Localization of sources with a frequency-hopped signaling sensor array

In this paper, we present a different approach to the problem of estimating the angle of arrivals (AOA's) of D targets in Frequency - Hopped signaling sensors array for active systems, with D smaller than the number of sensor elements, L . This method is based on the application of the Maximum Likelihood Estimator for a new proposed model of received data available in different channels . The simulation results show that this approach improves the resolution in the estimation of the angle of arrivals compared wit h Monotone-Frequency signaling case. Its drawback, however, is that when the Signal-to-Noise Ratio, SNR, is low the performanc e deteriorates and a large number of snapshots is required .Dans cet article, nous présentons une méthode pour la résolution du problème d'estimation des angles d'arrivée de D cibles, par un réseau de L capteurs, où D < L, pour les systèmes actifs émettant des signaux codés en « Frequency Hopped ». Cette méthode est basée sur l'application de l'estimateur du maximum de vraisemblance à un nouveau modèle de données reçues sur différents canaux. Les résultats de simulation montrent que cette approche améliore la résolution des angles d'arrivée des cibles, comparativement à celle de la fréquence monotone. Cependant, quand le rapport signal sur bruit (Signal to Noise Ratio, SNR) est faible, la performance se dégrade et nécessite donc un nombre d'échantillons plus élevé

Carbon-poor stellar cores as supernova progenitors

Exploring stellar models which ignite carbon off-center (in the mass range of about 1.05 - 1.25 Msun, depending on the carbon mass fraction) we find that they may present an interesting SN I progenitor scenario, since whereas in the standard scenario runaway always takes place at the same density of about 2 X 10^9 gr/cm^3, in our case, due to the small amount of carbon ignited, we get a whole range of densities from 1 X 10^9 up to 6 X 10^9 gr/cm^3. These results could contribute in resolving the emerging recognition that at least some diversity among SNe I exists, since runaway at various central densities is expected to yield various outcomes in terms of the velocities and composition of the ejecta, which should be modeled and compared to observations.Comment: 49 pages, 20 figure

Nucleosynthesis in Type II Supernovae

Presupernova evolution and explosive nucleosynthesis in massive stars for main-sequence masses from 13 $M_\odot$ to 70 $M_\odot$ are calculated. We examine the dependence of the supernova yields on the stellar mass, ^{12}C(\alpha, \gamma) ^{16}O} rate, and explosion energy. The supernova yields integrated over the initial mass function are compared with the solar abundances.Comment: 1 Page Latex source, 10 PostScript figures, to appear in Nuclear Physics A, Vol. A616 (1997

A critical period for auditory thalamocortical connectivity.

1 1 8 9 a r t I C l e S Neural circuits are shaped by experience during periods of heightened brain plasticity in early life 1,2 . Children raised in an English-speaking environment easily distinguish between the phonemes /la/ and /ra/, whereas those growing up in Japan find it increasingly difficult 3 . Passive exposure of young rodents to a variety of sound features reveals a cascading series of developmental windows that open and close shortly after hearing onset to define the persistent and specific influences of early experience on the functional organization of auditory cortex Motivated by the well known binocular interactions shaped by experience in developing visual cortex 7-9 , we used in vivo neurophysiological recordings to determine whether mouse A1 also exhibits a critical period for tonotopic map plasticity induced through passive tone exposure, and whether such plasticity is present in the auditory thalamus (ventral medial geniculate body, MGBv). We then isolated the connection between MGBv and primary auditory cortex (A1) (ref. 10) in an acute brain slice preparation 11 and used voltage-sensitive dye imaging (VSDI) techniques in vitro. We mapped A1 responses to electrical stimulation of discrete sites in MGBv across early postnatal days (P8-20), following tone-rearing or gene manipulation. Our results reveal a critical period for acoustically driven topographic plasticity at thalamocortical connections in mouse A1. RESULTS Tone exposure modifies tonotopic maps in A1, but not MGBv The auditory system is tonotopically organized 10 such that tones of similar frequency activate neighboring neurons at each station along the pathway. Given that rats show experience-dependent tonotopic map reorganization following passive tone exposure during the second postnatal week 2,12 , we first used high-density in vivo mapping to delineate A1 tonotopy in young adult mice 13 that were reared either in typical acoustic environments To determine whether remapping in A1 could be explained by a shifted frequency representation in the principal subcortical input source, we also examined best frequency distributions in the MGBv. We inserted a multichannel silicon probe at an angle that matched the plane of section used in subsequent thalamocortical slice experiment

First Steps Towards Gamification Of Online Physics And Mathematics Assignments

The objective of this practice paper is to describe and analyse the use of online learning tasks on engineering mathematics and physics courses. The development of learning tasks was inspired by the promising effects of gamification techniques in higher education. Hence, some gamification elements, such as bonus points and immediate feedback were integrated into the learning tasks. Course results and student feedback demonstrate the positive impact of gamification of online learning tasks on students’ motivation and learning. In the end, further possibilities of increasing the number and repertoire of gamification techniques in engineering mathematics and physics courses are discussed

High Latitude Radio Emission in a Sample of Edge-On Spiral Galaxies

We have mapped 16 edge-on galaxies at 20 cm using the VLA. For 5 galaxies, we could form spectral index, energy and magnetic field maps. We find that all but one galaxy show evidence for non-thermal high latitude radio continuum emission, suggesting that cosmic ray halos are common in star forming galaxies. The high latitude emission is seen over a variety of spatial scales and in discrete and/or smooth features. In general, the discrete features emanate from the disk, but estimates of CR diffusion lengths suggest that diffusion alone is insufficient to transport the particles to the high latitudes seen (> 15 kpc in one case). Thus CRs likely diffuse through low density regions and/or are assisted by other mechanisms (e.g. winds). We searched for correlations between the prevalence of high latitude radio emission and a number of other properties, including the global SFR, supernova input rate per unit star forming, and do not find clear correlations with any of these properties.Comment: 40 pages of text, 3 figures, 6 tables, and an appendix of 21 jpeg figures (which is a radio continuum catalogue of 17 galaxies). to appear in A. J. (around January 1999

Red Wolf Multispecies Justice Publication 2023

Our understanding of multispecies justice is still solidifying. In spring 2023, a group of Utah State University undergraduate and graduate students attended a course by Dr.Kirsten Vinyeta on Multispecies Justice and Indigenous Approaches to the Environment. Throughout this course, we studied the works of scholars and writers from a variety of social locations and identities who challenge Western theoretical frameworks in social science. This publication celebrates our intellectual struggle with this emerging field and opens a forum for conversations about justice for humans and additional species. This issue features various writings, reflections, and photos from students taking the Multispecies Justice and Indigenous Approaches to the Environment course. Children of students and faculty also contributed artwork with multispecies elements. We would like to thank all contributors for making this publication possible. We thank Dr. Jessica Schad for her wise guidance. Our special thanks to the Community and Natural Resources Institute (CANRI) for funding the publication of this booklet

First Stars. I. Evolution without mass loss

The first generation of stars was formed from primordial gas. Numerical simulations suggest that the first stars were predominantly very massive, with typical masses M > 100 Mo. These stars were responsible for the reionization of the universe, the initial enrichment of the intergalactic medium with heavy elements, and other cosmological consequences. In this work, we study the structure of Zero Age Main Sequence stars for a wide mass and metallicity range and the evolution of 100, 150, 200, 250 and 300 Mo galactic and pregalactic Pop III very massive stars without mass loss, with metallicity Z=10E-6 and 10E-9, respectively. Using a stellar evolution code, a system of 10 equations together with boundary conditions are solved simultaneously. For the change of chemical composition, which determines the evolution of a star, a diffusion treatment for convection and semiconvection is used. A set of 30 nuclear reactions are solved simultaneously with the stellar structure and evolution equations. Several results on the main sequence, and during the hydrogen and helium burning phases, are described. Low metallicity massive stars are hotter and more compact and luminous than their metal enriched counterparts. Due to their high temperatures, pregalactic stars activate sooner the triple alpha reaction self-producing their own heavy elements. Both galactic and pregalactic stars are radiation pressure dominated and evolve below the Eddington luminosity limit with short lifetimes. The physical characteristics of the first stars have an important influence in predictions of the ionizing photon yields from the first luminous objects; also they develop large convective cores with important helium core masses which are important for explosion calculations.Comment: 17 pages, 24 figures, 2 table

Formation of Supermassive Black Holes

Evidence shows that massive black holes reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than the host (~ 0.1%), are linked to the evolution of galactic structure. In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation had to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for `seed' black holes that are likely to place at early cosmic epochs, and possible observational tests of these scenarios.Comment: To appear in The Astronomy and Astrophysics Review. The final publication is available at http://www.springerlink.co