism attention and an increase in workshops to educate genealogists on citation

Monte Carlo Neutrino Transport Through Remnant Disks from Neutron Star Mergers

We present Sedonu, a new open source, steady-state, special relativistic Monte Carlo (MC) neutrino transport code, available at bitbucket.org/srichers/sedonu. The code calculates the energy- and angle-dependent neutrino distribution function on fluid backgrounds of any number of spatial dimensions, calculates the rates of change of fluid internal energy and electron fraction, and solves for the equilibrium fluid temperature and electron fraction. We apply this method to snapshots from two-dimensional simulations of accretion disks left behind by binary neutron star mergers, varying the input physics and comparing to the results obtained with a leakage scheme for the case of a central black hole and a central hypermassive neutron star. Neutrinos are guided away from the densest regions of the disk and escape preferentially around 45 degrees from the equatorial plane. Neutrino heating is strengthened by MC transport a few scale heights above the disk midplane near the innermost stable circular orbit, potentially leading to a stronger neutrino-driven wind. Neutrino cooling in the dense midplane of the disk is stronger when using MC transport, leading to a globally higher cooling rate by a factor of a few and a larger leptonization rate by an order of magnitude. We calculate neutrino pair annihilation rates and estimate that an energy of 2.8e46 erg is deposited within 45 degrees of the symmetry axis over 300 ms when a central BH is present. Similarly, 1.9e48 erg is deposited over 3 s when an HMNS sits at the center, but neither estimate is likely to be sufficient to drive a GRB jet.Comment: 23 pages, 16 figures, Accepted to The Astrophysical Journa

Fast Flavor Transformations

The neutrino fast flavor instability (FFI) can change neutrino flavor on timescales of nanoseconds and length scales of centimeters. It is expected to beubiquitous in core-collapse supernovae and neutron star mergers, potentiallymodifying the neutrino signal we see, how matter is ejected from theseexplosions, and the types of heavy elements that form in the ejecta and enrichthe universe. There has been a great deal of recent interest in understandingthe role the FFI plays in supernovae and mergers, but the short length and timescales and the strong nonlinearity have prevented the FFI from being includedconsistently in these models. We review the theoretical nature of the FFIstarting with the quantum kinetic equations, where the instability exists inneutron star mergers and supernovae, and how the instability behaves aftersaturation in simplified simulations. We review the proposed methods to testfor instability in moment-based calculations where the full distribution is notavailable and describe the numerical methods used to simulate the instabilitydirectly. Finally, we close by outlining the trajectory toward realistic,self-consistent models that will allow a more complete understanding of theimpact of the FFI in supernovae and mergers.<br

Fast Flavor Transformations

The neutrino fast flavor instability (FFI) can change neutrino flavor on timescales of nanoseconds and length scales of centimeters. It is expected to beubiquitous in core-collapse supernovae and neutron star mergers, potentiallymodifying the neutrino signal we see, how matter is ejected from theseexplosions, and the types of heavy elements that form in the ejecta and enrichthe universe. There has been a great deal of recent interest in understandingthe role the FFI plays in supernovae and mergers, but the short length and timescales and the strong nonlinearity have prevented the FFI from being includedconsistently in these models. We review the theoretical nature of the FFIstarting with the quantum kinetic equations, where the instability exists inneutron star mergers and supernovae, and how the instability behaves aftersaturation in simplified simulations. We review the proposed methods to testfor instability in moment-based calculations where the full distribution is notavailable and describe the numerical methods used to simulate the instabilitydirectly. Finally, we close by outlining the trajectory toward realistic,self-consistent models that will allow a more complete understanding of theimpact of the FFI in supernovae and mergers.<br

Neutron to proton ratios of quasiprojectile and midrapidity emission in the 64^{64}Zn + 64^{64}Zn reaction at 45 MeV/nucleon

Simultaneous measurement of both neutrons and charged particles emitted in the reaction $^{64}$Zn + $^{64}$Zn at 45 MeV/nucleon allows comparison of the neutron to proton ratio at midrapidity with that at projectile rapidity. The evolution of N/Z in both rapidity regimes with increasing centrality is examined. For the completely re-constructed midrapidity material one finds that the neutron-to-proton ratio is above that of the overall $^{64}$Zn + $^{64}$Zn system. In contrast, the re-constructed ratio for the quasiprojectile is below that of the overall system. This difference provides the most complete evidence to date of neutron enrichment of midrapidity nuclear matter at the expense of the quasiprojectile

Dual-frequency VLBI study of Centaurus A on sub-parsec scales

Centaurus A is the closest active galactic nucleus. High resolution imaging using Very Long Baseline Interferometry (VLBI) enables us to study the spectral and kinematic behavior of the radio jet-counterjet system on sub-parsec scales, providing essential information for jet emission and formation models. Our aim is to study the structure and spectral shape of the emission from the central-parsec region of Cen A. As a target of the Southern Hemisphere VLBI monitoring program TANAMI (Tracking Active Galactic Nuclei with Milliarcsecond Interferometry), VLBI observations of Cen A are made regularly at 8.4 and 22.3 GHz with the Australian Long Baseline Array (LBA) and associated telescopes in Antarctica, Chile, and South Africa. The first dual-frequency images of this source are presented along with the resulting spectral index map. An angular resolution of 0.4 mas x 0.7 mas is achieved at 8.4 GHz, corresponding to a linear scale of less than 0.013 pc. Hence, we obtain the highest resolution VLBI image of Cen A, comparable to previous space-VLBI observations. By combining with the 22.3 GHz image, which has been taken without contributing transoceanic baselines at somewhat lower resolution, we present the corresponding dual-frequency spectral index distribution along the sub-parsec scale jet revealing the putative emission regions for recently detected gamma-rays from the core region by Fermi/LAT. We resolve the innermost structure of the milliarcsecond scale jet and counterjet system of Cen A into discrete components. The simultaneous observations at two frequencies provide the highest resolved spectral index map of an AGN jet allowing us to identify multiple possible sites as the origin of the high energy emission.Comment: 5 pages, 3 figures (1 color); A&A, accepte