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The paper presents an analysis of the correlation between the level of trust in management, colleagues, and self-reported health among industrial workers. It was revealed that a high level of trust in the management determines the presence of a good self-reported health of employees. Trust in the workplace affects the psychological well-being and adaptation of the individual, that’s why it is important to improve psychological climate and reduce the level of the stress at the workplace., На материалах социологического опроса работников промышленных предприятий Пермского края (n = 439) представлен анализ корреляции уровня доверия руководству и коллегам и самооценки здоровья работников. Выявлено, что высокий уровень доверия руководству связан с хорошей самооценкой здоровья у работников. Обоснован тезис о необходимости формирования благоприятного социально-психологического климата и доверия на рабочем месте как факторов психологического и физического здоровья.

In this paper, some features of electromagnetic transmission of the waves of ”semiconductor dielectric” periodic Bragg structure with a finite number of periods have been investigated. In the absence of absorption, for a structure with p-type semiconductor layers, we have analyzed the dependences on the external magnetic field of photon spectrum and transmission coefficient spectrum. It has been shown that with an increasing magnetic field, there is a significant narrowing of bandwidth and broadening of band gaps, as well as formation of new band gaps in the resonance region. The boundaries of all forbidden and allowed bands are shifted to higher frequencies with the increase of the angle of radiation incidence.

In this paper, some features of electromagnetic transmission of the waves of ”semiconductor dielectric” periodic Bragg structure with a finite number of periods have been investigated. In the absence of absorption, for a structure with p-type semiconductor layers, we have analyzed the dependences on the external magnetic field of photon spectrum and transmission coefficient spectrum. It has been shown that with an increasing magnetic field, there is a significant narrowing of bandwidth and broadening of band gaps, as well as formation of new band gaps in the resonance region. The boundaries of all forbidden and allowed bands are shifted to higher frequencies with the increase of the angle of radiation incidence.

In this paper, some features of electromagnetic transmission of the waves of ”semiconductor dielectric” periodic Bragg structure with a finite number of periods have been investigated. In the absence of absorption, for a structure with p-type semiconductor layers, we have analyzed the dependences on the external magnetic field of photon spectrum and transmission coefficient spectrum. It has been shown that with an increasing magnetic field, there is a significant narrowing of bandwidth and broadening of band gaps, as well as formation of new band gaps in the resonance region. The boundaries of all forbidden and allowed bands are shifted to higher frequencies with the increase of the angle of radiation incidence.

We explore the possibilities for detecting pulsars that have ceased to radiate in the radio band. We consider two models: the model with hindered particle escape from the pulsar surface (first suggested by Ruderman and Sutherland 1975) and the model with free particle escape (Arons 1981; Mestel 1999). In the model with hindered particle escape, the number of particles that leave the pulsar magnetosphere is small and their radiation cannot be detected with currently available instruments. At the same time, for the free particle escape model, both the number of particles and the radiation intensity are high enough for such pulsars to be detectable with the presently available receivers such as GLAST and AGILE spacecrafts. It is also possible that extinct radio pulsars can be among the unidentified EGRET sources., Comment: 5 pages, 1 figure corrected version of the paper that was published in Astronomy Letters

We explore the possibilities for detecting pulsars that have ceased to radiate in the radio band. We consider two models: the model with hindered particle escape from the pulsar surface (first suggested by Ruderman and Sutherland 1975) and the model with free particle escape (Arons 1981; Mestel 1999). In the model with hindered particle escape, the number of particles that leave the pulsar magnetosphere is small and their radiation cannot be detected with currently available instruments. At the same time, for the free particle escape model, both the number of particles and the radiation intensity are high enough for such pulsars to be detectable with the presently available receivers such as GLAST and AGILE spacecrafts. It is also possible that extinct radio pulsars can be among the unidentified EGRET sources., Comment: 5 pages, 1 figure corrected version of the paper that was published in Astronomy Letters

We explore the possibilities for detecting pulsars that have ceased to radiate in the radio band. We consider two models: the model with hindered particle escape from the pulsar surface (first suggested by Ruderman and Sutherland 1975) and the model with free particle escape (Arons 1981; Mestel 1999). In the model with hindered particle escape, the number of particles that leave the pulsar magnetosphere is small and their radiation cannot be detected with currently available instruments. At the same time, for the free particle escape model, both the number of particles and the radiation intensity are high enough for such pulsars to be detectable with the presently available receivers such as GLAST and AGILE spacecrafts. It is also possible that extinct radio pulsars can be among the unidentified EGRET sources., Comment: 5 pages, 1 figure corrected version of the paper that was published in Astronomy Letters

We revisit the case of magneto-rotational evolution of neutron stars (NSs) with accounting for changes of the angle \chi between spin and magnetic axes. This element of the evolution of NSs is very important for age estimates and population modeling, but usually it is neglected. In the framework of two models of energy losses we demonstrate that unless NSs are born with the inclination angle \chi_0 very close (within 1 degree) to the position of maximal losses, pulsars with short initial periods quickly reach regions of small energy losses (aligned rotators in the case of magneto-dipole losses and orthogonal rotators -- in the case of current losses) without significant spin-down. This means that either most of known NSs should be born with relatively long periods close to presently observed values, or the initial inclination angles should be large (close to 90) for the magnetodipole model and very small (close to 0) for the current losses model, or that both models cannot be applied for the whole evolutionary track of a typical NS. In particular, magnetar candidates should be born with periods close to the observed ones within the scope of both models of energy losses. We discuss how these considerations can influence population synthesis models and age estimates for different types of isolated NSs. Focusing on the model of current losses we illustrate our conclusion with evolutionary track reconstructions on the P--\sin \chi plane. We conclude, that most probably both existing models of energy losses -- magneto-dipole and longitudinal current -- require serious modifications, on the other hand, estimates obtained under the standard assumption of \sin \chi=1=const does not have solid theoretical ground and should be taken with care., Comment: 12 pages, 7 figures

We revisit the case of magneto-rotational evolution of neutron stars (NSs) with accounting for changes of the angle \chi between spin and magnetic axes. This element of the evolution of NSs is very important for age estimates and population modeling, but usually it is neglected. In the framework of two models of energy losses we demonstrate that unless NSs are born with the inclination angle \chi_0 very close (within 1 degree) to the position of maximal losses, pulsars with short initial periods quickly reach regions of small energy losses (aligned rotators in the case of magneto-dipole losses and orthogonal rotators -- in the case of current losses) without significant spin-down. This means that either most of known NSs should be born with relatively long periods close to presently observed values, or the initial inclination angles should be large (close to 90) for the magnetodipole model and very small (close to 0) for the current losses model, or that both models cannot be applied for the whole evolutionary track of a typical NS. In particular, magnetar candidates should be born with periods close to the observed ones within the scope of both models of energy losses. We discuss how these considerations can influence population synthesis models and age estimates for different types of isolated NSs. Focusing on the model of current losses we illustrate our conclusion with evolutionary track reconstructions on the P--\sin \chi plane. We conclude, that most probably both existing models of energy losses -- magneto-dipole and longitudinal current -- require serious modifications, on the other hand, estimates obtained under the standard assumption of \sin \chi=1=const does not have solid theoretical ground and should be taken with care., Comment: 12 pages, 7 figures

We study the statistical distribution of extinct radio pulsars -- isolated neutron stars, that just crossed the death line. An important element that distinguishes our study from other works is a consistent allowance for the evolution of the angle between the magnetic and spin axes. We find the distribution of extinct radio pulsars in spin period for two models: the model with hindered particle escape from the neutron star surface and the model with free particle escape. The total number of extinct radio pulsars is shown to be much smaller than for the model in which the evolution of an inclination angle is disregarded. The decrease in total number of extinct radio pulsars arises from the fact, that account for evolution of the inclination angle allows the transition of a neutron star to the propeller stage appear at much smaller periods (P~5-10 s) than it is commonly assumed., Comment: 7 pages, 8 figures. Corrected Introduction and figures 1 and 8

We analyze the statistical distribution of neutron stars at the stage of a supersonic propeller. An important point of our analysis is allowance for the evolution of the angle of inclination of the magnetic axis to the spin axis of the neutron star for the boundary of the transition to the supersonic propeller stage for two models: the model with hindered particle escape from the stellar surface and the model with free particle escape. As a result, we have shown that a consistent allowance for the evolution of the inclination angle in the region of extinct radio pulsars for the two models leads to an increase in the total number of neutron stars at the supersonic propeller stage. This increase stems from he fact that when allowing for the evolution of the inclination angle $\chi$ for neutron stars in the region of extinct radio pulsars and, hence, for the boundary of the transition to the propeller stage, this transition is possible at shorter spin periods (P~5-10 s) than assumed in the standard model., Comment: 15 pages, 6 figures; scale corrected for figures 3-6

We analyze the statistical distribution of neutron stars at the stage of a supersonic propeller. An important point of our analysis is allowance for the evolution of the angle of inclination of the magnetic axis to the spin axis of the neutron star for the boundary of the transition to the supersonic propeller stage for two models: the model with hindered particle escape from the stellar surface and the model with free particle escape. As a result, we have shown that a consistent allowance for the evolution of the inclination angle in the region of extinct radio pulsars for the two models leads to an increase in the total number of neutron stars at the supersonic propeller stage. This increase stems from he fact that when allowing for the evolution of the inclination angle $\chi$ for neutron stars in the region of extinct radio pulsars and, hence, for the boundary of the transition to the propeller stage, this transition is possible at shorter spin periods (P~5-10 s) than assumed in the standard model., Comment: 15 pages, 6 figures; scale corrected for figures 3-6

We study the statistical distribution of extinct radio pulsars -- isolated neutron stars, that just crossed the death line. An important element that distinguishes our study from other works is a consistent allowance for the evolution of the angle between the magnetic and spin axes. We find the distribution of extinct radio pulsars in spin period for two models: the model with hindered particle escape from the neutron star surface and the model with free particle escape. The total number of extinct radio pulsars is shown to be much smaller than for the model in which the evolution of an inclination angle is disregarded. The decrease in total number of extinct radio pulsars arises from the fact, that account for evolution of the inclination angle allows the transition of a neutron star to the propeller stage appear at much smaller periods (P~5-10 s) than it is commonly assumed., Comment: 7 pages, 8 figures. Corrected Introduction and figures 1 and 8