Relevant bibliographies by topics / Sun Ray

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Sun Ray'

Author: Grafiati
Published: 4 June 2021
Last updated: 7 February 2022

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Journal articles on the topic "Sun Ray"

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Vyas, Snehalata. "SUN RAY AND COLOR THERAPY." International Journal of Research -GRANTHAALAYAH 2, no. 3SE (December 31, 2014): 1. http://dx.doi.org/10.29121/granthaalayah.v2.i3se.2014.3643.

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The entire body of beings is colorful. All the components of the body have different colors. All the cells of the body are also colored. If any part of the body becomes ill, then there is an imbalance of colors along with its chemical substances. Color therapy balances those colors.If you feel a lack of energy, you get a lack of confidence, if the thinking is not clear then color therapy can help you. Colors have a profound effect on the brain on our mind. This color strength has also made it useful for healing. There are many diseases for which color is used for treatment. Due to these characteristics, it has been named "Color Therapy". प्राणियों का सम्पूर्ण शरीर रंगीन है। शरीर के समस्त अवयवों का रंग अलग-अलग है। शरीर की समस्त कोषिकायें भी रंगीन है। शरीर का कोई अंग बीमार होता है तो उसका रासायनिक द्रव्यों के साथ-साथ रंगो का असंतुलन हो जाता है। रंग चिकित्सा उन रंगो को संतुलित कर देती है।आप ऊर्जा की कमी महसूस करते है आत्मविष्वास में कमी पाते है, सोच स्पष्ट नहीं हो पाती है तो रंग चिकित्सा आपकी सहायता कर सकती है। रंगो का हमारे मन पर मस्तिष्क पर गहरा असर पड़ता है। रंगो की इस ताकत ने उपचार के लिए भी उपयोगी बना दिया है। कई बिमारियाँ है जिनके उपचार के लिए रंगो का इस्तेमाल किया जाता है। इन खूबियों के कारण इसे ‘‘कलर थेरेपी‘‘ यानी रंग चिकित्सा का नाम दिया गया है।
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Swinbanks, David. "Japanese set to X-ray Sun." Nature 352, no. 6331 (July 1991): 96. http://dx.doi.org/10.1038/352096a0.

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Gopalswamy, Nat. "Positron Processes in the Sun." Atoms 8, no. 2 (April 22, 2020): 14. http://dx.doi.org/10.3390/atoms8020014.

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Positrons play a major role in the emission of solar gamma-rays at energies from a few hundred keV to >1 GeV. Although the processes leading to positron production in the solar atmosphere are well known, the origin of the underlying energetic particles that interact with the ambient particles is poorly understood. With the aim of understanding the full gamma-ray spectrum of the Sun, I review the key emission mechanisms that contribute to the observed gamma-ray spectrum, focusing on the ones involving positrons. In particular, I review the processes involved in the 0.511 MeV positron annihilation line and the positronium continuum emissions at low energies, and the pion continuum emission at high energies in solar eruptions. It is thought that particles accelerated at the flare reconnection and at the shock driven by coronal mass ejections are responsible for the observed gamma-ray features. Based on some recent developments I suggest that energetic particles from both mechanisms may contribute to the observed gamma-ray spectrum in the impulsive phase, while the shock mechanism is responsible for the extended phase.
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Ueda, Hiroshi. "On the vanishing point of sun-ray." Journal of Graphic Science of Japan 19, no. 1 (1985): 7–10. http://dx.doi.org/10.5989/jsgs.19.7.

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Kosovichev, A. G., and V. V. Zharkova. "X-ray flare sparks quake inside Sun." Nature 393, no. 6683 (May 1998): 317–18. http://dx.doi.org/10.1038/30629.

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Podgorny, A. I., and I. M. Podgorny. "X-ray bright points on the Sun." Astronomy Reports 44, no. 6 (June 2000): 407–13. http://dx.doi.org/10.1134/1.163864.

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Orlando, S., G. Peres, and F. Reale. "Viewing the sun as an X-ray star." Advances in Space Research 32, no. 6 (September 2003): 955–64. http://dx.doi.org/10.1016/s0273-1177(03)00297-7.

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Krucker, Sam, Arnold O. Benz, T. S. Bastian, and Loren W. Acton. "X‐Ray Network Flares of the Quiet Sun." Astrophysical Journal 488, no. 1 (October 10, 1997): 499–505. http://dx.doi.org/10.1086/304686.

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Zeman, Ellen J. "Yohkoh Returns X‐Ray Images of the Sun." Physics Today 45, no. 5 (May 1992): 19. http://dx.doi.org/10.1063/1.2809656.

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Grant, Andrew. "A puzzling gamma-ray survey of the Sun." Physics Today 71, no. 10 (October 2018): 21. http://dx.doi.org/10.1063/pt.3.4038.

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Dissertations / Theses on the topic "Sun Ray"

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Kóta, J., and J. R. Jokipii. "Transient Cosmic-ray Events beyond the Heliopause: Interpreting Voyager-1 Observations." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624725.

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In 2013 March and 2014 May, Voyager-1 (V1) experienced small but significant increases in the flux of galactic cosmic rays (GCRs) in the hundred MeV/n range. Additionally, V1 also saw episodic depletion of GCR flux around perpendicular pitch angles. We discuss the pitch-angle distribution and the time profiles of these events. In a previous paper, we interpreted the 2013 "bump" as the GCRs remotely sensing a shock that reached the magnetic field line passing through V1: particles gained energy as they were reflected on the approaching region of the stronger magnetic field of the disturbance. Here, we point out that energy gain is not restricted to reflected particles -GCRs passing through the disturbance also gain energy. The effect should be present in a broad range of pitch angles with the maximum increase of GCR intensity predicted to occur at the critical reflection angle. In this paper, the shock is not step-like, but a gradual increase of the magnetic field strength, B, taking a few days, in agreement with V1 measurements. This smoothens the profile of the predicted bump in the GCR flux. We also address the linear episodic decreases seen around perpendicular pitch angles. These events are interpreted in terms of adiabatic cooling behind the shock due to the slow weakening of B. We present simple numerical model calculations and find that a gradual shock followed by a slow decrease of B, as observed, may account for both the episodic increases and the anisotropic depletion of GCR fluxes.
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O'Dwyer, Brendan. "EUV & X-ray spectroscopic diagnostics of the solar corona." Thesis, University of Cambridge, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.610731.

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Miyake, Fusa, A. J. Timothy Jull, Irina P. Panyushkina, Lukas Wacker, Matthew Salzer, Christopher H. Baisan, Todd Lange, Richard Cruz, Kimiaki Masuda, and Toshio Nakamura. "Large 14C excursion in 5480 BC indicates an abnormal sun in the mid-Holocene." NATL ACAD SCIENCES, 2017. http://hdl.handle.net/10150/623129.

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Radiocarbon content in tree-rings can be an excellent proxy of the past incoming cosmic ray intensities to the Earth. Although such past cosmic ray variations have been studied by measurements of 14C contents in tree rings with ≧10 year time resolution for the Holocene (1), there are few annual 14C data. There is a little understanding about annual 14C variations in the past with the exception of a few periods including the AD774-775 annual 14C excursion (2). Here, we report the result of 14C measurements using the bristlecone pine tree rings for the period from 5490 BC to 5411 BC with 1-2 year resolution, and a finding of an extraordinarily large 14C increase (20‰) from 5481 BC to 5471 BC (the 5480 BC event). The 14C increase rate of this event is much larger than that of the normal Grand Solar Minima. We propose the possible causes of this event are a special phase of grand solar minimum, or a combination of successive solar proton events and a normal grand solar minimum.
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Mathur, Abhishek, and n/a. "Multi Agents for Heterogeneous Operating System Environments." University of Canberra. Information Sciences & Engineering, 2007. http://erl.canberra.edu.au./public/adt-AUC20070810.090108.

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As IT industries develop, upgrade and diversify, heterogeneous operating environments running a mix of new and legacy systems become increasingly important. Such environments are currently inadequate due to lack of compatibility with each other. This thesis investigates how agents can be utilised to facilitate such heterogeneous environments, aiding enterprise systems in building bridges between incompatible software and hardware systems. An autonomous agent has independent agency and decision-making astuteness. When placed in heterogeneous environments to interact with other such agents, the consequences of its action and its preferred choice of actions are greatly influenced by actions of other agents interacting in heterogeneous environments. The main objectives of this thesis include examining the roles of agents in heterogeneous operating environments, development of a novel multi agent base architecture and an associated framework for single and heterogeneous environment. The research work also studies the plausible application to test the developed proof of concept by developing application and using the framework that utilises Windows services in a totally incompatible Solaris based Sun Ray ultra thin client environment. The work includes a novel method of modeling agent based communication architecture suitable for correspondence between two inherently different operating systems - Solaris and Microsoft Windows. The circumstances in which coordination or coordination failure occurs between these systems are investigated. The proposed method of agent based communication that can potentially overcome the barriers formed by two completely different software and hardware architectural regimes. An analysis of printing services in MS Windows and Solaris environments, review the age long problem of lack of device drivers for commonly (and cheaply) available Ink Jet printers for Unix (and like) operating systems. A novel method is proposed that uses agents in heterogeneous environment to overcome this problem. A new architecture that utilises Windows based printing services on a Sun Ray ultra thin client is presented to test and evaluate the proof of concept. This thesis is motivated by the need to provide a low cost printing solution to Sun Ray users. Most Windows based desktop users currently have access to variety of low cost printing solutions. Printer vendors ship device drivers only for Windows or at most Macintosh, as other operating systems such as Solaris, MVS, z/OS are used for corporate solutions and low cost desktop printing have not been a major requirement in the past.
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Meehan, Patrick James. "Development of a Water Cloud Radiance Model for Use in Training an Artificial Neural Network to Recover Cloud Properties from Sun Photometer Observations." Thesis, Virginia Tech, 2021. http://hdl.handle.net/10919/103742.

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As the planetary climate continues to evolve, it is important to build an accurate long-term climate record. State-of-the-art atmospheric science requires a variety of approaches to the measurement of the atmospheric structure and composition. This thesis supports the possibility of inferring cloud properties from sun photometer observations of the cloud solar aureole using an artificial neural network (ANN). Training of an ANN requires a large number of input and output parameter sets. A cloud radiance model is derived that takes into consideration the cloud depth, the mean size of the cloud water particles, and the cloud liquid water content. The cloud radiance model derived here is capable of considering the wavelength of the incident sunlight and the cloud lateral dimensions as parameters; however, here we consider only one wavelength—550 nm—and one lateral dimension—500 m—to demonstrate its performance. The cloud radiance model is then used to generate solar aureole profiles corresponding to the cloud parameters as they would be observed using a sun photometer. Coefficients representative of the solar aureole profiles may then be used as inputs to a trained ANN to infer the parameters used to generate the profile. This process is demonstrated through examples. A manuscript submitted for possible publication based on an early version of the cloud radiance model was deemed naïve by reviewers, ultimately leading to improvements documented here.
Master of Science
The Earth's climate is driven by heat from the sun and the exchange of heat between the Earth and space. The role of clouds is paramount in this process. One aspect of "cloud forcing" is cloud structure and composition. Required measures may be obtained by satellite or surface-based observations. Described here is the creation of a numerical model that calculates the disposition of individual bundles of light within water clouds. The clouds created in the model are all described by the mean size of the cloud water droplets, the amount of water in the cloud, and cloud depth. Changing these factors relative to each other changes the amount of light that traverses the cloud and the angle at which the individual bundles of light leave the cloud as measured using a device called a sun photometer. The measured amount and angle of bundles of light leaving the cloud are used to recover the parameters that characterize the cloud; i.e., the size of the cloud water droplets, the amount of water in the cloud, and the cloud depth. Two versions of the cloud radiance model are described.
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Salas, Matamoros Carolina. "Radio and X-ray studies of Coronal Mass Ejections and their relevance for Space Weather." Thesis, Paris Sciences et Lettres (ComUE), 2016. http://www.theses.fr/2016PSLEO016/document.

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La couronne solaire est un milieu très dynamique : instabilités du champ magnétique, qui structure le plasma, conduit à l'accélération et le chauffage des particules chargées et à l'éjection de grandes structures dans l'héliosphère, les émissions de masse coronale (CME, selon ces sigles en anglais). Ces structures magnétiques éjectées peuvent interagir avec le champ magnétique de la Terre et affecter le plasma de l'environnement. Ces structures conduisent également à l'induction des courants électriques dans le sol à des latitudes élevées. L'étude de l'origine et de la propagation de ces émissions est d'intérêt pour l’astrophysique dans l’encadre des applications générales et pour la météorologie de l’espace. La compréhension des processus de base est une condition importante pour l'élaboration des méthodes de prévision des arrivées de ces perturbations en utilisant des observations de la couronne solaire. Les CMEs sont observées et étudiées à travers des images coronographiques. La limitation fondamentale du coronographe est qu'il montre la couronne seulement dans le plan du ciel, donc il bloque, forcément, la vue sur le disque solaire. Mais le geoefficacité d'une CME dépend essentiellement de la proximité à la ligne Soleil- Terre et de l'évolution dans la basse couronne que ne sont pas visibles à travers des observations coronographiques. Un des problèmes est la difficulté d’estimer l'arrivée d'une CME à la Terre, parce que les mesures avec coronographes directes de la vitesse de propagation des CMEs qui est dirigée vers la Terre ne sont pas possibles dans la ligne Soleil-Terre. Cette thèse présente l'étude des CMEs en trois étapes : (1) une étude de cas de l'évolution CME dans la bassecouronne et son rôle dans l'accélération des particules, (2) la relation entre la polarisation de l'émission de sursauts radio de type IV associées à CMEs dans la couronne et l'orientation du champ magnétique observé quand les CMEs arrivent à la Terre, et (3) des estimations radiatives de la vitesse des CMEs pour les prévisions des temps d’arrivée des CMEs à la Terre. Imagerie en utilisant des émissions radio dans la basse couronna peut montrer les signatures des CMEs sur le disque solaire. Des études précédentes avec le Radiohéliographe de Nançay (NRH) suggèrent, en fait, que les images de radio aux longueurs d'onde métriques peuvent suivre l'évolution des CMEs bien avant qu'ils deviennent visibles dans la couronne. Le diagnostic de l'évolution CME dans la basse couronne développée dans ce travail a été illustrée par l'étude de l'événement éruptif du 26 Avril 2008, qui a offert une occasion unique d'étudier le lien physique entre une seule CME bien identifiée, l'accélération des électrons tracé par émission radio, ainsi que la production des particules énergétiques solaires (SEP, selon ces sigles en anglais) observées dans l'espace. Nous effectuons une analyse détaillée en combinant les observations radio (NRH et DAM, Wind / WAVES spectrographe) et les observations de la couronne avec des satellites dans EUV et lumière blanche, ainsi que des mesures ‘in situ’ des particules énergétiques près de 1UA (satellites SoHO et STEREO). En combinant des images prises à partir de plusieurs points de vue, nous avons pu déduire l'évolution 3D en fonction du temps du front de l’éjection de mass qui s’est développée autour de l’éruption de la CME. Enfin, nous avons identifié, à partir des observations radio et SEP, trois régions différentes d'accélération des particules associées à l'évolution de la même CME, séparés en longitude environ 140°
The solar corona is a highly dynamical medium: instabilities of the magnetic field, which structure the plasma, lead to the acceleration and heating ofcharged particles and to the ejection of large structures into the heliosphere, the Coronal Mass Ejections (CMEs). These ejected magnetic structures can interact with the Earth's magnetic field and thereby affect the plasma environment and the high atmosphere of the Earth. Studying the origin and propagation of CMEs is of interest for both astrophysics in general and space weather applications. The understanding of the basic processes is indeed a pre-requisite for developing prediction methods of potentially geo-effective disturbances based on observations of the solar corona.The CMEs are observed and studied primarily through coronographic images. The basic limitation of the coronagraph is that it shows the corona only in the plane of the sky, and blocks by necessity the view on the solar disk. But the geoeffectiveness of a CME depends crucially on the proximity to the Sun-Earth line and the measurements of the propagation speed, onset and early evolution of CMEs in the low corona are not accessible to coronographic observations. This thesis presents the study of CMEs in three different stages: (1) a case study of the CME evolution in the low corona and of its role in particle acceleration, (2) the relationship between the polarisation of the type IV radio emission associated with Earth-directed CMEs in the corona and the orientation of the magnetic field observed as the CMEs arrive at the Earth, and (3) the estimation of the travel times of CMEs to the Earth. Radio imaging with the Nancay Radioheliograph (NRH) suggest that radio images at metric wavelengths track the early evolution of CMEs well before they become visible in the corona. The examination of the CME evolution in the low corona developed in this work was illustrated through the study of the eruptive event on 26 April 2008, which offered a unique opportunity to investigate the physical link between a single well-identified CME, electron acceleration as traced by radio emission, and the production of solar energetic particles (SEPs) observed in space. We conduct a detailed analysis combining radio observations (NRH and Decameter Array, Wind/WAVES spectrograph) with remote-sensing observations of the corona in extreme ultraviolet (EUV) and white light as well as in-situ measurements of energetic particles near 1AU (SoHO and STEREO spacecraft). By combining images taken from multiple vantage points we were able to derive the time-dependent evolution of the 3D pressure front developing around the erupting CME. Finally, we identified, from the radio and SEP observations, three different particle acceleration regions associated to the evolution of the same CME, separated in longitude by about 140$^\circ$. The observations for this event showed that it is misleading to interpret multi-spacecraft SEP measurements in terms of one acceleration region in the corona
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Sun, Fu [Verfasser], John [Akademischer Betreuer] Banhart, John [Gutachter] Banhart, and Yan [Gutachter] Lu. "X-ray radiographic and tomographic investigations of cycled lithium ion batteries / Fu Sun ; Gutachter: John Banhart, Yan Lu ; Betreuer: John Banhart." Berlin : Technische Universität Berlin, 2017. http://d-nb.info/1156180074/34.

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Törnros, Martin. "Interactive visualization of space weather data." Thesis, Linköpings universitet, Medie- och Informationsteknik, 2013. http://urn.kb.se/resolve?urn=urn:nbn:se:liu:diva-101986.

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This work serves to present the background, approach, and selected results for the initial master thesis and prototyping phase of Open Space, a joint visualization software development project by National Aeronautics and Space Administration (NASA), Linköping University (LiU) and the American Museum of Natural History (AMNH). The thesis report provides a theoretical introduction to heliophysics, modeling of space weather events, volumetric rendering, and an understanding of how these relate in the bigger scope of Open Space. A set of visualization tools that are currently used at NASA and AMNH are presented and discussed. These tools are used to visualize global heliosphere models, both for scientific studies and for public presentations, and are mainly making use of geometric rendering techniques. The paper will, in detail, describe a new approach to visualize the science models with volumetric rendering to better represent the volumetric structure of the data. Custom processors have been developed for the open source volumetric rendering engine Voreen, to load and visualize science models provided by the Community Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center (GSFC). Selected parts of the code are presented by C++ code examples. To best represent models that are defined in non-Cartesian space, a new approach to volumetric rendering is presented and discussed. Compared to the traditional approach of transforming such models to Cartesian space, this new approach performs no such model transformations, and thus minimizes the amount of empty voxels and introduces less interpolation artifacts. Final results are presented as rendered images and are discussed from a scientific visualization perspective, taking into account the physics representation, potential rendering artifacts, and the rendering performance.
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Tenholt, Frederik [Verfasser], Julia [Gutachter] Tjus, and Horst [Gutachter] Fichtner. "Studying the temporal variation of the cosmic-ray sun shadow : comparison of IceCube data with models of the solar magnetic field / Frederik Tenholt ; Gutachter: Julia Tjus, Horst Fichtner ; Fakultät für Physik und Astronomie." Bochum : Ruhr-Universität Bochum, 2020. http://d-nb.info/1205976329/34.

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Tenholt, Frederik Josef [Verfasser], Julia [Gutachter] Tjus, and Horst [Gutachter] Fichtner. "Studying the temporal variation of the cosmic-ray sun shadow : comparison of IceCube data with models of the solar magnetic field / Frederik Tenholt ; Gutachter: Julia Tjus, Horst Fichtner ; Fakultät für Physik und Astronomie." Bochum : Ruhr-Universität Bochum, 2020. http://d-nb.info/1205976329/34.

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Books on the topic "Sun Ray"

1

Single ray of sun. 2nd ed. Aberystwyth: Celtic Studies, 2003.

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Van Allen, James Alfred, 1914-, ed. Cosmic rays, the sun, and geomagnetism: The works of Scott E. Forbush. Washington, D.C: American Geophysical Union, 1993.

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Tallents, G. J., and James Dunn. Soft X-ray lasers and applications VIII: 4-6 August 2009, San Diego, California, United States. Bellingham, Wash: SPIE, 2009.

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Yŏhae Yi Sun-sin: Nŏ raya sesang ŭl hwapʻyŏngkʻe harira. Sŏul-si: Wijŭdŏm Hausŭ, 2008.

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COSPAR. Scientific Commission E. E1.5 Symposia. The sun and similar stars/cosmic ray spectra and composition: Proceedings of the E2.4 and E1.5 symposia of COSPAR Scientific Commission E which were held during the thirty-second COSPAR Scientific Assembly, Nagoya, Japan, July, 1998. Oxford: Published for the Committee on Space Research [by] Pergamon, 2000.

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Kikō), Foton Fakutorī Kenkyūkai (2004 Kō-enerugī Kasokuki Kenkyū. Kō X-sen o mochiita dainamikku kōzō no kanōsei: Foton Fakutorī Kenkyūkai. Tsukuba-shi: High Energy Accelerator Research Organization, 2005.

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Foton Fakutorī Kenkyūkai (2003 Kō-enerugī Kasokuki Kenkyū Kikō). X-sen shōkaku sanran, kaisetsu kenkyū no hatten ni mukete: Genjō to kongo no kadai. [Tsukuba-shi]: High Energy Accelerator Research Organization, 2004.

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SPIE, ed. Optics for EUV, X-Ray, and gamma-ray astronomy III: 29-30 August 2007, San Diego, California, USA. Bellingham, Wash: SPIE, 2007.

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Kikō), Foton Fakutorī Kenkyūkai (2011 Kō-enerugī Kasokuki Kenkyū. X-sen topogurafī no genjō to tenbō: PF Kenkyūkai. Tsukuba-shi: KEK, 2011.

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Society of Photo-optical Instrumentation Engineers, ed. Hard X-ray and gamma-ray detector physics IX: 27-29 August 2007, San Diego, California, USA. Bellingham, Wash: SPIE, 2007.

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Book chapters on the topic "Sun Ray"

1

Hurford, G. J. "X-ray Instrumentation." In The Sun: A Laboratory for Astrophysics, 435–45. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2765-3_21.

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Mikurda, K., R. Falewicz, and P. Preś. "X-Ray Limb Flares with Plasma Ejections." In The Dynamic Sun, 239–42. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0760-3_15.

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Gabriel, A. H. "Soft X-ray Instrumentation." In The Sun: A Laboratory for Astrophysics, 423–34. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2765-3_20.

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Caillault, Jean-Pierre, David J. Helfand, John A. Nousek, and Leo O. Takalo. "X-ray selected M-dwarfs and the diffuse X-ray background." In Cool Stars, Stellar Systems, and the Sun, 100–102. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/3-540-16763-3_148.

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Rieger, Erich, and Gerhard Rank. "The Sun as a Gamma-Ray Source." In The Universe in Gamma Rays, 91–126. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04593-0_5.

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Weekes, Trevor C. "Gamma Ray Astronomy at High Energies." In From the Sun to the Great Attractor, 187–232. Berlin, Heidelberg: Springer Berlin Heidelberg, 2000. http://dx.doi.org/10.1007/3-540-45371-7_5.

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Mallik, P. C. V., J. C. Brown, and A. L. MacKinnon. "Solar X-Ray Processes." In Magnetic Coupling between the Interior and Atmosphere of the Sun, 463–64. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-02859-5_57.

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Kurt, V. G. "Electrons and X-Ray Emission of Solar Flares." In Basic Plasma Processes on the Sun, 409–13. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0667-9_71.

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Yano, Junko, Jan Kern, Kenneth Sauer, Yulia Pushkar, Uwe Bergmann, Pieter Glatzel, Johannes Messinger, Athina Zouni, and Vittal K. Yachandra. "Structure of the Photosynthetic Mn4Ca Cluster Using X-ray Spectroscopy." In Photosynthesis. Energy from the Sun, 533–38. Dordrecht: Springer Netherlands, 2008. http://dx.doi.org/10.1007/978-1-4020-6709-9_121.

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Shrivastava, P. K., and S. P. Agrawal. "Cosmic Ray Signatures of Different Types of Solar Wind Streams." In Basic Plasma Processes on the Sun, 259–60. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0667-9_46.

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Conference papers on the topic "Sun Ray"

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Herrick, Dan R. "Sun ray self-help guide." In Proceeding of the 39th ACM annual conference. New York, New York, USA: ACM Press, 2011. http://dx.doi.org/10.1145/2070364.2070403.

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Svoboda, R. "Neutrinos from the Sun." In The 26th international cosmic ray conference (ICRC). AIP, 2000. http://dx.doi.org/10.1063/1.1291486.

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Mazziotta, Mario Nicola, Pedro De la Torre Luque, Leonardo Di Venere, Alberto Fassò, Alfredo Ferrari, Francesco Loparco, Paola Sala, and Davide Serini. "Cosmic-ray interactions with the Sun." In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.1321.

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Lee, Jeongwoo. "Particle Acceleration in the Sun and Beyond." In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.1088.

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Huber, Martin C. E. "SOHO - A GLOBAL VIEW OF SUN AND HELIOSPHERE." In 25th International Cosmic Ray Conference. WORLD SCIENTIFIC, 1998. http://dx.doi.org/10.1142/9789814529044_0004.

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Jurysek, Jakub, and Michael Prouza. "Sun/Moon photometer for Cherenkov Telescope Array – first results." In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0853.

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Widmark, Axel. "Thermalization time scales for WIMP capture by the Sun." In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0916.

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Romanov, Andrey, Tommaso Chiarusi, Luigi Antonio Fusco, Matteo Sanguineti, and Federico Versari. "The Sun shadow observation with the ANTARES neutrino telescope." In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1001.

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Alvarez-Castillo, David, Oleksandr Sushchov, Piotr Homola, Dmitriy Beznosko, Nikolai Budnev, Dariusz Gora, Alok Gupta, et al. "Simulations of Cosmic Ray Ensembles originated nearby the Sun." In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0457.

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Horack, J. M., S. D. Storey, G. J. Fishman, C. A. Meegan, R. B. Wilson, T. M. Koshut, R. S. Mallozzi, and W. S. Paciesas. "BATSE observations of gamma-ray bursts in sun-referenced coordinate systems." In COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44254.

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Reports on the topic "Sun Ray"

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Branduardi-Raymont, Graziella, and et al. SMILE Definition Study Report. ESA SCI, December 2018. http://dx.doi.org/10.5270/esa.smile.definition_study_report-2018-12.

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Abstract:
The SMILE definition study report describes a novel self-standing mission dedicated to observing solar wind-magnetosphere coupling via simultaneous in situ solar wind/magnetosheath plasma and magnetic field measurements, X-Ray images of the magnetosheath and magnetic cusps, and UV images of global auroral distributions defining system-level consequences. The Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) will complement all solar, solar wind and in situ magnetospheric observations, including both space- and ground-based observatories, to enable the first-ever observations of the full chain of events that drive the Sun-Earth connection.
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Rolison, John M., and Ross W. WIlliams. Application of the 226Ra-230Th-234U and 227Ac-231Pa-235U radiochronometers to UF6 Cylinders. Office of Scientific and Technical Information (OSTI), January 2018. http://dx.doi.org/10.2172/1430909.

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Nino, Juan C., James Baciak, Paul Johns, Soumitra Sulekar, James Totten, and Jyothir Nimmagadda. BiI3 Crystals for High Energy Resolution Gamma-Ray Spectroscopy. Office of Scientific and Technical Information (OSTI), April 2017. http://dx.doi.org/10.2172/1352061.

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Good, William Stanley. Magnetic X-Ray Scattering Study of GdCo2Ge2 and NdCo2Ge2. Office of Scientific and Technical Information (OSTI), January 2002. http://dx.doi.org/10.2172/804538.

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Dickens, J. K., and D. C. Larson. Gamma-ray decay of levels in /sup 53/Cr. Office of Scientific and Technical Information (OSTI), November 1987. http://dx.doi.org/10.2172/5389860.

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Saitoh, T., P. M. Villella, and D. S. Dessau. X-ray absorption measurements of charge-ordered La{sub 0.5}Sr{sub 1.5}MnO{sub 4}. Office of Scientific and Technical Information (OSTI), April 1997. http://dx.doi.org/10.2172/603681.

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Roy, Utpal N. CdxZn1-xTeySe1-y (CZTS): An Emerging High-Performance Gamma-Ray Detector. Office of Scientific and Technical Information (OSTI), April 2018. http://dx.doi.org/10.2172/1431283.

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Gaffney, Kelly J. Ultrafast X-ray Science at the Sub-Picosecond Pulse Source. Office of Scientific and Technical Information (OSTI), September 2005. http://dx.doi.org/10.2172/878358.

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Hague, C. F., M. Tronc, and F. De Groot. Resonant x-ray emission from gas-phase TiCl{sub 4}. Office of Scientific and Technical Information (OSTI), April 1997. http://dx.doi.org/10.2172/603536.

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Tan, Lizhi. Investigations of the R5(SixGe1-x)4 Intermetallic Compounds by X-Ray Resonant Magnetic Scattering. Office of Scientific and Technical Information (OSTI), August 2008. http://dx.doi.org/10.2172/939380.

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