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Osobliwe zjawiska przyrodnicze w Rocznikach, czyli kronikach sławnego Królestwa Polskiego przez Jana Długosza opisane

Grad Marek

Przegląd Geofizyczny

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2020

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Z. 3-4

195--213

PL

W dwunastu księgach Roczników, czyli kronik sławnego Królestwa Polskiego Jan Długosz opisał dzieje Polski od jej legendarnych początków do roku 1480. W Rocznikach znajdujemy opisy niezwykłych zjawisk przyrodniczych. Do zjawisk astronomicznych zaliczymy opisy kilkunastu komet i zaćmienia Słońca. Z ekstremalnymi zjawiskami w atmosferze wiążą się uciążliwe i niebezpieczne dla ludzi ulewy, powodzie, susze, wichry, śniegi, mrozy, pioruny. Ze stanem atmosfery wiążą się także spektakularne zjawiska optyczne, jak potrójne Słońce (poboczne Słońce), czy potrójny Księżyc. Rzadkie i niebezpieczne są lokalne trzęsienia ziemi, ale w Rocznikach odnotowane zostały również liczne odczucia dalszych trzęsień ziemi. Fragmenty kilkudziesięciu opisów i krótkich wzmianek zostały zestawione chronologicznie na końcu tego opracowania.

EN

In twelve books of Annales seu cronicae incliti Regni Poloniae, Jan Długosz described the history of Poland from its legendary beginnings, until 1480. In the Annales we find descriptions of unusual natural phenomena. Astronomical phenomena include descriptions of a dozen comets and solar eclipses. Extreme phenomena in the atmosphere involve nuisance and dangerous for humans downpours, floods, droughts, strong winds, snows, frosts, lightning. The state of the atmosphere is also associated with spectacular optical phenomena, such as the triple Sun (Sun dog), or the triple Moon (Moon dog). Local earthquakes are rare and dangerous, but there are also numerous of further earthquakes described in the Annales. Text fragments from dozens of natural phenomena descriptions were compiled chronologically at the end of this study.

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Wpływ zaćmienia Słońca na produkcję energii elektrycznej przez system fotowoltaiczny

Strzelczyk P., Gil P.

Czasopismo Inżynierii Lądowej, Środowiska i Architektury / Journal of Civil Engineering, Environment and Architecture

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2017

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z. 64, nr 1

155--164

PL

W pracy zaprezentowano wpływ zaćmienia słonecznego z dnia 20.03.2015 na zmiany mocy oraz energii elektrycznej produkowanej przez system fotowoltaiczny w porównaniu do bezchmurnego dnia 17.03.2015 oraz do dnia 20.03.2014. System fotowoltaiczny wykorzystuje moduły z krzemu monokrystalicznego oraz inwerter solarny Soladin 600 podłączony do uczelnianej sieci elektrycznej. Moc szczytowa systemu wynosi 330W. Instalacja pracuje w Rzeszowie (φ=50°02’N λ=22°17’E). Moduły fotowoltaiczne zamontowane są na ramie pod stałym kątem 30° względem horyzontu (poziomu). Układ pomiarowy systemu fotowoltaicznego obejmował pomiar napięcia oraz prądu DC przed inwerterem, napięcia, prądu AC, mocy oraz częstotliwości na wyjściu inwertera. Zaprezentowano również pomiary całkowitego i bezpośredniego natężenia promieniowania słonecznego oraz promieniowanie rozproszone w dniu zaćmienia Słońca 20.03.2015 oraz w dniach 17.03.2015 i 20.03.2014 padające na płaszczyznę poziomą. Wszystkie parametry były mierzone co 10 sekund i uśredniane do 1 minutowych wartości. Dokonano również obserwacji wizualnych tarczy Słońca przy wykorzystaniu aparatu fotograficznego DSLR SONY A-57 oraz teleskopu typu Maksutow-Cassegrain o ogniskowej f=1500mm, oraz aperturze 127mm. Światłosiła teleskopu wynosi F 1:11,8. Zestaw zamontowany był na montażu paralaktycznym HEQ-5 SynScan. Wyniki badań ukazują, że podczas maksimum zaćmienia Słońca w Rzeszowie, które wystąpiło o godzinie 10:56 chwilowa moc systemu fotowoltaicznego zmalała o 60%, natomiast dobowa energia elektryczna zmalała o -13,4% w stosunku do niezachmurzonego dnia.

EN

The paper presents the impact of solar eclipse of 20.03.2015 on power and electricity produced changes by the PV system compared to the cloudless day 03.17.2015 and on 20.03.2014. The system uses photovoltaic monocrystalline silicon modules and solar inverter Soladin 600 connected to the electricity grid. Peak power system is 330W. Installation works in Rzeszow (φ = 50°02'N λ = 22°17'E). PV modules are mounted on the frame at a constant angle of 30° relative to the horizon. The measuring system comprised the measurement of voltage and DC current before an inverter, voltage, AC current, power and frequency at the output of the inverter. Also presented measurements of total and direct solar radiation and the scattered radiation in the day of a solar eclipse 03.20.2015 and on 03.17.2015 and 20.03.2014 falling on a horizontal plane. All parameters were measured every 10 seconds and averaged to 1 minute values. Also made visual observations of the sun using a camera Sony DSLR A-57 and Maksutov-Cassegrain telescope with a focal length f = 1500mm, 127mm aperture. Maximum aperture telescope is F 1: 11.8. Set was mounted on an equatorial mount HEQ-5 SynScan. The results show that the maximum eclipse in Rzeszow, which occurred at 10:56 instantaneous power photovoltaic system decreased by 60%, while the daily electricity decreased by -13.4% compared to cloudless day.

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Zaćmienie słońca a generacja fotowoltaiczna

Billewicz K.

Energetyka

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2015

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nr 7

491--492

PL

Podano, w jaki sposób zaćmienie słońca wpływa na poziom wytwarzania energii elektrycznej przez ogniwa słoneczne na przykładzie ogniw znajdujących się na dachu budynku Politechniki Wrocławskiej.

EN

Discussed is how a solar eclipse influences the level of electric energy generation by solar cells on the example of cells mounted on the building belonging to Wrocław Polytechnic University.

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The Propagation of An Impulsive Coronal Mass Ejections (CMEs) due to the High Solar Flares and Moreton Waves

Hamidi Z. S., Shariff N. N. M.

International Letters of Chemistry, Physics and Astronomy

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2014

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Vol. 14, iss. 1

118--126

EN

This paper provides a short review of some of the basic concepts related to the origin of Coronal Mass Ejections (CMEs). The numerous ideas which have been put forward to elucidate the initiation of CMEs are categorized in terms of whether this event is a gradual CME or impulsive CME. In this case, an earth-directed Coronal Mass Ejection (CME) was observed on April 2, 2014 by the Large Angle Spectrometric Coronagraph (LASCO) C2. This recent observations obtained a large impulsive CMEs. The CME, originating from the active region AR2027. The speed of CMEs is 1600 kms-1. A halo CME, a bright expanding ring at the North-West region is exploded beginning at about 14:36 UT, and the process of departing, expansion and propagation are highlighted. We discuss the correspondence of this event with the structure of the CME in the LASCO data. It is believed that the high solar flare and a Moreton waves initiate this kind of CMEs.

5

Statistical Study of Nine Months Distribution of Solar Flares

Hamidi Z. S., Shariff N. N. M., Monstein C.

International Letters of Chemistry, Physics and Astronomy

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2014

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Vol. 14, iss. 1

1--11

EN

Solar flare is one of the solar activities that take place in the outermost layer of the corona. Solar flares can heat the material to several million degrees in just a few minutes and at the same time they release the numerous amount of energy. It is believed that a change of magnetic field lines potentially creates the solar flares. The objectives of the study are to identify and compare the types of solar flares (in X-Ray) region and to improve understanding of solar flares. Data are taken from the NOAA website, from the United States Department of Commerce, NOAA, Space Weather Prediction Center (SPWC). Solar radio flux readings were merged together with the three classes and a total of nine graphs were plotted. In illustrating the relationship of solar radio flux and solar flares, it can be explained by studying the range values of flux corresponding to flares values. From this case study, it was found that the minimum value of solar radio flux in order for the flares to occur is equivalent 68 x 10-22Wm-2Hz-1. Thus, whenever the values of solar radio flux are high, there should be a higher number of flares produced by the sun. The overall range of solar radio flux recorded in this study ranging from 68 x 10-22 Wm-2Hz-1 to 96 x 10-22 Wm-2Hz-1. Observing and collecting data from the Sun and develop our very own new prediction methods will leads the accuracy of the prediction of the behavior of the Sun more precisely.

6

Scenario of Solar Radio Burst Type III During Solar Eclipse on 14th November 2012

Hamidi Z. S., Shariff N. N. M., Monstein C.

International Letters of Chemistry, Physics and Astronomy

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2014

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Vol. 13, iss. 2

135--143

EN

A compact solar flare was observed during a total solar eclipse event on 13-14 November 2012. This phenomenon is beginning in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. During the eclipse, the highest magnitude was 1.0500, occurring only 12 hours before perigee, with the maximum eclipse totality lasting just over four minutes. Considering the observational facts, the solar radio burst type III can be detected from the National Space Centre Malaysia by the Compound Low Cost Low Frequency Transportable Observatory (CALLISTO) system from 00:00 UT –1:30 UT. The group and individual solar burst type III can be detected in the region of 150-400 MHz. However, the eclipse cannot be observed from our site. From the observation, it was found that the eruption in the active region is becoming more active with a tens of groups solar radio burst type III can be observed. It continuing bursting within the first one hour. The sunspot number exceeds to 108 and solar wind speed 454.9 km/sec. Still the Sun remains active and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles.

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Measurements of the ionosphere plasma electron density variation by the Kharkov incoherent scatter radar

Cherniak I., Lysenko V.

Acta Geophysica

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2013

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Vol. 61, no. 5

1289--1303

EN

The present paper is devoted to the description of an improved method for determination of the ionospheric electron density values by Kharkov Incoherent Scatter Radar. This method allows to improve the resolution of the incoherent signals parameters up to ∼20 km in the range of 100–400 km and ∼100 km in the range of 200–1100 km. This approach was used to investigate variability of the ionospheric electron density over East European region in the heights interval of 100–1000 km during the period from 2003 to 2008, including case-studies of solar eclipses and ionospheric storms.