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Journal articles on the topic 'Space and Solar Physics'

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Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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1

Kuznetsov, V. D., and L. M. Zelenyi. "Space projections on solar-terrestrial physics." Geomagnetism and Aeronomy 49, no. 8 (December 2009): 1137–47. http://dx.doi.org/10.1134/s0016793209080209.

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2

Krimigis, S. M. "Committee on Solar and Space Physics." Eos, Transactions American Geophysical Union 67, no. 33 (1986): 635. http://dx.doi.org/10.1029/eo067i033p00635-01.

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3

Simarski, L. "NRC assesses solar and space physics." Eos, Transactions American Geophysical Union 72, no. 35 (1991): 371. http://dx.doi.org/10.1029/90eo00280.

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4

Gómez, Daniel, Luis N. Martín, and Pablo Dmitruk. "Magnetohydrodynamics in solar and space physics." Advances in Space Research 51, no. 10 (May 2013): 1916–23. http://dx.doi.org/10.1016/j.asr.2012.09.016.

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5

Grigoryev, V. M. "A space-borne solar stereoscope experiment in solar physics." Solar Physics 148, no. 2 (December 1993): 389–91. http://dx.doi.org/10.1007/bf00645098.

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6

Rutten, Robert J., and Luc Damé. "SIMURIS: High-Resolution Solar Physics." International Astronomical Union Colloquium 141 (1993): 184–87. http://dx.doi.org/10.1017/s0252921100029055.

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AbstractThe magnetic fields of the Sun provide the major incentive to do solar physics. The small spatial extent of the magnetically constrained structures and processes in the solar atmosphere provide the major incentive for high resolution solar telescopes. The visibility of the outer solar atmosphere in the ultraviolet and X-ray domains provide the major incentive for solar space telescopes. Cost provides the major incentive to use interferometric techniques. SIMURIS employs short-wave interferometry from space to measure solar structures and processes with high resolution.
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7

Hill, Frank. "Solar physics with the Virtual Solar Observatory." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 612. http://dx.doi.org/10.1017/s1743921307012100.

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The Virtual Solar Observatory (VSO) is a lightweight web service unifying twelve major solar data archives. With the VSO, users can simultaneously search for data from 50 space- and ground-based instruments covering the time period from 1915 to the present.
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8

Domingo, V. "Helioseismology from space, the SOHO project." Symposium - International Astronomical Union 123 (1988): 545–48. http://dx.doi.org/10.1017/s007418090015867x.

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As a cornerstone of its long term plan for space science research, the European Space Agency (ESA) is developing the Solar Terrestrial Physics Programme that consists of two parts: one, the Solar and Heliospheric Observatory (SOHO) for the study of the solar internal structure and the physics of the solar corona and the solar wind, and another, CLUSTER, a series of four spacecraft flying in formation to study small scale plasma phenomena in several regions of the magnetosphere and in the near Earth solar wind. The feasibility of the missions was demonstrated in Phase A studies carried out by industrial consortia under the supervision of ESA (1,2). According to the current plans an announcement of opportunity calling for instrument proposals will be issued by ESA during the first quarter of 1987. It is foreseen that the spacecraft will be launched by the end of 1994.
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9

Lanzerotti, L. J. "International Cooperation in Solar and Space Physics." Eos, Transactions American Geophysical Union 66, no. 1 (1985): 1. http://dx.doi.org/10.1029/eo066i001p00001-02.

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10

Harley, Phil. "Space-based solar." Physics World 35, no. 11 (December 1, 2022): 25iii—26i. http://dx.doi.org/10.1088/2058-7058/35/11/25.

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11

Doschek, G. A. "Recent Advances in EUV Solar Astronomy." International Astronomical Union Colloquium 152 (1996): 503–10. http://dx.doi.org/10.1017/s0252921100036460.

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I discuss recent advances in EUV solar astronomy. The new work is primarily a result of current solar space missions such as the Yohkoh high energy solar physics mission, as well as upcoming space missions such as the ESA Solar and Heliospheric Observatory (SOHO). I discuss spectroscopic and atomic physics work, and new results concerning solar flares that are directly relevant to stellar research.
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12

Wing, Simon, and Jay R. Johnson. "Applications of Information Theory in Solar and Space Physics." Entropy 21, no. 2 (February 1, 2019): 140. http://dx.doi.org/10.3390/e21020140.

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Characterizing and modeling processes at the sun and space plasma in our solar system are difficult because the underlying physics is often complex, nonlinear, and not well understood. The drivers of a system are often nonlinearly correlated with one another, which makes it a challenge to understand the relative effects caused by each driver. However, entropy-based information theory can be a valuable tool that can be used to determine the information flow among various parameters, causalities, untangle the drivers, and provide observational constraints that can help guide the development of the theories and physics-based models. We review two examples of the applications of the information theoretic tools at the Sun and near-Earth space environment. In the first example, the solar wind drivers of radiation belt electrons are investigated using mutual information (MI), conditional mutual information (CMI), and transfer entropy (TE). As previously reported, radiation belt electron flux (Je) is anticorrelated with solar wind density (nsw) with a lag of 1 day. However, this lag time and anticorrelation can be attributed mainly to the Je(t + 2 days) correlation with solar wind velocity (Vsw)(t) and nsw(t + 1 day) anticorrelation with Vsw(t). Analyses of solar wind driving of the magnetosphere need to consider the large lag times, up to 3 days, in the (Vsw, nsw) anticorrelation. Using CMI to remove the effects of Vsw, the response of Je to nsw is 30% smaller and has a lag time <24 h, suggesting that the loss mechanism due to nsw or solar wind dynamic pressure has to start operating in <24 h. Nonstationarity in the system dynamics is investigated using windowed TE. The triangle distribution in Je(t + 2 days) vs. Vsw(t) can be better understood with TE. In the second example, the previously identified causal parameters of the solar cycle in the Babcock–Leighton type model such as the solar polar field, meridional flow, polar faculae (proxy for polar field), and flux emergence are investigated using TE. The transfer of information from the polar field to the sunspot number (SSN) peaks at lag times of 3–4 years. Both the flux emergence and the meridional flow contribute to the polar field, but at different time scales. The polar fields from at least the last 3 cycles contain information about SSN.
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13

GAN, Weiqun, Jin CHANG, and Yuqian MA. "40 Years of Space Solar Physics in China." Chinese Journal of Space Science 41, no. 01 (January 1, 2021): 76–83. http://dx.doi.org/10.3724/sp.j.0254-6124.2021.0107.

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14

Zelenyi, L. M., V. D. Kuznetsov, Yu D. Kotov, A. A. Petrukovich, M. M. Mogilevsky, K. A. Boyarchuk, G. N. Zastenker, and Yu I. Yermolaev. "Russian Space Program: Experiments in Solar-Terrestrial Physics." Proceedings of the International Astronomical Union 2004, IAUS223 (June 2004): 573–80. http://dx.doi.org/10.1017/s1743921304006921.

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15

Harvey, Christopher C., Michel Gangloff, Todd King, Christopher H. Perry, D. Aaron Roberts, and James R. Thieman. "Virtual observatories for space and solar physics research." Earth Science Informatics 1, no. 1 (April 2008): 5–13. http://dx.doi.org/10.1007/s12145-008-0008-1.

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16

Li, Yangfeng, Wenqi Wang, Chen Yue, Xiaotao Hu, Yimeng Song, Zaole Su, Haiqiang Jia, Wenxin Wang, Yang Jiang, and Hong Chen. "Enhanced absorption in the space charge region of GaAs solar cells." Europhysics Letters 136, no. 3 (November 1, 2021): 37002. http://dx.doi.org/10.1209/0295-5075/ac3cd1.

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Abstract The photo-generated currents of GaAs solar cells with different lengths of space charge region are obtained and analyzed in this study. The enhanced absorption coefficient in the space charge region is adopted to calculate the photo-generated current based on the solar cell physics theory. The calculated currents coincide well with the experimental currents both under single wavelength incidence and solar spectrum irradiation conditions.
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17

Archontis, Vasilis, and Loukas Vlahos. "Introduction to the physics of solar eruptions and their space weather impact." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2148 (May 13, 2019): 20190152. http://dx.doi.org/10.1098/rsta.2019.0152.

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The physical processes, which drive powerful solar eruptions, play an important role in our understanding of the Sun–Earth connection. In this Special Issue, we firstly discuss how magnetic fields emerge from the solar interior to the solar surface, to build up active regions, which commonly host large-scale coronal disturbances, such as coronal mass ejections (CMEs). Then, we discuss the physical processes associated with the driving and triggering of these eruptions, the propagation of the large-scale magnetic disturbances through interplanetary space and the interaction of CMEs with Earth's magnetic field. The acceleration mechanisms for the solar energetic particles related to explosive phenomena (e.g. flares and/or CMEs) in the solar corona are also discussed. The main aim of this Issue, therefore, is to encapsulate the present state-of-the-art in research related to the genesis of solar eruptions and their space-weather implications. This article is part of the theme issue ‘Solar eruptions and their space weather impact’.
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18

Sturrock, P. A. "Solar Neutrino Variability and Its Implications for Solar Physics and Neutrino Physics." Astrophysical Journal 688, no. 1 (October 23, 2008): L53—L56. http://dx.doi.org/10.1086/594993.

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19

Showstack, Randy. "Solar and space physics decadal strategy outlines key recommendations." Eos, Transactions American Geophysical Union 93, no. 35 (August 28, 2012): 339. http://dx.doi.org/10.1029/2012eo350003.

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20

Stone, R. "SOLAR PHYSICS: A Space Weather Aerie in the Caucasus?" Science 301, no. 5637 (August 29, 2003): 1175–76. http://dx.doi.org/10.1126/science.301.5637.1175.

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21

WeiQun, GAN, YAN YiHua, and HUANG Yu. "Prospect for space solar physics in 2016–2030." SCIENTIA SINICA Physica, Mechanica & Astronomica 49, no. 5 (January 8, 2019): 059602. http://dx.doi.org/10.1360/sspma2018-00301.

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22

Chilingarian, A. A., and A. E. Reymers. "Particle detectors in solar physics and space weather research." Astroparticle Physics 27, no. 5 (June 2007): 465–72. http://dx.doi.org/10.1016/j.astropartphys.2007.02.001.

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23

Moldwin, Mark B., and Cherilynn Morrow. "Research Career Persistence for Solar and Space Physics PhD." Space Weather 14, no. 6 (June 2016): 384–90. http://dx.doi.org/10.1002/2016sw001382.

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24

Singh, Ashok Kumar, Asheesh Bhargawa, Devendraa Siingh, and Ram Pal Singh. "Physics of Space Weather Phenomena: A Review." Geosciences 11, no. 7 (July 8, 2021): 286. http://dx.doi.org/10.3390/geosciences11070286.

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In the last few decades, solar activity has been diminishing, and so space weather studies need to be revisited with more attention. The physical processes involved in dealing with various space weather parameters have presented a challenge to the scientific community, with a threat of having a serious impact on modern society and humankind. In the present paper, we have reviewed various aspects of space weather and its present understanding. The Sun and the Earth are the two major elements of space weather, so the solar and the terrestrial perspectives are discussed in detail. A variety of space weather effects and their societal as well as anthropogenic aspects are discussed. The impact of space weather on the terrestrial climate is discussed briefly. A few tools (models) to explain the dynamical space environment and its effects, incorporating real-time data for forecasting space weather, are also summarized. The physical relation of the Earth’s changing climate with various long-term changes in the space environment have provided clues to the short-term/long-term changes. A summary and some unanswered questions are presented in the final section.
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25

Vieira, L. E. A., A. L. Clúa de Gonzalez, A. Dal Lago, C. Wrasse, E. Echer, F. L. Guarnieri, F. Reis Cardoso, et al. "Preliminary design of the INPE's Solar Vector Magnetograph." Proceedings of the International Astronomical Union 10, S305 (December 2014): 195–99. http://dx.doi.org/10.1017/s1743921315004767.

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AbstractWe describe the preliminary design of a magnetograph and visible-light imager instrument to study the solar dynamo processes through observations of the solar surface magnetic field distribution. The instrument will provide measurements of the vector magnetic field and of the line-of-sight velocity in the solar photosphere. As the magnetic field anchored at the solar surface produces most of the structures and energetic events in the upper solar atmosphere and significantly influences the heliosphere, the development of this instrument plays an important role in reaching the scientific goals of The Atmospheric and Space Science Coordination (CEA) at the Brazilian National Institute for Space Research (INPE). In particular, the CEA's space weather program will benefit most from the development of this technology. We expect that this project will be the starting point to establish a strong research program on Solar Physics in Brazil. Our main aim is acquiring progressively the know-how to build state-of-the-art solar vector magnetograph and visible-light imagers for space-based platforms to contribute to the efforts of the solar-terrestrial physics community to address the main unanswered questions on how our nearby Star works.
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26

Gopalswamy, Nat, Pertti Mäkelä, Seiji Yashiro, Sachiko Akiyama, and Hong Xie. "Solar activity and space weather." Journal of Physics: Conference Series 2214, no. 1 (February 1, 2022): 012021. http://dx.doi.org/10.1088/1742-6596/2214/1/012021.

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Abstract After providing an overview of solar activity as measured by the sunspot number (SSN) and space weather events during solar cycles (SCs) 21-24, we focus on the weak solar activity in SC 24. The weak solar activity reduces the number of energetic eruptions from the Sun and hence the number of space weather events. The speeds of coronal mass ejections (CMEs), interplanetary (IP) shocks, and the background solar wind all declined in SC 24. One of the main heliospheric consequences of weak solar activity is the reduced total (magnetic + gas) pressure, magnetic field strength, and Alfvén speed. There are three groups of phenomena that decline to different degrees in SC 24 relative to the corresponding ones in SC 23: (i) those that decline more than SSN does, (ii) those that decline like SSN, and (iii) those that decline less than SSN does. The decrease in the number of severe space weather events such as high-energy solar energetic particle (SEP) events and intense geomagnetic storms is deeper than the decline in SSN. The reduction in the number of severe space weather events can be explained by the backreaction of the weak heliosphere on CMEs. CMEs expand anomalously and hence their magnetic content is diluted resulting in weaker geomagnetic storms. The reduction in the number of intense geomagnetic storms caused by corotating interaction regions is also drastic. The diminished heliospheric magnetic field in SC 24 reduces the efficiency of particle acceleration, resulting in fewer high-energy SEP events. The numbers of IP type II radio bursts, IP socks, and high-intensity energetic storm particle events closely follow the number of fast and wide CMEs (and approximately SSN) because all these phenomena are closely related to CME-driven shocks. The number of halo CMEs in SC 24 declines less than SSN does, mainly due to the weak heliospheric state. Phenomena such as IP CMEs and magnetic clouds related to frontside halos also do not decline significantly. The mild space weather is likely to continue in SC 25, whose strength has been predicted to be not too different from that of SC 24.
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27

Akasofu, Syun-Ichi. "A Short History of the Development of Space Physics Based on Studies of Geomagnetic Storms." Journal of Research in Philosophy and History 5, no. 1 (February 13, 2022): p39. http://dx.doi.org/10.22158/jrph.v5n1p39.

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Space physics is one of the rapidly developing scientific fields, covering space from the sun to a distance of about 100 times between the sun and the earth, the region called the heliosphere. It includes parts of solar physics, geomagnetism (a study of geomagnetic storms), ionospheric physics, auroral physics, cosmic ray physics and planetary physics. The rapid progress in space physics owes a long history of debates and controversies among these sub-fields, as well as the advent of satellites and space probs, which began during the 1960s. A study of geomagnetic storms has an interesting development preceding space physics, so that it may be worthwhile to study history of space physics by following the development of the history of geomagnetic storms. The author has joined in space physics in its earliest days.
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28

Gnedin, Yu N., A. A. Solov'ev, and S. V. Avakyan. "Space Solar Patrol and some fundamental questions of astrophysics, solar physics, and geophysics." Journal of Optical Technology 73, no. 4 (April 1, 2006): 218. http://dx.doi.org/10.1364/jot.73.000218.

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29

Abdusamatov, H. I. "Space-based solar limbograph." Journal of Optical Technology 73, no. 4 (April 1, 2006): 242. http://dx.doi.org/10.1364/jot.73.000242.

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30

Parker, E. N. "Solar Activity and Classical Physics." Chinese Journal of Astronomy and Astrophysics 1, no. 2 (April 2001): 99–124. http://dx.doi.org/10.1088/1009-9271/1/2/99.

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31

Leibacher, John, Takashi Sakurai, and Lidia van Driel-Gesztelyi. "Solar Physics Publication Ethics Policies." Solar Physics 260, no. 1 (November 2009): 1–3. http://dx.doi.org/10.1007/s11207-009-9477-8.

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32

Cliver, Ed, and Lidia van Driel-Gesztelyi. "Solar Physics Memoir Series Reinstituted." Solar Physics 267, no. 2 (November 6, 2010): 233–34. http://dx.doi.org/10.1007/s11207-010-9667-4.

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33

Švestka, Zdeněk. "Sixty Years in Solar Physics." Solar Physics 267, no. 2 (November 25, 2010): 235–50. http://dx.doi.org/10.1007/s11207-010-9675-4.

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34

Parker, E. N. "The future of solar physics." Solar Physics 100, no. 1-2 (October 1985): 599–619. http://dx.doi.org/10.1007/bf00158448.

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35

Neugebauer, Marcia. "Pioneers of space physics: A career in the solar wind." Journal of Geophysical Research: Space Physics 102, A12 (December 1, 1997): 26887–94. http://dx.doi.org/10.1029/97ja02444.

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36

Thieman, J. R., D. A. Roberts, and T. A. King. "SPASE: The Connection along Solar and Space Physics Data Centers." Data Science Journal 12 (2013): WDS147—WDS153. http://dx.doi.org/10.2481/dsj.wds-025.

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37

Dawson, Jim. "Solar and Space Physics Get a Detailed 10-Year Plan." Physics Today 55, no. 10 (October 2002): 23–25. http://dx.doi.org/10.1063/1.1522158.

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38

Flood, Dennis J. "Advanced space solar cells." Progress in Photovoltaics: Research and Applications 6, no. 3 (May 1998): 187–92. http://dx.doi.org/10.1002/(sici)1099-159x(199805/06)6:3<187::aid-pip227>3.0.co;2-8.

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39

Pomoell, Jens, and Rami Vainio. "A note on using thermally driven solar wind models in MHD space weather simulations." Proceedings of the International Astronomical Union 6, S274 (September 2010): 102–4. http://dx.doi.org/10.1017/s1743921311006661.

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AbstractOne of the challenges in constructing global magnetohydrodynamic (MHD) models of the inner heliosphere for, e.g., space weather forecasting purposes, is to correctly capture the acceleration and expansion of the solar wind. In many current models, the solar wind is driven by varying the polytropic index so that a desired heating is obtained. While such schemes can yield solar wind properties consistent with observations, they are not problem-free. In this work, we demonstrate by performing MHD simulations that altering the polytropic index affects the properties of propagating shocks significantly, which in turn affect the predicted space weather conditions. Thus, driving the solar wind with such a mechanism should be used with care in simulations where correctly capturing the shock physics is essential. As a remedy, we present a simple heating function formulation by which the polytropic wind can be used while still modeling the shock physics correctly.
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40

Baker, Daniel N. "Plasma physics and the 2013–2022 decadal survey in solar and space physics." Plasma Physics and Controlled Fusion 58, no. 10 (September 6, 2016): 104003. http://dx.doi.org/10.1088/0741-3335/58/10/104003.

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41

Wrenn, G. L., D. J. Rodgers, and K. A. Ryden. "A solar cycle of spacecraft anomalies due to internal charging." Annales Geophysicae 20, no. 7 (July 31, 2002): 953–56. http://dx.doi.org/10.5194/angeo-20-953-2002.

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Abstract. It is important to appreciate how the morphology of internal charging of spacecraft systems, due to penetrating electrons, differs from that of the more common surface charging, due to electrons with lower energy. A specific and recurrent anomaly on a geostationary communication satellite has been tracked for ten years so that solar cycle and seasonal dependencies can be clearly established. Concurrent measurements of sunspot number, solar wind speed and 2-day >2 MeV electron fluence are presented to highlight pertinent space weather relationships, and the importance of understanding the complex particle interaction processes involved.Key words. Magnetospheric physics (energetic particles; trapped; solar wind – magnetosphere interactions) – space plasma physics (spacecraft sheaths, wakes, charging)
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42

Hannaford, Peter. "Foreword." Australian Journal of Physics 46, no. 1 (1993): 1. http://dx.doi.org/10.1071/ph930001.

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This special issue contains selected papers of Plenary and Keynote Lectures presented at the Tenth National Congress of the Australian Institute of Physics, held at the University of Melbourne from 10 to 14 February, 1992. The Congress was attended by nearly 1000 delegates, including numerous distinguished physici~ts from Australia and abroad, who were treated to a smorgasbord of physics ranging from astrophysics to particle physics. The Congress was organised around a series of fifteen separate sections, representing various branches of physics in which there is active Australian interest, and incorporated the First Conference of the Vacuum Society of Australia; the Fifth Gaseous Electronics Meeting; the Fourteenth AINSE Nuclear and Particle Physics Conference; the 1992 Physics Teachers Conference; the Third Australasian Conference on Remote Sensing of Atmospheres and Oceans; and the South Pacific Solar-Terrestrial and Space Physics Workshop.
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43

Goddard, Alison. "Space: Cluster tackles the solar wind." Physics World 9, no. 5 (May 1996): 7. http://dx.doi.org/10.1088/2058-7058/9/5/5.

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44

Kuznetsov, V. D. "Space solar research: achievements and prospects." Physics-Uspekhi 58, no. 6 (June 30, 2015): 621–29. http://dx.doi.org/10.3367/ufne.0185.201506k.0664.

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45

KHEIRABADI, Fouad, Hooshmand ALIZADEH, and Hossein NOURMOHAMMADZAD. "Improving Climatic Comfort of Citizens by Adjusting the Orientation and Extension of Physics of City Squares: Case Study of Yazd." Chinese Journal of Urban and Environmental Studies 05, no. 02 (June 2017): 1750012. http://dx.doi.org/10.1142/s2345748117500129.

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The heat of the earth is provided by solar radiation. A change in the angle of solar radiation and the surface of the earth causes changes in the ambient temperature. Sometimes, these changes reduce climatic comfort of human beings. Climatic comfort is established when there is a balance between excreted and absorbed temperatures of the skin of the body. Orientation and extension rates of physics of squares relative to the geographical north influence the amount of received direct sunlight in different months. Relevant studies show that the squares of the city of Yazd reduce the climatic comfort of its citizens; moreover, the physics of Yazd's squares apply various extension rates, which led to high building costs to citizens and relevant organizations. This study, by using the correlation method and R software, measures different orientation and extension rates of physics of squares in Yazd. It analyzes two models with orientation and physical extension as variables and evaluates the shade and sunlight in the space. The results reveal significant differences between desirable and undesirable options. Considering the climatic comfort of space users and residents at the same time, a rectangle with an extension ratio of one to several and the north-south orientation, making the lowest facade face the south, is the most appropriate physic for city squares.
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46

Tsurutani, Bruce T., Gurbax S. Lakhina, and Rajkumar Hajra. "The physics of space weather/solar-terrestrial physics (STP): what we know now and what the current and future challenges are." Nonlinear Processes in Geophysics 27, no. 1 (February 25, 2020): 75–119. http://dx.doi.org/10.5194/npg-27-75-2020.

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Abstract. Major geomagnetic storms are caused by unusually intense solar wind southward magnetic fields that impinge upon the Earth's magnetosphere (Dungey, 1961). How can we predict the occurrence of future interplanetary events? Do we currently know enough of the underlying physics and do we have sufficient observations of solar wind phenomena that will impinge upon the Earth's magnetosphere? We view this as the most important challenge in space weather. We discuss the case for magnetic clouds (MCs), interplanetary sheaths upstream of interplanetary coronal mass ejections (ICMEs), corotating interaction regions (CIRs) and solar wind high-speed streams (HSSs). The sheath- and CIR-related magnetic storms will be difficult to predict and will require better knowledge of the slow solar wind and modeling to solve. For interplanetary space weather, there are challenges for understanding the fluences and spectra of solar energetic particles (SEPs). This will require better knowledge of interplanetary shock properties as they propagate and evolve going from the Sun to 1 AU (and beyond), the upstream slow solar wind and energetic “seed” particles. Dayside aurora, triggering of nightside substorms, and formation of new radiation belts can all be caused by shock and interplanetary ram pressure impingements onto the Earth's magnetosphere. The acceleration and loss of relativistic magnetospheric “killer” electrons and prompt penetrating electric fields in terms of causing positive and negative ionospheric storms are reasonably well understood, but refinements are still needed. The forecasting of extreme events (extreme shocks, extreme solar energetic particle events, and extreme geomagnetic storms (Carrington events or greater)) are also discussed. Energetic particle precipitation into the atmosphere and ozone destruction are briefly discussed. For many of the studies, the Parker Solar Probe, Solar Orbiter, Magnetospheric Multiscale Mission (MMS), Arase, and SWARM data will be useful.
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47

Strong, Keith, Julia Saba, and Therese Kucera. "Understanding Space Weather: The Sun as a Variable Star." Bulletin of the American Meteorological Society 93, no. 9 (September 1, 2012): 1327–35. http://dx.doi.org/10.1175/bams-d-11-00179.1.

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The American Meteorological Society has recently adopted space weather as a new core competency. This is the first in a series of papers discussing the multidisciplinary aspects of space weather. This paper concerns the physics behind solar variability, the driver of space weather. We follow the tortuous journey of the energy from its production in the solar core until it escapes into interplanetary space, showing how the internal dynamics and structure of the Sun change its nature. We show how the production and dissipation of magnetic fields are a key clue to untangling the riddle of the sunspot cycle and how that, in turn, affects the amount of radiation that the Earth receives from the Sun—the total solar irradiance.
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48

Avakyan, S. V., I. M. Afanas'ev, N. A. Voronin, I. A. Zotkin, and D. A. Chernikov. "Space Solar Patrol and problems of space weather." Journal of Optical Technology 73, no. 4 (April 1, 2006): 222. http://dx.doi.org/10.1364/jot.73.000222.

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49

Blinov, V. V., V. M. Vladimirov, S. N. Kulinich, A. I. Nikiforov, D. N. Pridachin, D. O. Pchelyakov, O. P. Pchelyakov, L. V. Sokolov, and D. V. Yarockiy. "Equipment for growing semiconductor heterostructures in outer space." Spacecrafts & Technologies 5, no. 2 (June 25, 2021): 110–15. http://dx.doi.org/10.26732/j.st.2021.2.06.

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This article describes the features of the equipment developed at the Rzhanov Institute of Semiconductor Physics for conducting experiments on growing semiconductor heterostructures from molecular beams in outer space under the conditions of an orbital flight of the International Space Station. Working out the processes of epitaxy of semiconductor films in outer space will allow us to grow complex semiconductor structures with sharp boundaries, which serve as the basis for the creation of solar cells, as well as devices of modern microwave, optoand microelectronics. Cascade photovoltaic converters based on such multilayer heterostructures of A3B5 semiconductor compounds have high efficiency and radiation resistance and, therefore, are most widely used for the manufacture of space solar cells. The high efficiency of such batteries is due to the wide spectral range in which solar radiation is effectively absorbed and used in photovoltaic conversion.
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50

Damé, L., L. Acton, M. Bruner, P. Connes, T. Cornwell, B. Foing, J. Heyvaerts, et al. "Solar physics at ultrahigh resolution from the space station with the Solar Ultraviolet Network (SUN)." Advances in Space Research 11, no. 5 (January 1991): 267–70. http://dx.doi.org/10.1016/0273-1177(91)90390-6.

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