615 research outputs found
Importance of the code of ethics in the organization
Counteracting the unethical actions and influencing the behavior of the human factor towards ethical behavior must be a priority of a companyβs policy. The research and recommendations in this direction outline the necessity of an Ethic code that shall comprise individual and company values, and whose harmonious interaction shall provide stability and efficiency of the management process. This code shall serve as a balancing force among the various interests and systems of values, which shall thus establish common ethical standards of behavior.ΠΡΠΎΡΠΈΠ΄ΡΡ Π°Π½ΡΡΠ΅ΡΠΈΡΠ½ΠΈΠΌ Π΄ΡΡΠΌ ΠΈ Π²ΠΏΠ»ΠΈΠ² Π΅ΡΠΈΡΠ½ΠΎΡ ΠΏΠΎΠ²Π΅Π΄ΡΠ½ΠΊΠΈ Π½Π° ΠΏΠΎΠ²Π΅Π΄ΡΠ½ΠΊΡ Π»ΡΠ΄ΡΡΠΊΠΎΠ³ΠΎ ΡΠ°ΠΊΡΠΎΡΡ ΠΏΠΎΠ²ΠΈΠ½Π½Ρ Π±ΡΡΠΈ ΠΏΡΡΠΎΡΠΈΡΠ΅ΡΠΎΠΌ ΠΏΠΎΠ»ΡΡΠΈΠΊΠΈ ΠΊΠΎΠΌΠΏΠ°Π½ΡΡ. ΠΠΎΡΠ»ΡΠ΄ΠΆΠ΅Π½Π½Ρ ΡΠ° ΡΠ΅ΠΊΠΎΠΌΠ΅Π½Π΄Π°ΡΡΡ Π² ΡΡΠΎΠΌΡ Π½Π°ΠΏΡΡΠΌΠΊΡ Π΄ΠΎΠ·Π²ΠΎΠ»ΠΈΠ»ΠΈ Π½Π°ΠΌΡΡΠΈΡΠΈ Π½Π΅ΠΎΠ±Ρ
ΡΠ΄Π½ΡΡΡΡ Π² Π΅ΡΠΈΡΠ½ΠΎΠΌΡ ΠΊΠΎΠ΄Π΅ΠΊΡΡ, ΡΠΊΠΈΠΉ ΠΏΠΎΠ²ΠΈΠ½Π΅Π½ Π²ΠΊΠ»ΡΡΠ°ΡΠΈ ΡΠ½Π΄ΠΈΠ²ΡΠ΄ΡΠ°Π»ΡΠ½Ρ ΡΠ° ΠΎΡΠ³Π°Π½ΡΠ·Π°ΡΡΠΉΠ½Ρ ΡΡΠ½Π½ΠΎΡΡΡ, Ρ Π³Π°ΡΠΌΠΎΠ½ΡΡΠ½Ρ Π²Π·Π°ΡΠΌΠΎΠ΄ΡΡ, ΡΠΊΠ° Π·Π°Π±Π΅Π·ΠΏΠ΅ΡΡΡ ΡΡΠ°Π±ΡΠ»ΡΠ½ΡΡΡΡ Ρ Π΅ΡΠ΅ΠΊΡΠΈΠ²Π½ΡΡΡΡ ΠΏΡΠΎΡΠ΅ΡΡ ΡΠΏΡΠ°Π²Π»ΡΠ½Π½Ρ. Π¦Π΅ΠΉ ΠΊΠΎΠ΄Π΅ΠΊΡ Π±ΡΠ΄Π΅ Π²ΠΈΡΡΡΠΏΠ°ΡΠΈ Π² ΡΠΊΠΎΡΡΡ Π²ΡΡΠ²Π½ΠΎΠ²Π°ΠΆΡΡΡΠΎΡ ΡΠΈΠ»ΠΈ ΠΌΡΠΆ ΡΡΠ·Π½ΠΈΠΌΠΈ ΡΠ½ΡΠ΅ΡΠ΅ΡΠ°ΠΌΠΈ ΡΠ° ΡΠΈΡΡΠ΅ΠΌΠ°ΠΌΠΈ ΡΡΠ½Π½ΠΎΡΡΠ΅ΠΉ, ΡΠΊΡ Π²ΡΡΠ°Π½ΠΎΠ²Π»ΡΡΡΡ Π·Π°Π³Π°Π»ΡΠ½Ρ Π΅ΡΠΈΡΠ½Ρ Π½ΠΎΡΠΌΠΈ ΠΏΠΎΠ²Π΅Π΄ΡΠ½ΠΊΠΈ.ΠΡΠΎΡΠΈΠ²ΠΎΠ΄Π΅ΠΉΡΡΠ²ΠΈΠ΅ Π½Π΅ΡΡΠΈΡΠ½ΡΠΌ Π΄Π΅ΠΉΡΡΠ²ΠΈΡΠΌ ΠΈ Π²Π»ΠΈΡΠ½ΠΈΠ΅ ΡΡΠΈΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΠΏΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ Π½Π° ΠΏΠΎΠ²Π΅Π΄Π΅Π½ΠΈΠ΅ ΡΠ΅Π»ΠΎΠ²Π΅ΡΠ΅ΡΠΊΠΎΠ³ΠΎ ΡΠ°ΠΊΡΠΎΡΠ° Π΄ΠΎΠ»ΠΆΠ½Ρ Π±ΡΡΡ ΠΏΡΠΈΠΎΡΠΈΡΠ΅ΡΠΎΠΌ ΠΏΠΎΠ»ΠΈΡΠΈΠΊΠΈ ΠΊΠΎΠΌΠΏΠ°Π½ΠΈΠΈ. ΠΡΡΠ»Π΅Π΄ΠΎΠ²Π°Π½ΠΈΡ ΠΈ ΡΠ΅ΠΊΠΎΠΌΠ΅Π½Π΄Π°ΡΠΈΠΈ Π² ΡΡΠΎΠΌ Π½Π°ΠΏΡΠ°Π²Π»Π΅Π½ΠΈΠΈ ΠΏΠΎΠ·Π²ΠΎΠ»ΠΈΠ»ΠΈ Π½Π°ΠΌΠ΅ΡΠΈΡΡ Π½Π΅ΠΎΠ±Ρ
ΠΎΠ΄ΠΈΠΌΠΎΡΡΡ Π² ΡΡΠΈΡΠ΅ΡΠΊΠΎΠΌ ΠΊΠΎΠ΄Π΅ΠΊΡΠ΅, ΠΊΠΎΡΠΎΡΡΠΉ Π΄ΠΎΠ»ΠΆΠ΅Π½ Π²ΠΊΠ»ΡΡΠ°ΡΡ Π² ΡΠ΅Π±Ρ ΠΈΠ½Π΄ΠΈΠ²ΠΈΠ΄ΡΠ°Π»ΡΠ½ΡΠ΅ ΠΈ ΠΎΡΠ³Π°Π½ΠΈΠ·Π°ΡΠΈΠΎΠ½Π½ΡΠ΅ ΡΠ΅Π½Π½ΠΎΡΡΠΈ, ΠΈ Π³Π°ΡΠΌΠΎΠ½ΠΈΡΠ½ΠΎΠ΅ Π²Π·Π°ΠΈΠΌΠΎΠ΄Π΅ΠΉΡΡΠ²ΠΈΠ΅ ΠΎΠ±Π΅ΡΠΏΠ΅ΡΠΈΠ²Π°ΡΡΠ΅Π΅ ΡΡΠ°Π±ΠΈΠ»ΡΠ½ΠΎΡΡΡ ΠΈ ΡΡΡΠ΅ΠΊΡΠΈΠ²Π½ΠΎΡΡΡ ΠΏΡΠΎΡΠ΅ΡΡΠ°ΡΠΏΡΠ°Π²Π»Π΅Π½ΠΈΡ. ΠΡΠΎΡ ΠΊΠΎΠ΄Π΅ΠΊΡ Π±ΡΠ΄Π΅Ρ Π²ΡΡΡΡΠΏΠ°ΡΡ Π² ΠΊΠ°ΡΠ΅ΡΡΠ²Π΅ ΡΡΠ°Π²Π½ΠΎΠ²Π΅ΡΠΈΠ²Π°ΡΡΠ΅ΠΉ ΡΠΈΠ»Ρ ΠΌΠ΅ΠΆΠ΄Ρ ΡΠ°Π·Π»ΠΈΡΠ½ΡΠΌΠΈ ΠΈΠ½ΡΠ΅ΡΠ΅ΡΠ°ΠΌΠΈ ΠΈ ΡΠΈΡΡΠ΅ΠΌΠ°ΠΌΠΈ ΡΠ΅Π½Π½ΠΎΡΡΠ΅ΠΉ, ΠΊΠΎΡΠΎΡΡΠ΅ Π΄ΠΎΠ»ΠΆΠ½Ρ, ΡΠ°ΠΊΠΈΠΌ ΠΎΠ±ΡΠ°Π·ΠΎΠΌ, ΡΡΡΠ°Π½ΠΎΠ²ΠΈΡΡ ΠΎΠ±ΡΠΈΠ΅ ΡΡΠΈΡΠ΅ΡΠΊΠΈΠ΅ Π½ΠΎΡΠΌΡ ΠΏΠΎΠ²Π΅Π΄Π΅Π½ΠΈΡ
Simulations of inner magnetosphere dynamics with an expanded RAM-SCB model and comparisons with Van Allen Probes observations
Abstract Simulations from our newly expanded ring current-atmosphere interactions model with self-consistent magnetic field (RAM-SCB), now valid out to 9 R E, are compared for the first time with Van Allen Probes observations. The expanded model reproduces the storm time ring current buildup due to the increased convection and inflow of plasma from the magnetotail. It matches Magnetic Electron Ion Spectrometer (MagEIS) observations of the trapped high-energy (\u3e50 keV) ion flux; however, it underestimates the low-energy (\u3c10 keV) Helium, Oxygen, Proton, and Electron (HOPE) observations. The dispersed injections of ring current ions observed with the Energetic particle, Composition, and Thermal plasma (ECT) suite at high (\u3e20 keV) energy are better reproduced using a high-resolution convection model. In agreement with Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) observations, RAM-SCB indicates that the large-scale magnetic field is depressed as close as βΌ4.5 RE during even a moderate storm. Regions of electromagnetic ion cyclotron instability are predicted on the duskside from βΌ6 to βΌ9 RE, indicating that previous studies confined to geosynchronous orbit may have underestimated their scattering effect on the energetic particles. Key Points Expanded RAM-SCB model reproduces well high-energy (\u3e50 keV) MagEIS observations The magnetic field is depressed as close as βΌ4.5 RE during even a moderate storm EMIC wave growth extends on duskside from βΌ6 to βΌ9 RE during storm main phase
Application and testing of the L neural network with the self-consistent magnetic field model of RAM-SCB
Abstract We expanded our previous work on L neural networks that used empirical magnetic field models as the underlying models by applying and extending our technique to drift shells calculated from a physics-based magnetic field model. While empirical magnetic field models represent an average, statistical magnetospheric state, the RAM-SCB model, a first-principles magnetically self-consistent code, computes magnetic fields based on fundamental equations of plasma physics. Unlike the previous L neural networks that include McIlwain L and mirror point magnetic field as part of the inputs, the new L neural network only requires solar wind conditions and the Dst index, allowing for an easier preparation of input parameters. This new neural network is compared against those previously trained networks and validated by the tracing method in the International Radiation Belt Environment Modeling (IRBEM) library. The accuracy of all L neural networks with different underlying magnetic field models is evaluated by applying the electron phase space density (PSD)-matching technique derived from the Liouville\u27s theorem to the Van Allen Probes observations. Results indicate that the uncertainty in the predicted L is statistically (75%) below 0.7 with a median value mostly below 0.2 and the median absolute deviation around 0.15, regardless of the underlying magnetic field model. We found that such an uncertainty in the calculated L value can shift the peak location of electron phase space density (PSD) profile by 0.2 RE radially but with its shape nearly preserved. Key Points L* neural network based on RAM-SCB model is developed L* calculation accuracy is estimated by PSD matching using RBSP data L* uncertainty causes a radial shift in the electron phase space density profile
Global, collisional model of highβenergy photoelectrons
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95539/1/grl8976.pd
A bounceβaveraged kinetic model of the ring current ion population
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94668/1/grl7966.pd
Energy Content of the Stormtime Ring Current
Given the important role the ring current plays in magnetospheric energetics, it is essential to understand its strength and evolution in disturbed times. There are currently three main methods for deducing the strength of the ring current: measuring ground magnetic perturbations, measuring high-altitude magnetic perturbations, or directly measuring ring current particles. The use of ground magnetometers is the most convenient, and many use the ground magnetometer-derived Dst index as a proxy for the ring current. Recent work suggests, however, that a substantial portion of Dst may not be caused only by the ring current but also by local induction effects or other magnetospheric currents, so simply using the Dst index may yield inaccurate results. This study uses direct particle measurements to calculate the strength of the ring current and compares this to the measured Dst values. We investigate several magnetic storm intervals, using the Polar Charge and Mass Magnetospheric Ion Composition Experiment (CAMMICE) to measure ring current ions. We then use the Dessler-Parker-Sckopke relation to compare this to the measured Dst. This analysis is used both to understand the general behavior of the ring current compared to Dst as well as to compare the usefulness of the Dst proxy for different types of storms. Ring current ions are shown in this analysis to contribute, on average, half of the Dst depression, with a large variation among individual events
Excitation of EMIC waves detected by the Van Allen Probes on 28 April 2013
Abstract We report the wave observations, associated plasma measurements, and linear theory testing of electromagnetic ion cyclotron (EMIC) wave events observed by the Van Allen Probes on 28 April 2013. The wave events are detected in their generation regions as three individual events in two consecutive orbits of Van Allen Probe-A, while the other spacecraft, B, does not detect any significant EMIC wave activity during this period. Three overlapping H+ populations are observed around the plasmapause when the waves are excited. The difference between the observational EMIC wave growth parameter (Eh) and the theoretical EMIC instability parameter (Sh) is significantly raised, on average, to 0.10 Β± 0.01, 0.15 Β± 0.02, and 0.07 Β± 0.02 during the three wave events, respectively. On Van Allen Probe-B, this difference never exceeds 0. Compared to linear theory (Eh\u3eSh), the waves are only excited for elevated thresholds
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