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    Wyświetlanie 1-13 z 13
    Tytuł:
    Comparative dynamic analysis of the portal cranes of type H and X
    Autorzy:
    Vasiljević, Rade
    Powiązania:
    https://bibliotekanauki.pl/articles/1839622.pdf
    Data publikacji:
    2020
    Wydawca:
    Polskie Towarzystwo Mechaniki Teoretycznej i Stosowanej
    Tematy:
    portal cranes
    type H
    type X
    Finite Element Method
    comparative dynamicanalysis
    Opis:
    In this paper, a comparative dynamic analysis of the portal cranes of type H and X is described. The difference of the considered cranes arises from the difference of their portals. These two types of portals have the same main geometric measurements. They differ only at the medium level in the horizontal plane. The first type of the portal on the middle level has an H-frame, while the second type has an X-frame. In this paper, dynamic parameters of the two portals have been compared. Estimation has been done to find which of the two types of portals has more favourable dynamic stability for overturn.
    Źródło:
    Journal of Theoretical and Applied Mechanics; 2020, 58, 4; 825-839
    1429-2955
    Pojawia się w:
    Journal of Theoretical and Applied Mechanics
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    RCV Type-X – estoński „bezzałogowy czołg”
    Autorzy:
    Kucharski, Bartłomiej.
    Powiązania:
    Wojsko i Technika 2021, nr 3, s. 24-28
    Data publikacji:
    2021
    Tematy:
    Milrem Robotics (Estonia)
    Przemysł zbrojeniowy
    Wozy bojowe
    Pojazdy bezzałogowe lądowe
    THeMIS (bezzałogowy pojazd naziemny)
    RCV Type-X (bezzałogowy pojazd bojowy)
    Dane taktyczno-techniczne sprzętu wojskowego
    Artykuł z czasopisma fachowego
    Artykuł z czasopisma wojskowego
    Opis:
    Artykuł dotyczy wozów bojowych produkcji estońskiej, kraju niewielkiego, ale otwartego na nowe technologie. Liderem rozwoju bezzałogowych pojazdów naziemnych jest prywatna firma Milrem Robotics, która w 2013 roku zbudowała gąsienicowy pojazd bezzałogowy z napędem hybrydowym THeMIS. W maju 2020 roku firma zaprezentowała kolejny pojazd – RCV Type-X, bezzałogowy pojazd bojowy. Pojazd ma być gotowy do produkcji w połowie 2023 roku, przedstawiono opis techniczny wozu.
    Fotografie.
    Dostawca treści:
    Bibliografia CBW
    Artykuł
    Tytuł:
    Differential equation of x = f(y) and interpretation of the solution in Mathematica program
    Równanie różniczkowe typu x = f(y) i interpretacja rozwiązania w programie Mathematica
    Autorzy:
    Czajkowski, Andrzej Antoni
    Oleszak, Wojciech Kazimierz
    Frączak, Piotr Stanisław
    Powiązania:
    https://bibliotekanauki.pl/articles/135928.pdf
    Data publikacji:
    2019
    Wydawca:
    Wyższa Szkoła Techniczno-Ekonomiczna w Szczecinie
    Tematy:
    differential equations
    equation of type x=f(y')
    analytical solution
    variable substitution method
    geometric interpretation of the solution
    Mathematica program
    równania różniczkowe
    równanie typu y=f(y')
    rozwiązanie analityczne
    metoda podstawienia nowej zmiennej
    interpretacja geometryczna rozwiązania
    program Mathematica
    Opis:
    Introduction and aims: The paper presents a method of solving x=f(y') equations. The main aim of the work is to show how to solve this type of differential equations. In addition, the purpose of the discussion is to present the appropriate algorithms in Mathematica program, which are used to present the geometric interpretation of the obtained solutions. Material and methods: The sources contain material on the subject of differential equations. The method of mathematical analysis has been used. Results: In the analysis of selected examples, the method of substitution of new variable t has been used and the solution of the studied differential equation has been obtained in the form of the system of equations x=x(t) and y=y(t). Conclusion: The solution of the differential equation of the type x=f(y') in the form of a system of equations x=x(t) and y=y(t) can be interpreted graphically using an appropriately used algorithm in Mathematica numerical program.
    Wstęp i cele: W pracy przedstawiono metodę rozwiązywania równań typu y=f(y'). Głównym celem pracy jest pokazanie sposobu rozwiązywania tego typu równań różniczkowych. Ponadto celem rozważań jest przestawienie odpowiednich algorytmów w programie Mathematica, które służą do przedstawienia interpretacji geometrycznej otrzymanych rozwiązań. Materiały i metody: Źródła zawierają materiał dotyczący tematyki równań różniczkowych. Zastosowano metodę analizy matematycznej. Wyniki: W analizie wybranych przykładów zastosowano metodę podstawienia nowej zmiennej t i otrzymano rozwiązanie badanego równania różniczkowego w postaci układu równań x=x(t) i y=y(t). Wniosek: Rozwiązanie równania różniczkowego typu y=f(y') w postaci układu równań x=x(t) i y=y(t) można zinterpretować graficznie stosując odpowiednio zastosowany algorytm w programie numerycznym Mathematica.
    Źródło:
    Problemy Nauk Stosowanych; 2019, 10; 15-24
    2300-6110
    Pojawia się w:
    Problemy Nauk Stosowanych
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Experimental study of X-ray emission yield in a Filippov-type Plasma Focus operating in neon and neon-krypton mixture
    Autorzy:
    Babazadeh, A.
    Roshan, M.
    Kiai, S.
    Powiązania:
    https://bibliotekanauki.pl/articles/147028.pdf
    Data publikacji:
    2002
    Wydawca:
    Instytut Chemii i Techniki Jądrowej
    Tematy:
    Filippov-type plasma focus
    gas admixture
    X-ray
    Opis:
    Since the installation of PF-DENA at AEOI about one year ago, we performed quantitative studies of variation of X-ray radiations from a new Filippov-type plasma focus device: Dena (90 kJ, 25 kV, 288 ěF). The operating gas was neon at a constant low pressure of 1 torr and different pressures of krypton admixture (up to 0.3 torr), with the discharge voltage up to 18 kV. For a charging voltage of 17 kV with 41 kJ stored energy and spark gap pressure of 1.2×10-2 torr, the maximum soft and little hard X-ray (SXR-HXR) emission is found for the neon, resulting in a total SXR yield of 2 V/shot measured by silicon semiconductor diode detectors. Concerning the effect of krypton admixture, a maximum intensity of SXR radiation has been observed at low krypton pressure that is about 1 V/shot. At higher pressure, the quantity of the SXR emission decreases down to zero. However, the maximum intensity of the HXR radiation yield in the same pressure range was found to be 2.5 V/shot. By increasing the pressure of krypton up to 0.3 torr, the results show that the krypton admixture gas generally causes, a decrease of the SXR radiation yield down to zero, whereas, the HXR emission yield carries a maximum value at the optimum pressure of krypton that is about 0.1 torr. Nevertheless, the pressure increments of krypton admixture lead to decreasing in the discharge voltage for the maximum X-ray production.
    Źródło:
    Nukleonika; 2002, 47, 3; 123-125
    0029-5922
    1508-5791
    Pojawia się w:
    Nukleonika
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Tendencies Group Type III Burst Form Type II Burst During Low activity
    Autorzy:
    Hamidi, Z. S.
    Mokthtar, Fatin Nabila
    Shariff, N. N. M.
    Ali, Marhana Omar
    Husien, Nurulhazwani
    Sabri, S. N. U.
    Zainol, N. H.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1191365.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    X-ray region
    radio region
    solar burst
    sun
    sun type II
    sun type III
    Opis:
    Using the e-CALLISTO network radio observations on 1st June 2015, we present an analysis of the complex type III and type II solar radio bursts during low activity. This event occurred on 1st July 2015 at 13:52 UT (complex solar burst type III) and 13:40 UT - 13:44 UT (solar burst type II). Solar burst type detected at (i) BIR, (ii) BLENSW, (iii) Essen, (iv) Glascow (v) Osra, (vi) Rwanda. The spectral shape consists of high flux densities at meter wavelengths. The energy going into plasma heating during each flare was estimated by computing the time evolution of the energy content of the thermal plasma and obtaining the peak value. This constitutes a lower limit to the thermal energy, since it does not account for the cooling of the plasma prior to this time nor to any heating at later times. It is also believed that the meter wavelength branch of the this type III spectrum may be attributable to second-phase accelerated electrons to form type II burst. There are four sunspots of the active regions (AR2355, AR2356, AR2357, and AR2358) during this event. The solar wind recorded during the event is 342.4 km/s and the density of the proton recorded is 4.1 protons/cm3. Moreover, the are some evidence that radio-quiet CMEs mostly came from the edges of the sun. The main goal of this study was to determine whether is there any possibilities that the radio burst can be formed even the Sun is at low activity and this event is one of the candidate events.
    Źródło:
    World Scientific News; 2016, 34; 121-134
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Geo-effective Disturbances from the “Beta-Gamma-Delta” Magnetic Fields on Active Region AR 2403
    Autorzy:
    Sabri, S. N. U.
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Zainol, N. H.
    Ali, M. Omar
    Hussien, Nurul Hazwani
    Powiązania:
    https://bibliotekanauki.pl/articles/1192069.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    Solar Radio Burst Type IV
    X-ray region
    Solar flare
    active region AR 2403
    Opis:
    This moving solar radio burst type IV, which lies in between 980 – 1260 MHZ was observed using Compound Astronomical Low-Cost Low- Frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) spectrometer and will discussed in detail. CALLISTO system was used and the data were recorded. From BLEN5M’s Radio Flux Density data, it shown that a brief description of the formation of a dynamic formation of solar radio burst type IV due to an active region, AR 2403. This event proved that solar radio burst type IV has a broadband continuum features and has strong pulsations in some range of time. In this event it was took about 8 minutes and it can be high in possibility solar flare and CMEs event followed due to this event. AR 2403 remained active and produced an X- class solar flares and it showed “Beta- Gamma-Delta” magnetic field that gives solar flares which can make geo-effective disturbance to our earth satellite and we have to investigate how plasma – magnetic field in the solar corona which can produce suprathermal electron pulsation about 8 minutes. In this event, it has solar wind speed in 364.8 km/sec and solar wind density in 11.0 protons/cm3.
    Źródło:
    World Scientific News; 2016, 37; 1-11
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Analysis of Solar Burst Type II, III, and IV and Determination of a Drift Rate of a Single Type III Solar Burst
    Autorzy:
    Hamidi, Z. S.
    Ibrahim, M. B.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/411732.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    sun
    solar burst
    type II,III,IV
    radio region
    X-ray region
    solar flare
    active region
    Opis:
    The main feature of solar radio type II, III and IV burst is outlined. In this event there are three combinations of bursts that related to the solar flare phenomenon on 6th July 2012. This event is one of good example to observe how far the influence of type II burst could impact the formation of type IV burst and III solar bursts. At first stage, it was observed that a sub-type of H burst form within 2 minutes before type IV solar burst form. The type IV burst is due to the eruption of active region AR 1515 with a fine structure (FS). We used a Blein CALLISTO data in this case. Further analysis also showed that the total energy of the burst are in the range of 4.875 × 10-25 J to 8.48 × 10-25 J and plasma frequency is equal to 1.24 × 104 Hz. Therefore, we could say that in this case, before the solar burst type III occurred, the ejection of CMEs already ejected.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 19, 2; 160-170
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    An Analysis of the Electron Density and Drift Rate of Solar Burst Type III During 13th of May 2015
    Autorzy:
    Ali, M. O.
    Hamidi, Z. S.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192997.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    Sun
    X-ray region
    radio region
    solar burst
    solar flare
    type III
    Opis:
    During 13th of May 2015, the solar wind is very high velocity, which is 733 kms-1 as compared to 367.5 kms-1. It is believed that the plasma–magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type II was recorded by CALLISTO spectrometer from 20-85 MHz. Using data from a the Blein observatory, the complex structure of solar burst type III can also be found in the early stage of the formation of type III solar burst type event due to active region AR 12339. The drift rate of solar burst type III exceeds 1.0 MHz/s with 6.318 x1012 e/m3 a density of electron in the solar corona. There were also 2 groups of solar radio burst type III were observed. This CME was detected at 08:36 UT which is 1and ½ hour after the solar burst detected. This event shows a strong radiation in radio region, but not in X-ray region.
    Źródło:
    World Scientific News; 2016, 31; 1-11
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Solar Burst Type IV Signature Associated with Solar Prominences on 20th January 2016
    Autorzy:
    Hamidi, Z. S.
    Hamzah, N.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1178518.pdf
    Data publikacji:
    2017
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    Sun
    X-ray region
    solar burst
    solar flare
    type IV radio region
    Opis:
    Proceeding from close association between solar eruptions, flare and CMEs, we analyze between burst at 980 MHz to 1270 MHz, recorded at the Blein, Switzerland on 20th January 2016. This burst indicates the emission radiation from the Sun from numerous high energy electrons in active region AR2484 and AR2487 forming a large prominence in that particular area. Solar prominences usually occur in loop shape and can last for weeks or months. This event allows us to investigate the electron density and drift rate of solar burst type IV During that time the Sun has the moderate number of sunspots with 55.The radio sources responsibly for IV appear to expand spherically through the solar corona after eject on y solar flare. This event shows a strong radiation in radio region, but not in X-ray region. This burst intense radio phenomena that follow with solar flares. It has a wide band and fine structure. It can be considered as an intermediate fast drift burst (IMDs). This fiber burst has a negative drift rate where the drift is interpreted by the group velocity of the whistler-mode waves. This burst appears is single SRBT III for approximately within 7 minutes with starting time is 8.23 UT. This burst duration is longer compared to the other events. It can be considered as a IV because it begins at the same time as the explosive phase of solar flare. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. At the same time, the number of particles traveled a given path in reconnecting area falls exponentially with the increase of this path because of losses owing to a leaving of particles the acceleration volume due to drift.
    Źródło:
    World Scientific News; 2017, 70, 2; 111-121
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Formation of Fundamental Structure of Solar Radio Burst Type II Due X6.9 Class Solar Flare
    Autorzy:
    Zainol, N. H.
    Hamidi, Z. S.
    Shariff, N. N. M.
    Ali, Marhana Omar
    Husien, Nurulhazwani
    Sabri, S. N. U.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1190115.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Sun
    solar burst
    type II
    radio region
    X-ray region
    solar flare
    Coronal Mass Ejections (CMEs)
    Opis:
    A vigorous solar flare event marked on the spectrometer of the CALLISTO data, being one of the highest solar flare event that successfully detected. The formation of solar burst type II in meter region and their associated with X6. 9-class solar flares have been reported. The burst has been observed at the Blein Obsevatory, Switzerland, which detected by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) system in the range of 170-870 MHz in the two polarizations of left and right circular polarization. It occurred between 08:01 UT to 08:08 UT within 7 minutes. The Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory CALLISTO spectrometer is a solar dedicated spectrometer system that has been installed all over the world to monitor the Sun activity in 24 hours. The growth of this burst is often accompanied by abundance enhancement of particles which may take the form of multiple independent drifting bands or other forms of fine structure. Due to the results, the drift rate of this burst is 85.71 MHz s-1, which is considered as a fast drift rate. The burst detected using CALLISTO also being compared to results detected by X-ray GOES data. Both different electromagnetic spectrum shows the exact time. The observations of the burst being discussed in details.
    Źródło:
    World Scientific News; 2016, 35; 30-43
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Relativistic Energy Associated with a Moving Fiber Burst Type μIV Associated with The Class A Solar Prominence
    Autorzy:
    Hamidi, Z. S.
    Norsham, N. A. M.
    Shariff, N. N. M.
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1194133.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Coronal Mass Ejections (CMEs)
    Sun
    X-ray region
    solar burst
    solar flare
    type IV radio region
    Opis:
    The relativistic energy electron emission is found to occur only during proton events. Solar prominences usually occur in loop shape and can last for weeks or months. This event allows us to investigate the electron density and drift rate of solar burst type IV During 21st September 2015. During that time the Sun has the highest number of sunspots. The radio sources responsibly for Ivm appear to expand spherically through the solar corona after eject on y solar flare. This event shows a strong radiation in radio region, but not in X-ray region. This burst intense radio phenomena that follow with solar flares. It has a wide band structure from 1412-1428 MHz. It can be considered as an intermediate f drift burst (IMDs). This fiber burst has a negative drift rate where the drift is interpreted by the group velocity of the whistler-mode waves. Their bandwidth is approximately 2% of the emission frequency. The are accompanied a parallel-drift absorption band in the background continuum radiation. The occurrence of the event is interesting in many aspects which is also in ZSIS site. From the dynamic spectra of the CALLISTO, it can be observed that there a moving type IV burst. This burst appears is single SRBT III for approximately 16 minutes at 708UT till 716UT. This burst duration is longer compared to the other events. It can be considered as a Ivμ because it begins at the same time as the explosive phase of solar flare. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. At the same time, the number of particles traveled a given path in reconnecting area falls exponentially with increase of this path because of losses owing to a leaving of particles the acceleration volume due to drifts.
    Źródło:
    World Scientific News; 2016, 57; 11-20
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Metal-titanium oxide / quantum dot porous silicon / silicon-metal solar cell
    Autorzy:
    Abd, Ahmad Naji
    Mishjil, Khudheir A.
    Abdulsada, Ali Hamid
    Habubi, N. F.
    Powiązania:
    https://bibliotekanauki.pl/articles/1177996.pdf
    Data publikacji:
    2018
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    AFM
    FTIR
    TiO2
    X-Ray diffraction
    XRD
    electrochemical etching p-type silicon wafer
    nanocrystalline porous silicon
    Opis:
    In this paper, the nanocrystalline porous silicon (PSi) films are prepared by electrochemical etching of p-type silicon wafer with current density 7 mA/cm2 and etching times on the formation nano-sized pore array with a dimension of around different etching time. The films were characterized by the measurement of XRD, FTIR spectroscopy and atomic force microscopy properties (AFM). We have estimated crystallites size from X-Ray diffraction about nanoscale for porous silicon and Atomic Force microscopy confirms the nanometric size Chemical fictionalization during the electrochemical etching show on the surface chemical composition of PS. The etching possesses inhomogeneous microstructures that contain a-Si clusters (Si3–Si–H) dispersed in amorphous silica matrix. From the FTIR analyses showed that the Si dangling bonds of the as-prepared PS layer have large amount of Hydrogen to form weak Si–H bonds. The atomic force microscopy investigation shows the rough silicon surface, with increasing etching process (current density and etching time) porous structure nucleates which leads to an increase in the depth and width (diameter) of surface pits. Consequently, the surface roughness also increase.
    Źródło:
    World Scientific News; 2018, 96; 134-148
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    A new lifetime distribution
    Nowy rozkład cyklu życia
    Autorzy:
    Celik, N.
    Guloksuz, C. T.
    Powiązania:
    https://bibliotekanauki.pl/articles/301097.pdf
    Data publikacji:
    2017
    Wydawca:
    Polska Akademia Nauk. Polskie Naukowo-Techniczne Towarzystwo Eksploatacyjne PAN
    Tematy:
    rodzina rozkładów TX
    funkcja niezawodności
    współczynnik ryzyka
    ucinanie typu II
    T-X family of distributions
    reliability function
    hazard rate
    Type II Censoring
    Stress-Strength Probability
    Opis:
    The well-known statistical distributions such as Exponential, Weibull and Gamma distributions have been commonly used for analysing the different types of lifetime data. In this paper, following the idea of the extension of T-X family of distributions, we propose a new type of exponential distribution. We define the survival function, the hazard function and the mean time to failure related to this new distribution. Type II censoring procedure is also considered for this distribution. Additionally, stress-strength reliability and the maximum likelihood (ML) estimators of the unknown parameters are obtained. As an application, a real data set is used to show that the proposed distribution gives best fit than the alternative ones.
    Powszechnie znane rozkłady statystyczne, takie jak rozkład wykładniczy, Weibulla czy rozkład Gamma znajdują szerokie zastosowanie w analizie różnych typów danych dotyczących cyklu życia. W niniejszym artykule, zaproponowano nowy typ rozkładu wykładniczego, w oparciu o rozszerzenie rodziny rozkładów TX. Zdefiniowano funkcję przeżycia, funkcję ryzyka (hazardu) oraz średni czas do uszkodzenia w odniesieniu do proponowanego rozkładu. Rozpatrywano także procedurę ucinania typu II dla nowego rozkładu. Dodatkowo określono niezawodność wytrzymałościową oraz estymatory największej wiarygodności nieznanych parametrów. Sposób wykorzystania proponowanego rozkładu zilustrowano wykorzystując rzeczywisty zbiór danych. Wykazano, że daje on lepsze dopasowanie niż modele alternatywne.
    Źródło:
    Eksploatacja i Niezawodność; 2017, 19, 4; 634-639
    1507-2711
    Pojawia się w:
    Eksploatacja i Niezawodność
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
      Wyświetlanie 1-13 z 13

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