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Journal articles on the topic 'Solar'

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Author: Grafiati

Published: 4 June 2021

Last updated: 8 June 2024

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1

Manchandani, Hanshul. "Space based solar power versus ground based solar power." International Journal of Research and Engineering 4, no. 11 (December 13, 2017): 260–62. http://dx.doi.org/10.21276/ijre.2017.4.11.1.

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2

Changhui Rao, Changhui Rao, Lei Zhu Lei Zhu, Xuejun Rao Xuejun Rao, Lanqiang Zhang Lanqiang Zhang, Hua Bao Hua Bao, Lin Kong Lin Kong, Youming Guo Youming Guo, et al. "Second generation solar adaptive optics for 1-m New Vacuum Solar Telescope at the Fuxian Solar Observatory." Chinese Optics Letters 13, no. 12 (2015): 120101–3. http://dx.doi.org/10.3788/col201513.120101.

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3

Shukla, Utkarsh. "Solar Autopilot Drone." Journal of Advanced Research in Power Electronics and Power Systems 07, no. 1&2 (May 13, 2020): 13–23. http://dx.doi.org/10.24321/2456.1401.202003.

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Advances in technology have made the drone an affordable tool for various purposes. This article focuses on gaining knowledge of drone at a working and conceptual level. Firstly, there is a detailed explanation of the construction of the drone. Some of the most essential elements of a drone include frame, propellers, engine, system of power the electronic control and communication system. Whether you fly your drone for commercial or recreational purposes, staying in the air as long as possible is the goal. But of course, the battery life of the drone can put a damper on how much you can accomplish while you’re flying.Batteries serve as a major drawback because they get exhausted after 15 minutes of flight and thereby landing the drone on ground. The batteries used for powering the drones are lithium-polymer batteries.This project aims to provide an ingenious solution to this hurdle by introducing the current popular photovoltaic system into the UAV power system design.Solar drones use solar cells powered directly from the sun and solve major issues related to conventional drones such as increasing the flight time and risk of the drone losing connectivity with its controller. The design is to be modular for easy module upgrade and replacement. Using photovoltaic system minimizes the environmental impact, an issue that can be controversial for large projects built for utilities because they tend to spread across hundreds of acres of land in remote regions.

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4

P.L.Verma, P. L. Verma, Anita Shukla, and Prabhat Pandey. "Solar Cycle Variability of Solar Activity Parameters and Cosmic Ray Intensity." International Journal of Scientific Research 3, no. 3 (June 1, 2012): 1–4. http://dx.doi.org/10.15373/22778179/march2014/138.

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5

Yermolaev, Yuri, Irina Lodkina, Aleksander Khokhlachev, Michael Yermolaev, Maria Riazantseva, Liudmila Rakhmanova, Natalia Borodkova, Olga Sapunova, and Anastasiia Moskaleva. "Solar wind parameters in rising phase of solar cycle 25: Similarities and differences with solar cycles 23 and 24." Solar-Terrestrial Physics 9, no. 4 (December 28, 2023): 55–62. http://dx.doi.org/10.12737/stp-94202307.

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Solar activity and solar wind parameters decreased significantly in solar cycles (SCs) 23–24. In this paper, we analyze solar wind measurements at the rising phase of SC 25 and compare them with similar data from the previous cycles. For this purpose, we simultaneously selected the OMNI database data for 1976–2022, both by phases of the 11-year solar cycle and by large-scale solar wind types (in accordance with catalog [http://www.iki.rssi.ru/pub/omni]), and calculated the mean values of the plasma and magnetic field parameters for the selected datasets. The obtained results support the hypothesis that the continuation of this cycle will be similar to that of cycle 24, i.e. SC 25 will be weaker than SCs 21 and 22

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6

Atallah Aljubourya, Dheeaa Al Deen, Puganeshwary Palaniandy, Hamidi Bin Abdul Aziz, and Shaik Feroz. "Comparative Study of Advanced Oxidation Processes to Treat Petroleum Wastewater." Hungarian Journal of Industry and Chemistry 43, no. 2 (October 1, 2015): 97–101. http://dx.doi.org/10.1515/hjic-2015-0016.

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AbstractThis study was carried out to compare the performance of different oxidation processes, such as solar photo-Fenton reaction, solar photocatalysis by TiO2, and the combination of the two for the treatment of petroleum wastewater from Sohar Oil Refinery by a central composite design with response surface methodology. The degradation efficiency was evaluated in terms of chemical oxygen demand (COD) and total organic carbon (TOC) reductions. Solar photocatalysis by the TiO2/Fenton method improved the performance of the photocatalyst at neutral pH for petroleum wastewater without the need to adjust the pH during this treatment. Under acidic conditions, the solar photo-Fenton process is more efficient than solar TiO2photocatalysis while it is less efficient under alkaline conditions. The TiO2dosage and pH are the two main factors that improved the TOC and COD reductions in the solar photocatalysis using combined TiO2/Fenton and the solar TiO2photocatalysis processes while the pH and H2O2concentration are the two key factors that affect the solar photo-Fenton process.

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7

Claus, Jurgen. "Solar Art: Solar Architecture." Leonardo 28, no. 3 (1995): 231. http://dx.doi.org/10.2307/1576080.

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8

Parker, E. N. "Solar Flares, the Solar Corona, and Solar Physics." Symposium - International Astronomical Union 195 (2000): 455–59. http://dx.doi.org/10.1017/s007418090016348x.

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The Sun serves as the local physics laboratory for studying the suprathermal activity phenomena of stars. Scrutiny of the Sun has led to the discovery of a host of previously unknown physical effects, largely within the classical physics of Newton and Maxwell, but including quantum mechanics and lepton physics as well.

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9

Chaplin, W. J., Y. Elsworth, B. A. Miller, G. A. Verner, and R. New. "Solarp‐Mode Frequencies over Three Solar Cycles." Astrophysical Journal 659, no. 2 (April 20, 2007): 1749–60. http://dx.doi.org/10.1086/512543.

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10

Rosana, N. T. Mary, and Joshua Amarnath . D. "Dye Sensitized Solar Cells for The Transformation of Solar Radiation into Electricity." Indian Journal of Applied Research 4, no. 6 (October 1, 2011): 169–70. http://dx.doi.org/10.15373/2249555x/june2014/53.

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11

Kirichenko, Aleksey, Ivan Loboda, Anton Reva, Artyom Ulyanov, and Sergey Bogachev. "Latitudinal distribution of solar microflares and high-temperature plasma at solar minimum." Solar-Terrestrial Physics 9, no. 2 (June 29, 2023): 3–8. http://dx.doi.org/10.12737/stp-92202301.

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The paper analyzes the latitudinal distribution of high-temperature plasma (T>4 MK) and microflares on the solar disk during low solar activity in 2009. The distribution of A0.1–A1.0 microflares contains belts typical of ordinary flares of B class and higher. In total, we have registered 526 flares, most of which, about 96 %, occurred at high latitudes. About 4 % of microflares were found near the solar equator. We believe that they were formed by the residual magnetic field of previous solar cycle 23. Ordinary flares were almost not observed near the equator during this period. The number of microflares in the southern hemisphere was slightly higher than in the northern one. This differs from the distribution of ordinary flares for which the northern hemisphere was previously reported to be dominant.

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12

Смирнов, Владимир, Vladimir Smirnov, Елена Смирнова, and Elena Smirnova. "Ionospheric effects of two solar flares in the maximum of solar cycle 23 and in the minimum of solar cycle 24." Solar-Terrestrial Physics 5, no. 2 (June 28, 2019): 76–80. http://dx.doi.org/10.12737/stp-52201911.

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Using data from the GPS and GLONASS navigation satellite systems, we analyze the responses of the mid-latitude ionosphere to the extreme solar flares that occurred at the maximum of solar cycle 23 (October 28, 2003) and at the minimum of solar cycle 24 (September 6, 2017) during the same season at close solar zenith angles. To obtain the response, we use the rate of change of the total electronic content, which is practically independent of characteristics of equipment and is determined only by parameters of a propagation medium (the ionosphere in our case). The ionospheric response is shown to be almost independent of the total duration of the flare. In both cases, the duration of the main response at a level of 0.5 is about 1.5–2 min, whereas the total duration of the response is about 10 min and fairly independent of solar flare importance.

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13

Skokić, Ivica, and Roman Brajša. "ALMA SOLAR EPHEMERIS GENERATOR." Rudarsko-geološko-naftni zbornik 34, no. 2 (2019): 59–65. http://dx.doi.org/10.17794/rgn.2019.2.7.

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14

Sadykova, S. B., M. Yerkalina, M. G. Zhumagulov, and N. R. Kartjanov. "Solar-powered water desalination." BULLETIN of L.N. Gumilyov Eurasian National University. Technical Science and Technology Series 130, no. 1 (2020): 66–70. http://dx.doi.org/10.32523/2616-68-36-2020-130-1-66-70.

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15

Taheem, Anubhav. "Solar Tracker: A Review." Journal of Advanced Research in Alternative Energy, Environment and Ecology 06, no. 3&4 (December 25, 2019): 34–50. http://dx.doi.org/10.24321/2455.3093.201905.

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16

Ugale, Prof Monica, Reva Gandhi, Pavneet Singh, Shreya Shankar, Vanshay Narang, and Saurav Singh. "Dual Axis Solar Tracker." International Journal of Research Publication and Reviews 4, no. 5 (May 2023): 6765–69. http://dx.doi.org/10.55248/gengpi.4.523.44612.

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17

Pathare, Prof N. R., Jyothprakash Beshetty, Kartikkumar Bawankar, Nandkishor Ghagare, Sumit Rangari, and Vicky Kashyap. "Development of Solar Tree." International Journal of Research Publication and Reviews 5, no. 5 (May 7, 2024): 6345–51. http://dx.doi.org/10.55248/gengpi.5.0524.1278.

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18

Richardson, John D., Chi Wang, and Karolen I. Paularena. "The solar wind: from solar minimum to solar maximum." Advances in Space Research 27, no. 3 (January 2001): 471–79. http://dx.doi.org/10.1016/s0273-1177(01)00074-6.

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19

Cox, Arthur N. "Solar Opacities Constrained by Solar Neutrinos and Solar Oscillations." International Astronomical Union Colloquium 121 (1990): 61–80. http://dx.doi.org/10.1017/s0252921100067828.

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AbstractThis review discusses the current situation for opacities at the solar center, the solar surface, and for the few million kelvin temperatures that occur below the convection zone. The solar center conditions are important because they are crucial for the neutrino production, which continues to be predicted about 4 times that observed. The main extinction effects there are free-free photon absorption in the electric fields of the hydrogen, helium and the CNO atoms, free electron scattering of photons, and the bound-free and bound-bound absorption of photons by iron atoms with two electrons in the 1s bound level. An assumption that the iron is condensed-out below the convection zone, and the opacity in the central regions is thereby reduced, results in about a 25 percent reduction in the central opacity but only a 5 percent reduction at the base of the convection zone. Furthermore, the p-mode solar oscillations are changed with this assumption, and do not fit the observed ones as well as for standard models. A discussion of the large effective opacity reduction by weakly interacting massive particles (WIMPs or Cosmions) also results in poor agreement with observed p-mode oscillation frequencies. The much larger opacities for the solar surface layers from the Los Alamos Astrophysical Opacity Library instead of the widely used Cox and Tabor values show small improvements in oscillation frequency predictions, but the largest effect is in the discussion of p-mode stability. Solar oscillation frequencies can serve as an opacity experiment for the temperatures and densities, respectively, of a few million kelvin and between 0.1 and 10 g/cm3. Current oscillation frequency calculations indicate that possibly the Opacity Library values need an increase of typically 15 percent just at the bottom of the convection zone at 3×106K. Opacities have uncertainties at the photosphere and deeper than the convection zone ranging from 10 to 25 percent. The equation of state that supplies data for the opacity calculations fortunately has pressure uncertainties of only about 1 percent, but opacity uncertainties will always be much larger. A discussion is given about opacity experiments that the stars provide. Opacities in the envelopes of the Hyades G stars, the Cepheids, δ Scuti variables, and the β Cephei variables indicate that significantly larger opacities, possibly caused by iron lines, seem to be required.

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20

Rohini V S and Ravi chimmalgi. "Delay analysis." international journal of engineering technology and management sciences 6, no. 6 (November 28, 2022): 137–42. http://dx.doi.org/10.46647/ijetms.2022.v06i06.022.

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TSSA and CTSI shows delay or lag wrt each other1,3,5. Solar cycle data (21,22,23) is used in the analysis and possible correlation between H alpha flare index and delay is worked out .It is found that these two parameters are anti correlated with a correlation factor of 0.8 9427 . The 27day solar activity shows heighest correlation factor. A new parameter called delay index number (DI) is defined.This paramter shows two sharp peaks wrt delay event number ,during the span of solar cycle 21,22,23. The peaks fall in soalr quite period 1986 and 1996. Thus D I acts as an indicator of quite phase (ie solar minima )of sun.The possible cause for sharp shoot up is under investigation.

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21

Kichigin, Gennadiy, Marina Kravtsova, and Valeriy Sdobnov. "Conditions for arrival of solar energetic protons in Earth after strong solar flares." Solar-Terrestrial Physics 8, no. 3 (September 30, 2022): 22–26. http://dx.doi.org/10.12737/stp-83202203.

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We analyze the Sun-to-Earth transport of energetic protons accelerated in solar flares. We use a model which assumes that protons move earthward in the Parker electromagnetic field. In this model, protons are shown to be recorded on Earth when they, moving away from the solar flare region, reach the vicinity of the heliospheric current sheet, while Earth is at a distance smaller than the proton Larmor radius from the current sheet neutral line. We present the analysis of experimental data on solar flares in August–September 2011. This analysis shows that the absence of energetic protons recording in the vicinity of Earth for some major solar flares can be explained by the proposed model.

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22

Ганхуа, Линь, Lin Ganghua, Ван Сяо-Фань, Wang Xiao Fan, Ян Сяо, Yang Xiao, Лю Со, et al. "Construction of a century solar chromosphere data set for solar activity related research." Solar-Terrestrial Physics 3, no. 2 (August 9, 2017): 5–8. http://dx.doi.org/10.12737/stp-3220171.

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This article introduces our ongoing project “Construction of a Century Solar Chromosphere Data Set for Solar Activity Related Research”. Solar activities are the major sources of space weather that affects human lives. Some of the serious space weather consequences, for instance, include interruption of space communication and navigation, compromising the safety of astronauts and satellites, and damaging power grids. Therefore, the solar activity research has both scientific and social impacts. The major database is built up from digitized and standardized film data obtained by several observatories around the world and covers a timespan more than 100 years. After careful calibration, we will develop feature extraction and data mining tools and provide them together with the comprehensive database for the astronomical community. Our final goal is to address several physical issues: filament behavior in solar cycles, abnormal behavior of solar cycle 24, large-scale solar eruptions, and sympathetic remote brightenings. Significant progresses are expected in data mining algorithms and software development, which will benefit the scientific analysis and eventually advance our understanding of solar cycles.

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23

Ma, Dongling. "Solar Energy and Solar Cells." Nanomaterials 11, no. 10 (October 12, 2021): 2682. http://dx.doi.org/10.3390/nano11102682.

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Thanks to the helpful discussions and strong support provided by the Publisher and Editorial Staff of Nanomaterials, I was appointed as a section Editor-in-Chief of the newly launched section “Solar Energy and Solar Cells” earlier this year (2021) [...]

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24

Bahcall, J. N. "Solar Models and Solar Neutrinos." Physica Scripta T121 (January 1, 2005): 46–50. http://dx.doi.org/10.1088/0031-8949/2005/t121/006.

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25

Barnard, Luke, Chris Scott, Matt Owens, Mike Lockwood, Kim Tucker-Hood, Julia Wilkinson, Briana Harder, and Elisabeth Baeten. "Solar Stormwatch: tracking solar eruptions." Astronomy & Geophysics 56, no. 4 (July 22, 2015): 4.20–4.24. http://dx.doi.org/10.1093/astrogeo/atv131.

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26

Herbst, Dianna. "Solar mapping: demystifying solar potential." Renewable Energy Focus 10, no. 4 (July 2009): 32–35. http://dx.doi.org/10.1016/s1755-0084(09)70150-4.

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27

Turck-Chièze, S. "Solar models and solar neutrinos." Nuclear Physics B - Proceedings Supplements 145 (August 2005): 17–22. http://dx.doi.org/10.1016/j.nuclphysbps.2005.03.026.

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28

Elsworth, Y. "Solar activity and solar oscillations." Symposium - International Astronomical Union 181 (1997): 277–85. http://dx.doi.org/10.1017/s0074180900061210.

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Helioseismology provides us with the tools to probe solar activity. So that we can consider how the solar oscillations are influenced by that activity, we first consider the phenomena that we associate with the active Sun. The surface of the Sun is not quiet but shows evidence of convection on a wide range of scales from a few hundred kilometres through to several tens-of-thousands of kilometres. The surface temperature shows signs of the convection structures with the temperature in the bright granules being some 100 K to 200 K hotter than the surrounding dark lanes. Sunspots, which are regions of high magnetic field that suppress convective flows, are clearly visible to even quite crude observations. They are several tens-of-thousands of kilometres in diameter and about 2000 K cooler than their surroundings. Ultraviolet and X-ray pictures from satellites show that the higher layers of the solar atmosphere are very non-uniform with bright regions of high activity. Contemporaneous magnetograms show that these regions are associated with sunspots. Flares - regions of magnetic reconnections - are seen at all wavelengths from X-ray through the visible to radio. They are the non-thermal component of the radio emission of the Sun. There are many other indicators of activity on the Sun.

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29

Harrison, R. A. "Solar corona and solar wind." Planetary and Space Science 40, no. 4 (April 1992): 592–93. http://dx.doi.org/10.1016/0032-0633(92)90277-u.

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30

ZIRKER, J. B. "Solar Astronomy: Solar Maximum Analysis." Science 230, no. 4726 (November 8, 1985): 660. http://dx.doi.org/10.1126/science.230.4726.660.

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31

WORTHY, WARD. "Solar." Chemical & Engineering News 69, no. 24 (June 17, 1991): 41–46. http://dx.doi.org/10.1021/cen-v069n024.p041.

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32

Reggiani, N., M. M. Guzzo, and P. C. de Holanda. "MHD solar fluctuations and solar neutrinos." Brazilian Journal of Physics 33, no. 4 (December 2003): 707–74. http://dx.doi.org/10.1590/s0103-97332003000400028.

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33

San Vicente González de Aspuru, Jose Ignacio. "Nerón, auriga solar = Nero, solar auriga." ARYS: Antigüedad, Religiones y Sociedades, no. 15 (November 5, 2018): 187. http://dx.doi.org/10.20318/arys.2017.3840.

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Resumen: Se analiza la trayectoria de Nerón como auriga. Esta actividad estaba mal considerada por relacionarse con ‘gente infame’, pero Nerón defendió su afición argumentando que la antigua tradición de la conducción de carros era propia de reyes y héroes. Su inclinación le venía de herencia familiar, ya que algunos Ahenobarbos habían practicado la conducción de carros. Nerón se preparó para este deporte y actuó en el circo como auriga. Lo hizo en un principio de manera privada, hasta que a partir del año 64 participó en espectáculos públicos. En su papel de conductor de carros de caballos terminó identificándose con Febo, el Sol, y se hizo representar en las monedas y esculturas con la corona radiada. Esta innovación tuvo éxito y el tocado solar permaneció en las imágenes monetales de los emperadores hasta el Bajo Imperio.Abstract: We analyze Nero´s trajectory as a charioteer. This activity was badly considered for being related to 'infamous people', but Nero defended his hobby by arguing that the ancient tradition of car driving was typical of kings and heroes. His interest came from family tradition, since some Ahenobarbi had practiced the driving of cars. Nero trained for this sport and performed in circus as a charioteer. At first he did it privately until 64 A.D., when he started to participate in public shows. In his role of horse carriages driver, he ended up identifying himself with Phoebus, the Sun, and was represented in coins and sculptures with the radiated crown. This innovation was successful and the headdress remained in monetary images of the emperors until the Late Empire.Palabras clave: Cuadriga, Apolo, Febo, Sol, Olimpia, Circo Máximo.Key words: Quadriga, Apollo, Phoebus, Sol, Olympia, Circus Maximus.

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34

Zhou, Zhiguang, Enas Sakr, Yubo Sun, and Peter Bermel. "Solar thermophotovoltaics: reshaping the solar spectrum." Nanophotonics 5, no. 1 (June 1, 2016): 1–21. http://dx.doi.org/10.1515/nanoph-2016-0011.

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Abstract Recently, there has been increasing interest in utilizing solar thermophotovoltaics (STPV) to convert sunlight into electricity, given their potential to exceed the Shockley-Queisser limit. Encouragingly, there have also been several recent demonstrations of improved system-level efficiency as high as 6.2%. In this work, we review prior work in the field, with particular emphasis on the role of several key principles in their experimental operation, performance, and reliability. In particular, for the problem of designing selective solar absorbers, we consider the trade-off between solar absorption and thermal losses, particularly radiative and convective mechanisms. For the selective thermal emitters, we consider the tradeoff between emission at critical wavelengths and parasitic losses. Then for the thermophotovoltaic (TPV) diodes, we consider the trade-off between increasing the potential short-circuit current, and maintaining a reasonable opencircuit voltage. This treatment parallels the historic development of the field, but also connects early insights with recent developments in adjacent fields.With these various components connecting in multiple ways, a system-level end-to-end modeling approach is necessary for a comprehensive understanding and appropriate improvement of STPV systems. This approach will ultimately allow researchers to design STPV systems capable of exceeding recently demonstrated efficiency values.

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35

Bahcall, John N., and Carlos Peña-Garay. "Solar models and solar neutrino oscillations." New Journal of Physics 6 (June 17, 2004): 63. http://dx.doi.org/10.1088/1367-2630/6/1/063.

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36

Mathew, Xavier. "Solar cells and solar energy materials." Solar Energy 80, no. 2 (February 2006): 141. http://dx.doi.org/10.1016/j.solener.2005.06.001.

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37

Gough, D. O. "Solar and Solar-Like Oscillations: Theory." Highlights of Astronomy 7 (1986): 283–93. http://dx.doi.org/10.1017/s1539299600006559.

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AbstractSolar five-minute oscillations provide a means of testing theoretical models of the sun. By judiciously combining data from low-degree modes, properties of the central and surface regions of the sun can be inferred separately. In principle, it should be possible to draw similar inferences from other stars, once adequate data are available. Recent solar rotational splitting data imply that in the equatorial regions much of the radiative envelope of the sun is rotating more slowly than the photosphere.

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38

Sofia, Sabatino, and Andrew S. Endal. "The solar-stellar connection - Solar studies." Publications of the Astronomical Society of the Pacific 99 (December 1987): 1241. http://dx.doi.org/10.1086/132109.

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39

Blizard, J. B. "Solar Inertial Motion and Solar Activity." Publications of the Astronomical Society of the Pacific 100 (October 1988): 1216. http://dx.doi.org/10.1086/132295.

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40

Ricci, B., and G. Fiorentini. "Helioseismology, solar models and solar neutrinos." Nuclear Physics B - Proceedings Supplements 81 (February 2000): 95–101. http://dx.doi.org/10.1016/s0920-5632(99)00864-6.

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41

Nocera, Daniel G. "Solar Fuels and Solar Chemicals Industry." Accounts of Chemical Research 50, no. 3 (March 21, 2017): 616–19. http://dx.doi.org/10.1021/acs.accounts.6b00615.

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42

WIENS, R., P. BOCHSLER, D. BURNETT, and R. WIMMERSCHWEINGRUBER. "Solar and solar wind isotopic compositions." Earth and Planetary Science Letters 226, no. 3-4 (October 15, 2004): 549–65. http://dx.doi.org/10.1016/s0012-821x(04)00431-5.

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43

Schatten, K. H. "Solar activity and the solar cycle." Advances in Space Research 32, no. 4 (August 2003): 451–60. http://dx.doi.org/10.1016/s0273-1177(03)00328-4.

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44

Ribes, Elisabeth, Istvan Vince, Pierre Mein, and Eduardo Neto Ferreira. "Solar Rotation over Solar Cycle 21." International Astronomical Union Colloquium 130 (1991): 241–45. http://dx.doi.org/10.1017/s0252921100079690.

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Abstract Having measured the rotation rate of sunspots through solar cycle 21, from 1977 to 1983, we have found that the mean differential rotation averaged over this seven year record is similar to the grand average differential rotation determined by Howard et al. (1984) over the period 1921-1982. However, the rotation rate does change from year to year. These changes are evidenced by a steepening or a flattening of the mean differential rotation profile, as well as significant changes in the equatorial rate. The presence of a time-dependent pattern of azimuthal rolls inferred from the meridional circulation pattern of the sunspots offers a qualitative explanation of the observed rotation rates. The amplitude of the changes is almost one order of magnitude larger than that of the torsional oscillations found by Howard and LaBonte (1981).

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45

Graetzel, Michael. "Editorial: Solar Cells and Solar Fuels." Current Opinion in Electrochemistry 2, no. 1 (April 2017): A4. http://dx.doi.org/10.1016/j.coelec.2017.05.005.

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46

Mutalikdesai, Amruta, and Sheela K. Ramasesha. "Emerging solar technologies: Perovskite solar cell." Resonance 22, no. 11 (November 2017): 1061–83. http://dx.doi.org/10.1007/s12045-017-0571-1.

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Wiens, Roger C., Peter Bochsler, Donald S. Burnett, and Robert F. Wimmer-Schweingruber. "Solar and solar-wind isotopic compositions." Earth and Planetary Science Letters 222, no. 3-4 (June 15, 2004): 697–712. http://dx.doi.org/10.1016/j.epsl.2004.03.025.

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Yeo, K. L., N. A. Krivova, and S. K. Solanki. "Solar Cycle Variation in Solar Irradiance." Space Science Reviews 186, no. 1-4 (July 4, 2014): 137–67. http://dx.doi.org/10.1007/s11214-014-0061-7.

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Castellani, V., S. Degl'Innocenti, G. Fiorentini, M. Lissia, and B. Ricci. "Solar neutrinos: beyond standard solar models." Physics Reports 281, no. 5-6 (March 1997): 309–98. http://dx.doi.org/10.1016/s0370-1573(96)00032-4.

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Mohan, Brindha V. G., V. Vasu, V. Vasu, A. Robson Benjamin, and M. Kottaisamy. "Luminescent Solar Concentrators – The Solar Waveguides." Current Science 114, no. 08 (April 25, 2018): 1656. http://dx.doi.org/10.18520/cs/v114/i08/1656-1664.

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