ECONOMIC EVALUATION OF WET CORN GLUTEN FEED IN BEEF FEEDLOT FINISHING

An economic evaluation of wet corn gluten feed used in beef feedlot finishing was done. Data were from feeding trials at North Dakota State University. Four rations were analyzed at 0 percent, 28 percent, 56 percent, and 85 percent wet corn gluten based on dry matter intake. Data were entered into a computer model that integrated the feeding trial data with economic input and output prices. A typical feedlot example was used. Results indicated that the 56 percent ration was the most biologically efficient. A matrix of results can be shown for various corn prices, relative to wet corn gluten feed prices and quantities fed. Based on this study, wet corn gluten feed is priced competitively with other feed stuffs.wet corn gluten feed, feeding trials, feedlot, finishing, beef, economic analysis, North Dakota, Farm Management,

ULF waves in the solar wind as direct drivers of magnetospheric pulsations

[1] Global magnetospheric ULF pulsations with frequencies in the Pc 5 range (f = 1.7–6.7 mHz) and below have been observed for decades in space and on the Earth. Recent work has shown that in some cases these pulsations appear at discrete frequencies. Global cavity and waveguide modes have been offered as possible sources of such waves. In these models the magnetosphere is presumed to resonate globally at frequencies determined solely by its internal properties such as size, shape, field topology, mass density distribution, etc. We show in this work that upstream solar wind number density and dynamic pressure variations precede and drive compressional magnetic field variations at geosynchronous orbit. Furthermore, spectral analysis shows that wave power spectra in both the solar wind and magnetosphere contain peaks at the same discrete frequencies. Therefore, in contrast to the cavity mode hypothesis, we suggest that discrete ULF pulsations observed within the magnetosphere are at least sometimes directly driven by density oscillations present in the ambient solar wind. Finally, we comment on possible sources for such pulsations observed in the solar wind

LANDSAT range resource information system project, volume 1

There are no author-identified significant results in this report

Implementasi Peraturan Daerah Kota Kupang Nomor 15 Tahun 2011 Tentang Retribusi Pelayanan Parkir di Tepi Jalan Umum

Sehubungan dengan adanya perbedaan potensi parkir dengan realisasi penerimaan saat operasional dilapangan Penelitian ini dilaksanakan untuk menjawab pertanyaan; Bagaimanakah Kontribusi Retribusi Pelayanan Parkir di Tepi Jalan Umum dalam mendukung peningkatan Pendapatan Asli Daerah dalam 5 (lima) tahun terakhir, dan Faktor – Faktor apakah yang mempengaruhi rendahnya kontribusi Retribusi Pelayanan Parkir di Tepi Jalan Umum terhadap penerimaan Pendapatan Asli Daerah. Temuan penelitian menperlihatkan bahwa, data perkembangan kontribusi retribusi parkir di tepi jalan umum terhadap total penerimaan PAD, periode tahun 2009 sebesar 1,62 % dan menurun terus menjadi 1,52% tahun 2013. Penerimaan retribusi daerah, pada tahun 2009 sebesar 4,17 % dan menurun menjadi 3,08 % pada tahun 2013. Selanjutnya penerimaan retribusi jasa umum sebesar 1,66% tahun 2009 dan menurun hingga tahun 2012 dan tahun 2013 meningkat menjadi 1,70 %. Secara umum dapat disimpulkan bahwa, kontribusi retribusi parkir di tepi jalan umum belum menunjukkan peranan yang signifikan terhadap pembentukkan PAD Kota Kupang. Faktor – faktor yang menyebabkan kecilnya angka penerimaan retribusi parkir di tepi jalan umum adalah; Faktor sistem managemen penanganan parkir dan faktor sistem pemungutan retribusi parkir yang belum berjalan secara baik. Berdasarkan pendekatan ROCCIPI ditemukan perilaku bermasalah terjadi pada semua pemegang peran

Mathematical models for radiation transfer

A radiation transfer model was modified to include semitransparent and opaque layers as well as molecular constituents. An example of the use of the program and an analysis of the mathematical model are included

A statistical study of the global structure of the ring current

[1] In this paper we derive the average configuration of the ring current as a function of the state of the magnetosphere as indicated by the Dst index. We sort magnetic field data from the Combined Release and Radiation Effects Satellite (CRRES) by spatial location and by the Dst index in order to produce magnetic field maps. From these maps we calculate local current systems by taking the curl of the magnetic field. We find both the westward (outer) and the eastward (inner) components of the ring current. We find that the ring current intensity varies linearly with Dst as expected and that the ring current is asymmetric for all Dst values. The azimuthal peak of the ring current is located in the afternoon sector for quiet conditions and near midnight for disturbed conditions. The ring current also moves closer to the Earth during disturbed conditions. We attempt to recreate the Dst index by integrating the magnetic perturbations caused by the ring current. We find that we need to multiply our computed disturbance by a factor of 1.88 ± 0.27 and add an offset of 3.84 ± 4.33 nT in order to get optimal agreement with Dst. When taking into account a tail current contribution of roughly 25%, this agrees well with our expectation of a factor of 1.3 to 1.5 based on a partially conducting Earth. The offset that we have to add does not agree well with an expected offset of approximately 20 nT based on solar wind pressure

On the standing wave mode of giant pulsations

Both odd-mode and even-mode standing wave structures have been proposed for giant pulsations. Unless a conclusion is drawn on the field-aligned mode structure, little progress can be made in understanding the excitation mechanism of giant pulsations. In order to determine the standing wave mode, we have made a systematic survey of magnetic field data from the AMPTE CCE spacecraft and from ground stations located near the geomagnetic foot point of CCE. We selected time intervals when CCE was close to the magnetic equator and also magnetically close to Syowa and stations in Iceland, and when either transverse or compressional Pc 4 waves were observed at CCE. Magnetograms from the ground stations were then examined to determine if there was a giant pulsation in a given time interval. One giant pulsation was associated with a compressional wave, while no giant pulsation was observed in association with transverse wave events. The CCE magnetic field record for the giant pulsation exhibited a remarkable similarity to a giant pulsation observed from the ATS 6 geostationary satellite near the magnetic equator (Hillebrand et al., 1982). In agreement with Hillebrand et al., we conclude that the compressional nature of the giant pulsation is due to an odd-mode standing wave structure. This conclusion places a strong constraint on the generation mechanism of giant pulsations. In particular, if giant pulsations are excited through the drift bounce resonance of ions with standing Alfvén waves, ω - mωd = ±Nωb, where ω is the wave frequency, m is the azimuthal wave number, ωd is the ion drift frequency,N is an integer, and ωb is the ion bounce frequency, then the resonance must occur at an even N

A quantitative assessment of empirical magnetic field models at geosynchronous orbit during magnetic storms

[1] We evaluate the performance of recent empirical magnetic field models (Tsyganenko, 1996, 2002a, 2002b; Tsyganenko and Sitnov, 2005, hereafter referred to as T96, T02 and TS05, respectively) during magnetic storm times including both pre- and post-storm intervals. The model outputs are compared with GOES observations of the magnetic field at geosynchronous orbit. In the case of a major magnetic storm, the T96 and T02 models predict anomalously strong negative Bz at geostationary orbit on the nightside due to input values exceeding the model limits, whereas a comprehensive magnetic field data survey using GOES does not support that prediction. On the basis of additional comparisons using 52 storm events, we discuss the strengths and limitations of each model. Furthermore, we quantify the performance of individual models at predicting geostationary magnetic fields as a function of local time, Dst, and storm phase. Compared to the earlier models (T96 and T02), the most recent storm-time model (TS05) has the best overall performance across the entire range of local times, storm levels, and storm phases at geostationary orbit. The field residuals between TS05 and GOES are small (≤3 nT) compared to the intrinsic short time-scale magnetic variability of the geostationary environment even during non-storm conditions (∼24 nT). Finally, we demonstrate how field model errors may affect radiation belt studies when estimating electron phase space density