Intranetwork Research Articles

Employee‘s Satisfaction within the Context of an Organization’s Development: Study Results

Purpose: The study's main objective was to assess employee satisfaction at the University of Technology and Life Sciences in Bydgoszcz. Specific objectives included areas of employee satisfaction, assessing the opportunities for professional development, job motivation, and satisfaction, the opinions on the changes necessary to be undertaken at the University to improve job satisfaction. Design/Methodology/Approach: The evaluation study was conducted using a survey questionnaire, which was distributed to the employees using an electronic questionnaire via the Limesurvey system, a traditional paper questionnaire, available at the University's lodges, and in a downloadable version available via the INTRA network. Conclusions: The study showed that the respondents are satisfied, among others, with their professional development at the University, the possibility of using their abilities or competencies, and their achievements. Practical implications: The study also showed that the respondents are satisfied with the opportunity to acquire knowledge, new skills, and self-fulfillment. In this group of questions, the university employees surveyed rate employment stability the lowest. It is insufficient for 22.32% of the respondents, while for 22.03%, it is sufficient. Originality/value Satisfaction testing is a valuable tool for streamlining the organization and increasing employee satisfaction.

Employee satisfaction within the context of an organization’s development – study results

Purpose: The main objective of the study was to assess employee satisfaction at the University of Technology and Life Sciences in Bydgoszcz. Specific objectives included areas of employee satisfaction, with regard to the assessment of the opportunities for professional development, job motivation and satisfaction, the opinions on the changes necessary to be undertaken at the University to improve job satisfaction. Design/methodology/approach: The evaluation study was conducted using a survey questionnaire, which was distributed to the employees by the means of an electronic questionnaire via the Limesurvey system, a traditional paper questionnaire, available at the University's lodges, and in a downloadable version available via the INTRA network. Findings: The study showed that the respondents are satisfied, among others, with their professional development at the university, the possibility of using their abilities or competences, and their achievements. Practical implications: The study also showed that the respondents are satisfied with the opportunity to acquire knowledge, new skills and self-fulfillment. In this group of questions, the university employees surveyed rate employment stability the lowest. For 22.32% of the respondents it is insufficient while for 22.03% it is sufficient. Originality/value Satisfaction testing is a useful tool for streamlining organization and increasing employee satisfaction.

Central Executive and Default Mode Network Intranet work Functional Connectivity Patterns in Chronic Migraine.

Background:The neural mechanisms of chronic migraine remain largely unknown but linked to the decreased connectivity to intrinsic brain networks.Objective:To characterize the intranetwork functional connectivity within the Central Executive Network (CEN) and Default Mode Network (DMN) in chronic migraine (CM), with and without medication overuse headache (MOH).Methods:Using functional magnetic resonance imaging, we performed post-hoc analysis of a total of 136 pairs of nodes to node functional connectivity (NTNC) within the CEN and 6 pairs of NTNC within the DMN in CM (n=13) and CMMOH (n=16) as compared to controls, and between these two subgroups.Results:Connectivity between right ventrolateral prefrontal cortex (PFC) to contralateral anterior thalamus and connectivity between left dorsal PFC/frontal eye field (FEF) to dorsomedial PFC were decreased within the CEN in both CM and CMMOH subgroups. In the CEN, there was more widespread disruption in the CMMOH (n=16) versus CM (n=13), when compared to healthy controls. Within the subgroups, connectivity between right inferior frontal gyrus to left dorsolateral PFC was decreased in CMMOH compared to CM. In the DMN, only one NTNC (left lateral parietal to precuneus/PCC) was disrupted in the CMMOH group when compared to controls.Conclusion:There are similar patterns of NTNC dysfunction within CEN in CM regardless of MOH status. We observed more extensive intranetwork disruption in CMMOH than CM. The decreased coherence between the right inferior frontal gyrus and the left dorsolateral PFC in CMMOH is likely associated with a significant disruption in the inhibitory control and a maladaptive response in risk aversion and reward; whereas the decreased coherence between right dorsolateral and ventrolateral PFC to contralateral dorsal PFC/FEF may be related to lack of cognitive control and top-down regulation of pain in both CM and CMMOH.

Tumores del sistema nervioso central en población pediátrica entre 0 y 14 años

Introducción: Los tumores pediátricos primarios del sistema nervioso central (SNC), ocupan el segundo lugar en frecuencia, superados solamente por las neoplasias hematológicas. Objetivo: Realizar una revisión y análisis de la literatura médica existente sobre tumores del SNC en población entre los 0 y 14 años centrado en la epidemiologia, factores etiológicos, manifestaciones clínicas y diagnóstico. Metodología: Se realizó una búsqueda en las bases de datos PubMed, MedlinePlus, BIREME y red interna de trabajos de grados y tesis de la Universidad Industrial de Santander. Además, se realizó revisión de las páginas de los entes gubernamentales encargados del registro epidemiológico sobre cáncer nacional e internacional. Resultados: Los tumores de SNC en la población pediátrica son la segunda causa de muerte infantil solo superado por la leucemia; tienen una clínica y factores etiológicos bien establecidos. La epidemiología no difiere en el mundo. Los síntomas más frecuentes son vómito, cefalea, ataxia, síntomas visuales y alteraciones motoras. Los factores etiológicos más representativos son virus, síndromes genéticos, infecciones maternas y perinatales, exposición a radiación electromagnética e ionizante; algunos son muy discutidos como la presencia de trauma al momento del nacimiento. Además, existen documentados factores protectores tales como consumo de antioxidantes, frutas y verduras, e historia reportada de alergias. Conclusiones: El adecuado entrenamiento a los médicos de atención primaria en la identificación de los signos y síntomas para la sospecha y diagnóstico de los estadios iniciales de estos tumores pueden disminuir los índices de mortalidad. [Nieves-Cuervo GM, Manrique-Hernández EF, Ojeda-Rincón SA, Galvis-Pabón S. Tumores del sistema nervioso central en población pediátrica entre 0 y 14 años. MedUNAB 2016; 19 (2): 124-133]

Relation between trees of fragmenting granules and supergranulation evolution

Context: The determination of the underlying mechanisms of the magnetic elements diffusion over the solar surface is still a challenge. Understanding the formation and evolution of the solar network (NE) is a challenge, because it provides a magnetic flux over the solar surface comparable to the flux of active regions at solar maximum. Aims: We investigate the structure and evolution of interior cells of solar supergranulation. From Hinode observations, we explore the motions on solar surface at high spatial and temporal resolution. We derive the main organization of the flows inside supergranules and their effect on the magnetic elements. Method: To probe the superganule interior cell, we used the Trees of Fragmenting Granules (TFG) evolution and their relations to horizontal Results: Evolution of TFG and their mutual interactions result in cumulative effects able to build horizontal coherent flows with longer lifetime than granulation (1 to 2 hours) over a scale up to 12\arcsec. These flows clearly act on the diffusion of the intranetwork (IN) magnetic elements and also on the location and shape of the network. Conclusions: From our analysis during 24 hours, TFG appear as one of the major elements of the supergranules which diffuse and advect the magnetic field on the Sun's surface. The strongest supergranules contribute the most to magnetic flux diffusion in the solar photosphere.

Solar Intranetwork Magnetic Elements: Flux Distributions

The current study aims at quantifying the flux distributions of solar intranetwork (IN) magnetic field based on the data taken in four quiet and two enhanced network areas with the Narrow-band Filter Imager of the Solar Optical Telescope on board the Hinode satellite. More than 14000 IN elements and 3000 NT elements were visually identified. They exhibit a flux distribution function with a peak at 1 – 3×1016 Mx (maxwell) and 2 – 3×1017 Mx, respectively. We found that the IN elements contribute approximately to 52 % of the total flux and an average flux density of 12.4 gauss of the quiet region at any given time. By taking the lifetime of IN elements of about 3 min (Zhou et al., Solar Phys.267, 63, 2010) into account, the IN fields are estimated to have total contributions to the solar magnetic flux up to 3.8×1026 Mx per day. No fundamental distinction can be identified in IN fields between the quiet and enhanced network areas.

Solar Intranetwork Magnetic Elements: Intrinsically Weak or Strong?

The high spatial resolution observation of a quiet region taken with the Solar Optical Telescope/Spectro-Polarimeter aboard the Hinode spacecraft is analyzed. Based on the Milne–Eddington atmospheric model, the vector magnetic field of the quiet region is derived by fitting the full Stokes profiles of the Fe i 630 nm line pair. We extract intranetwork (IN) region from the quiet region and identify 5058 IN magnetic elements, and study their magnetic properties. As a comparison, the magnetic properties of network (NT) region are also analyzed. The main results are as follows. i) The IN area displays a predominance of weak (hecto-gauss) field concentration, i.e., 99.8 % of IN area shows the weak field. Moreover, the vector magnetic field exhibits concentration toward horizontal direction. However, for the NT region, we discover the coexistence of weak field and strong (kilo-gauss, kG) field. In the IN and NT regions, the filling factor shows almost the same probability distribution function with the peak at about 0.28. ii) All IN magnetic elements show field strength less than 1 kG. However, some NT elements display the coexistence of weak field and strong field. Regardless of NT or IN elements, about 20 % of elements lies in the Doppler blue-shift region. Our results imply that not all magnetic elements lie in the down-draft sites.

Solar Intranetwork Magnetic Elements: Evolution and Lifetime

Based on Hinode SOT/NFI observations with greatly improved spatial and temporal resolution and polarization sensitivity, the lifestory of the intranetwork (IN) magnetic elements are explored in a solar quiet region. A total of 2282 IN elements are followed from their appearance to disappearance and their fluxes measured. By tracing individual IN elements their lifetimes are obtained, which fall in the range from 1 to 20 min. The average lifetime is 2.9±2.0 min. The observed lifetime distribution is well represented by an exponential function. Therefore, the e-fold characteristic lifetime is determined by a least-square fitting to the observations, which is 2.1±0.3 min. The lifetime of IN elements is correlated closely with their flux. The evolution of IN elements is described according to the forms of their birth and disappearance. Based on the lifetime and flux obtained from the new observations, it is estimated that the IN elements have the capacity of heating the corona with a power of 2.1×1028 erg s−1 for the whole Sun.

Special section: Grid/distributed computing systems security

We are delighted to present to you the special section of Future Generation Computer Systems (FGCS) on grid/distributed computing systems security. This special section contains five technical papers dealing with cutting-edge research and technology related to the design,modeling, and implementation of architectures, algorithms and protocols of computer systems or environments. In the paper ‘‘Secure verifiable non-interactive oblivious transfer protocol using RSA and bit commitment in a distributed environment’’, Soongohn Kim et al. analyze the basic concept of an OT (Oblivious Transfer) protocol for exchanging secret information fairly, survey the basic idea of an interactive and secure noninteractive OT protocol, and present a new non-interactive type of OTprotocolwhich is verifiable. The amount of traffic of transferring information of the suggested method is less than or equal to that of the conventional interactive method. The paper ‘‘Structure design and test of an enterprise security management system with advanced internal security’’ by Seoksoo Kim et al., analyzes existing enterprise security management systems and, on the basis of the results, proposes and tests an enterprise security management system with reinforced internal security. For the test, the authors used a firewall through log analysis and designed Intranet work using a virtual IP system. J. H. Abawajy proposes a new two-level adaptive space-sharing scheduling policy for non-dedicated heterogeneous commodity-

Comparison of Magnetic Flux Distribution between a Coronal Hole and a Quiet Region

Employing Big Bear Solar Observatory (BBSO) deep magnetograms and H${\alpha}$ images in a quiet region and a coronal hole, observed on September 14 and 16, 2004, respectively, we have explored the magnetic flux emergence, disappearance and distribution in the two regions. The following results are obtained: (1) The evolution of magnetic flux in the quiet region is much faster than that in the coronal hole, as the flux appeared in the form of ephemeral regions in the quiet region is 4.3 times as large as that in the coronal hole, and the flux disappeared in the form of flux cancellation, 2.9 times as fast as in the coronal hole. (2) More magnetic elements with opposite polarities in the quiet region are connected by arch filaments, estimating from magnetograms and H${\alpha}$ images. (3) We measured the magnetic flux of about 1000 magnetic elements in each observing region. The flux distribution of network and intranetwork (IN) elements is similar in both polarities in the quiet region. For network fields in the coronal hole, the number of negative elements is much more than that of positive elements. However for the IN fields, the number of positive elements is much more than that of negative elements. (4) In the coronal hole, the fraction of negative flux change obviously with different threshold flux density. 73% of the magnetic fields with flux density larger than 2 Gauss is negative polarity, and 95% of the magnetic fields is negative, if we only measure the fields with their flux density larger than 20 Gauss. Our results display that in a coronal hole, stronger fields is occupied by one predominant polarity; however the majority of weaker fields, occupied by the other polarity.

Magnetic field evolution in a quiet region and a coronal hole

Using Big Bear Solar Observatory (BBSO) magnetograms and H ${\alpha}$ images in a quiet region and a coronal hole, observed on 9 14 and 16, 2004, respectively, we have explored the magnetic flux emergence, disappearance and distribution in the two regions. The following results are obtained: (1) The evolution of magnetic flux in the quiet region is much faster than that in the coronal hole, as the flux appeared in the form of ephemeral regions in the quiet region is four times as large as that in the coronal hole, and the flux disappeared in the form of flux cancellation, three times as fast as in the coronal hole. (2) More magnetic elements with opposite polarities in the quiet region are connected by arch filaments. (3) The flux distribution of network and intranetwork (IN) elements is similar in both polarities in the quiet region. For network fields in the coronal hole, the number of negative elements is much more than that of positive elements. However for the IN fields, the number of positive elements is much more than that of negative elements. (4) In the coronal hole, the fraction of negative flux change obviously with different threshold flux density. 73% of the magnetic fields with flux density larger than 2 Gauss is negative polarity, and 95% of the magnetic fields is negative, if we only measure the fields with their flux density larger than 20 Gauss. These results display that in a coronal hole, stronger fields is occupied by one predominant polarity; however the majority of weaker fields, occupied by the other polarity.

An Intra Network Proposal for the Regional Integration of Landcare

The use of online forums and geospatial planning support systems in websites for community-based natural resource management is increasing. Interlocking regional intranet websites have the potential to address the challenges of integrating catchment-wide objectives and strategies with grass-roots Landcare activities. In this article it is argued that a well-implemented Landcare Intra Network (LIN) would facilitate the delivery of ecological and social information, enhance communication between the various stakeholders and enable more genuine joint decision-making across rural landscapes. In this way a LIN would have the potential to support sustainable practices across various ecological and political scales and a range of social and economic perspectives.

What ‘sells’ an Intranet?

What is it that makes an Intranet work? How do you get members of the organisation to use it? With apologies to Estate Agents, the answer can probably be summed up as ‘Planning, Planning and Planning.’ That is, planning Who the Intranet is for, planning What it is intended to achieve; and planning How it is to be achieved.

The Polarity Distribution of Intranetwork and Network Fields

We have studied the relative polarity distribution of intranetwork (IN) and network (NW) fields for the first time, using very deep magnetograms obtained at Big Bear Solar Observatory (BBSO) and Huairou Solar Observation Station (HSOS). We found 80 network cells and measured the polarities of intranetwork and network magnetic flux within each cell. The analysis reveals that, in enhanced networks, the signed sum of the IN flux in a cell and the signed sum of the network flux on the boundary of the cell is opposite with 90% probability; in mixed-polarity network, the corresponding signed fluxes are opposite with a probability of 75%. We suggest that:(1) Some of the excess flux within a cell may connect to a weak field component of the IN field that is below the detection limit.(2) Some IN flux, preferentially close to the cell boundary, may be topologically connected to the network field.(3) Some observational effects might produce this anti-correlation.

The Relation of Ca II K FEATURES TO MAGNETIC FIELD

We studied quantitatively the relation between the intensity of Caii K-line bright features and the intensity of the associated magnetic elements using two data sets obtained at the Big Bear Solar Observatory. Both network and intranetwork (IN) structures were considered. Magnetic field changes always affected the K-line emission; for example, the appearance of new bipoles was always followed by enhanced K-line emission. There is an almost linear correlation between the K-line intensity and the magnetic field strength of the stronger network elements (elements with absolute field strength higher than 11–19.5 G). We identified two classes of intranetwork K-line elements: magnetic and non-magnetic ones. The number of the magnetic K-line IN elements above a 1-sigma threshold was only 5%–10% of the number of the non-magnetic ones. The magnetic K-line IN elements were almost 3 to 4 times brighter compared to the non-magnetic elements. On the other hand, the non-magnetic elements were moving with typical velocities of 35–40 km s−1 while the velocities of the magnetic K-line elements were of the order of 1 km s−1.

The velocities of intranetwork and network magnetic fields

We analyzed two sequences of quiet-Sun magnetograms obtained on June 4, 1992 and July 28, 1994. Both were observed during excellent seeing conditions such that the weak intranetwork (IN) fields are observed clearly during the entire periods. Using the local correlation tracking technique, we derived the horizontal velocity fields of IN and network magnetic fields. They consist of two components: (1) radial divergence flows which move IN fields from the network interior to the boundaries, and (2) lateral flows which move along the network boundaries and converge toward stronger magnetic elements. Furthermore, we constructed divergence maps based on horizonal velocities, which are a good representation of the vertical velocities of supergranules. For the June 4, 1992 data, the enhanced network area in the field of view has twice the flux density, 10% higher supergranular velocity and 20% larger cell sizes than the quiet, unenhanced network area. Based on the number densities and flow velocities of IN fields derived in this paper and a previous paper (Wang et al., 1995), we estimate that the lower limit of total energy released from the recycling of IN fields is 1.2 × 1028 erg s−1, which is comparable to the energy required for coronal heating.

Flux distribution of solar intranetwork magnetic fields

Big Bear deep magnetograms of June 4, 1992 provide unprecedented observations for direct measurements of solar intranetwork (IN) magnetic fields. More than 2500 individual IN elements and 500 network elements are identified and their magnetic flux measured in a quiet region of 300 × 235 arc sec. The analysis reveals the following results: (1) IN element flux ranges from 1016 Mx (detection limit) to 2 × 1018 Mx, with a peak flux distribution of 6 × 1016 Mx. (2) More than 20% of the total flux in this quiet region is in the form of IN elements at any given time. (3) Most IN elements appear as a cluster of mixed polarities from an emergence center (or centers) somewhere within the network interior. (4) The IN flux is smaller than the network flux by more than an order of magnitude. It has a uniform spatial distribution with equal amount of both polarities. It is speculated that IN fields are intrinsically different from network fields and may be generated from a different source as well.

The velocity pattern of weak solar magnetic fields

The proper motion of magnetic elements on the quiet sun has been measured by means of local correlation tracking. The existence of a pattern in the intranetwork (IN) flow is confirmed. This velocity field is consistent with the direct Doppler measurement of the horizontal component of the supergranular velocity field. The IN elements generally move toward the network boundaries. By tracking test points, it is confirmed that the magnetic elements converge in areas corresponding to the magnetic network. But because the IN elements are of random polarity, they cannot contribute to the growth or maintenance of the magnetic network. By calculating the cross correlation between the magnetogram and Dopplergram, it is confirmed that the supergranule boundaries and the magnetic network are roughly correlated.

Weak solar fields and their connection to the solar cycle

Videomagnetograph observations of the weak solar magnetic fields are discussed. Intranetwork (IN) elements are found to emerge in bipolar form, but to flow in a random pattern rather than toward the network elements. Merging of IN fields is found to be more important than the ephemeral regions as a source of new network elements. Arguments for and against the hypothesis that all solar fields are intrinsically strong are considered. It is noted that reconnection and merging of magnetic fields take place continually under the conditions presently examined.

The smallest observable elements of magnetic flux

We have followed disappearing elements of magnetic flux to determine the smallest elements detectable with the Big Bear videomagnetograph. All the elements followed were disappearing through interaction with elements of opposite polarity. The last remaining visible segment of magnectic field of such features can be used to infer the total magnetic flux of these and other small flux elements visible on the magnetograms. We used both photographic and digital videomagnetograms combining 4096 Zeeman frames made at Big Bear. Fifteen elements were measured near the vanishing point, in a 2–8 hr period. The minimum observable fluxes fall in the range of 1.0 × 1016 to 1.4 × 1017 Mx, and the apparent size of these elements is in the range of 1 to 9 square arc sec. The process of disappearance appears to be a smooth one. The smallest detectable elements of network field and ephemeral regions (ER) appear to be the same as the small intra-network (IN) field elements. The present limit is still instrumental; elements smaller than 1 × 1016 would not have been detected.