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Journal articles on the topic 'Sun Ray'

Author: Grafiati

Published: 4 June 2021

Last updated: 7 February 2022

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1

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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2

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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3

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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4

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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5

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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6

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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7

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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8

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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9

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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10

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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11

Chown, Marcus. "Dark-matter particles could ‘X-ray’ the sun." New Scientist 192, no. 2579 (November 2006): 15. http://dx.doi.org/10.1016/s0262-4079(06)61174-3.

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12

Edsjö, J., J. Elevant, R. Enberg, and C. Niblaeus. "Neutrinos from cosmic ray interactions in the Sun." Journal of Cosmology and Astroparticle Physics 2017, no. 06 (June 19, 2017): 033. http://dx.doi.org/10.1088/1475-7516/2017/06/033.

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13

Becker Tjus, J., P. Desiati, N. Döpper, H. Fichtner, J. Kleimann, M. Kroll, and F. Tenholt. "Cosmic-ray propagation around the Sun: investigating the influence of the solar magnetic field on the cosmic-ray Sun shadow." Astronomy & Astrophysics 633 (January 2020): A83. http://dx.doi.org/10.1051/0004-6361/201936306.

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The cosmic-ray Sun shadow, which is caused by high-energy charged cosmic rays being blocked and deflected by the Sun and its magnetic field, has been observed by various experiments, such as Argo-YBJ, Tibet, HAWC, and IceCube. Most notably, the shadow’s size and depth was recently shown to correlate with the 11-year solar cycle. The interpretation of such measurements, which help to bridge the gap between solar physics and high-energy particle astrophysics, requires a solid theoretical understanding of cosmic-ray propagation in the coronal magnetic field. It is the aim of this paper to establish theoretical predictions for the cosmic-ray Sun shadow in order to identify observables that can be used to study this link in more detail. To determine the cosmic-ray Sun shadow, we numerically compute trajectories of charged cosmic rays in the energy range of 5−316 TeV for five different mass numbers. We present and analyze the resulting shadow images for protons and iron, as well as for typically measured cosmic-ray compositions. We confirm the observationally established correlation between the magnitude of the shadowing effect and both the mean sunspot number and the polarity of the magnetic field during the solar cycle. We also show that during low solar activity, the Sun’s shadow behaves similarly to that of a dipole, for which we find a non-monotonous dependence on energy. In particular, the shadow can become significantly more pronounced than the geometrical disk expected for a totally unmagnetized Sun. For times of high solar activity, we instead predict the shadow to depend monotonously on energy and to be generally weaker than the geometrical shadow for all tested energies. These effects should become visible in energy-resolved measurements of the Sun shadow, and may in the future become an independent measure for the level of disorder in the solar magnetic field.

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14

Jardine, M., A. Collier Cameron, K. Wood, and J. F. Donati. "Magnetic Loop Models: from Sun to Stars." Symposium - International Astronomical Union 219 (2004): 529–40. http://dx.doi.org/10.1017/s0074180900182555.

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I review recent progress in determining the nature of the loop structures that form the coronae of solar-like stars. This progress has been driven by observational advances, in particular the new results from X-ray satellites (Chandra and XMM-Newton) and the availability of surface magnetograms from Zeeman-Doppler imaging. It is now clear that stars that are similar to the Sun in mass, but which rotate more rapidly, have a very different magnetic field structure. Their surfaces are more heavily spotted, with spots appearing at all latitudes, extending all the way up to the rotation pole. Their coronae are correspondingly much brighter in X-rays, containing plasma that is hotter and denser than on the Sun. In addition, stellar coronae can support massive co-rotating prominences out to many stellar radii. Recent efforts in modelling these magnetic structures are now bringing together both the surface magnetograms and also the coronal X-ray emission. The resulting coronal loop models show complex loop structures on all scales, with much of the X-ray emission coming from high latitudes where is does not suffer rotational self-eclipse. The observed high densities and X-ray emission measures are a natural consequence of the high magnetic flux density at the surface. The stripping of the corona due to centrifugal effects at high rotation rates can also explain the saturation and supersaturation of X-ray emission with increasing rotation rates, and the recent observation of a high rotational modulation in a supersaturated star.

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15

DeLuca, E. E., M. A. Weber, A. L. Sette, L. Golub, K. Shibasaki, T. Sakao, and R. Kano. "Science of the X-ray Sun: The X-ray telescope on Solar-B." Advances in Space Research 36, no. 8 (January 2005): 1489–93. http://dx.doi.org/10.1016/j.asr.2004.12.073.

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16

Marsh, Andrew J., David M. Smith, Lindsay Glesener, Iain G. Hannah, Brian W. Grefenstette, Amir Caspi, Säm Krucker, et al. "FirstNuSTARLimits on Quiet Sun Hard X-Ray Transient Events." Astrophysical Journal 849, no. 2 (November 8, 2017): 131. http://dx.doi.org/10.3847/1538-4357/aa9122.

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17

Farnik, F., and H. Garcia. "Phobos-goes soft x-ray observations of the sun." Astrophysical Journal 444 (May 1995): 929. http://dx.doi.org/10.1086/175663.

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18

Alexander, David. "Temperature structure of the quiet Sun X ray corona." Journal of Geophysical Research: Space Physics 104, A5 (May 1, 1999): 9701–8. http://dx.doi.org/10.1029/1998ja900016.

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19

Reale, F., G. Peres, and S. Orlando. "The Sun as an X‐Ray Star. III. Flares." Astrophysical Journal 557, no. 2 (August 20, 2001): 906–20. http://dx.doi.org/10.1086/321598.

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20

Cowen, R. "Yohkoh: A New X-Ray View of the Sun." Science News 141, no. 25 (June 20, 1992): 404. http://dx.doi.org/10.2307/3976567.

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21

Schmitt, J. H. M. M. "Magnetic activity of cool stars in the Hertzsprung-Russell diagram." Proceedings of the International Astronomical Union 7, S286 (October 2011): 296–306. http://dx.doi.org/10.1017/s1743921312005005.

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AbstractI review the X-ray emission from cool stars with outer convection zones in comparison to the Sun with a focus on the properties of low-activity stars. I present the recent results of long-term X-ray monitoring which demonstrate the existence of X-ray cycles on stars with known calcium cycles. The evidence of a minimum stellar X-ray flux is presented and arguments are put forward for the view that the Sun in its extended minimum between 2008 - 2009 behaved very much like a Maunder-minimum Sun.

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22

Rieger, E. "Gamma-Ray Precursors of Solar Flares." International Astronomical Union Colloquium 142 (1994): 645–48. http://dx.doi.org/10.1017/s0252921100077927.

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AbstractBursts have been observed by the gamma-ray spectrometer on SMM at medium- and high-energy gamma-rays that precede the flare maximum. The negligible contribution of nuclear lines in the spectra of these events and their impulsive appearance suggests that they are hard-electron-dominated events superposed on the flares. Spatial resolution at gamma-ray energies will be necessary to decide whether this kind of bursts is cospatial with the flares or whether they occur in the flares’ vicinity.Subject headings: Sun: flares — Sun: X-rays, gamma rays

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23

Bos, F., F. Tenholt, J. Becker Tjus, and S. Westerhoff. "Observation of the Cosmic-Ray Shadow of the Moon and Sun with IceCube." ASTRA Proceedings 2 (August 5, 2015): 5–8. http://dx.doi.org/10.5194/ap-2-5-2015.

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Abstract. Moon shadow analyses are standard methods to calibrate cosmic-ray detectors. We report on a three-year observation of cosmic-ray Moon and Sun shadows in different detector configurations. The cosmic-ray Moon shadow was observed with high statistical significance (> 6σ) in previous analyses when the IceCube detector operated in a smaller configuration before it was completed in December 2010. This work shows first analyses of the cosmic-ray Sun shadow in IceCube. A binned analysis in one-dimension is used to measure the Moon and Sun shadow with high statistical significance greater than 12σ.

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24

Siegert, Thomas. "Vertical position of the Sun with γ-rays." Astronomy & Astrophysics 632 (November 29, 2019): L1. http://dx.doi.org/10.1051/0004-6361/201936659.

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We illustrate a method for estimating the vertical position of the Sun above the Galactic plane by γ-ray observations. Photons of γ-ray wavelengths are particularly well suited for geometrical and kinematic studies of the Milky Way because they are not subject to extinction by interstellar gas or dust. Here, we use the radioactive decay line of 26Al at 1.809 MeV to perform maximum likelihood fits to data from the spectrometer SPI on board the INTEGRAL satellite as a proof-of-concept study. Our simple analytic 3D emissivity models are line-of-sight integrated, and varied as a function of the Sun’s vertical position, given a known distance to the Galactic centre. We find a vertical position of the Sun of z0 = 15 ± 17 pc above the Galactic plane, consistent with previous studies, finding z0 in a range between 5 and 29 pc. Even though the sensitivity of current MeV instruments is several orders of magnitude below that of telescopes for other wavelengths, this result reveals once more the disregarded capability of soft γ-ray telescopes. We further investigate possible biases in estimating the vertical extent of γ-ray emission if the Sun’s position is set incorrectly, and find that the larger the true extent, the less is it affected by the observer position. In the case of 26Al with an exponential scale height of 150 pc (700 pc) in the inner (full) Galaxy, this may lead to misestimates of up to 25%.

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25

ZIRAKASHVILI, VLADIMIR N. "COSMIC RAY ANISOTROPY PROBLEM." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6858–60. http://dx.doi.org/10.1142/s0217751x05030314.

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The anisotropy of cosmic rays, produced by Galactic supernovae is calculated. It is a factor 100 ÷ 1000 larger than the observed value at 1 PeV. It is shown that this contradiction can be explained if a cosmic ray diffusion coefficient is small in the local vicinity of the Sun.

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26

Young, Peter R. "The Sun: Our own backyard plasma laboratory." Proceedings of the International Astronomical Union 15, S350 (April 2019): 333–40. http://dx.doi.org/10.1017/s1743921319008366.

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AbstractThe Sun's atmosphere increases in temperature from 6000 degrees at the surface to over a million degrees at heights of a few thousand kilometers. This surprising temperature increase is still an active area of scientific study, but is generally thought to be driven by the dynamics of the Sun's magnetic field. The combination of a 2-to-3 order of magnitude temperature range and a low plasma density makes the solar atmosphere perhaps the best natural laboratory for the study of ionized atoms. Atomic transitions at ultraviolet (UV) and X-ray wavelength regions generally show no optical depth effects, and the lines are not subject to the interstellar absorption that affects astronomical sources. Here I highlight the importance of atomic data to modeling UV and X-ray solar spectra, with a particular focus on the CHIANTI atomic database. Atomic data needs and problems are discussed and future solar mission concepts presented.

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27

Kundu, M. R., and S. M. White. "Millimeter and Microwave Activity of the Sun." Symposium - International Astronomical Union 142 (1990): 457–65. http://dx.doi.org/10.1017/s007418090008846x.

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The emission of solar flares at millimeter wavelengths is of great interest both in its own right and because it is generated by the energetic electrons which also emit gamma rays. Since high-resolution imaging at gamma-ray energies is not presently possible, millimeter observations can act as a substitute. Except for that class of flares known as gamma-ray flares the millimetric emission is optically thin. It can be used as a powerful diagnostic of the energy distribution of electrons in solar flares and its evolution, and of the magnetic field. We have carried out high-spatial-resolution millimeter observations of solar flares this year using the Berkeley-Illinois-Maryland Array (BIMA), and report on the preliminary results in this paper (Kundu et al 1990; White et al 1990). We also report some recent results obtained from multifrequency observations using the VLA (White et al 1990).

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28

Vilmer, N. "Solar Hard X-Ray and Gamma-Ray Observations from GRANAT." International Astronomical Union Colloquium 142 (1994): 611–21. http://dx.doi.org/10.1017/s0252921100077885.

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AbstractHard X-rays and gamma-rays are the most direct signature of the energetic electrons and ions which are accelerated during solar flares. Since the beginning of 1990 the PHEBUS instrument and the SIGMA anticoincidence shield aboard GRANAT have provided hard X-ray and gamma-ray observations of solar bursts in the energy range 0.075-124 and 0.200-15 MeV, respectively. After a brief description of the experiments, we present some results obtained on solar bursts recorded in 1990 and 1991 June. Special emphasis is given to the results related with particle acceleration during solar flares.The first part of the review is devoted to the constraints obtained on the electron acceleration timescale through the analysis of the temporal characteristics of the bursts. Combined studies of hard X-ray and gamma-ray emissions from PHEBUS and radio emissions from the Nançay Multifrequency Radioheliograph are used to infer constraints on the coronal magnetic topology involved in flares. The characteristics (location, spectrum) of the radio-emitting sources are found to vary within a flare from one hard X-ray peak to the other. Hard X-ray and gamma-ray burst onsets and rapid increases of the > 10 MeV emission are coincident with changes in the associated radio emission pattern. These results will be discussed in the context of the flare energy release.The second part of the paper concerns the heliocentric angle distribution of > 10 MeV events and presents more detailed observations of some of the largest flares in the gamma-ray line and the high-energy domains produced by ultrarelativistic electrons and > 100 MeV nucleon−1 ions. The PHEBUS observations of the gamma-ray line flare of 11 June 1991 have been used to deduce the hardness of the accelerated ion spectrum. The link between the main part of the flare and the late long-lasting >50 MeV emission detected by EGRET/COMPTON is discussed. Finally some observations of the large 1990 May 24 flare which produced a large neutron event at ground level are presented.Subject headings: acceleration of particles — Sun: flares — Sun: radio radiation — Sun: X-rays, gamma rays

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29

Moreno-Insertis, Fernando. "X-ray jets and magnetic flux emergence in the Sun." Proceedings of the International Astronomical Union 4, S259 (November 2008): 201–10. http://dx.doi.org/10.1017/s1743921309030452.

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AbstractMagnetized plasma is emerging continually from the solar interior into the atmosphere. Magnetic flux emergence events and their consequences in the solar atmosphere are being observed with high space, time and spectral resolution by a large number of space missions in operation at present (e.g. SOHO, Hinode, Stereo, Rhessi). The collision of an emerging and a preexisting magnetic flux system in the solar atmosphere leads to the formation of current sheets and to field line reconnection. Reconnection under solar coronal conditions is an energetic event; for the field strengths, densities and speeds involved in the collision of emerging flux systems, the reconnection outflows lead to launching of high-speed (hundreds of km/s), high-temperature (107 K) plasma jets. Such jets are being observed with the X-Ray and EUV detectors of ongoing satellite missions. On the other hand, the spectacular increase in computational power in recent years permits to carry out three-dimensional numerical experiments of the time evolution of flux emerging systems and the launching of jets with a remarkable degree of detail.In this review, observation and modeling of the solar X-Ray jets are discussed. A two-decade long computational effort to model the magnetic flux emergence events by different teams has led to numerical experiments which explain, even quantitatively, many of the observed features of the X-ray jets. The review points out that, although alternative mechanisms must be considered, flux emergence is a prime candidate to explain the launching of the solar jets.

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30

Saeed, Mohsin, Min Zha, and Zhen Cao. "Simulation of the Galactic Cosmic Ray Shadow of the Sun." Chinese Physics Letters 34, no. 12 (December 2017): 129601. http://dx.doi.org/10.1088/0256-307x/34/12/129601.

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31

CHUPP, EDWARD L. "Frontiers of Gamma Ray and Neutron Observations from the Sun." Annals of the New York Academy of Sciences 655, no. 1 Frontiers in (June 1992): 278–91. http://dx.doi.org/10.1111/j.1749-6632.1992.tb17077.x.

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32

Mohammadi, Afshin, Behrooz Ilkhanizadeh, and Mohammad Ghasemi-rad. "Mandibular plasmocytoma with sun-ray periosteal reaction: A unique presentation." International Journal of Surgery Case Reports 3, no. 7 (2012): 296–98. http://dx.doi.org/10.1016/j.ijscr.2012.02.009.

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33

Ueda, K., R. Kano, S. Tsuneta, and H. Shibahashi. "Orientation of X-Ray Bright Points in the Quiet Sun." Solar Physics 261, no. 1 (December 15, 2009): 77–85. http://dx.doi.org/10.1007/s11207-009-9482-y.

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34

Mastichiadis, A., R. J. Protheroe, and S. A. Stephens. "Cosmic Ray Positron Production by Gamma Ray Interactions on Starlight." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 115–17. http://dx.doi.org/10.1017/s1323358000025133.

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AbstractWe examine the production of cosmic ray positrons by photon-photon pair production of high-energy γ-rays on starlight photons. We start by calculating the production rate as a function of positron energy and distance from the Sun resulting from interactions with sunlight. The results are generalized to production on other types of star. We calculate the average production rate per unit volume averaged over the local region of the galaxy, and we estimate the contribution to the observed intensity from this process.

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35

Hanasoge, Shravan M., T. L. Duvall, M. L. Derosa, and M. S. Miesch. "Can we detect convection in the Sun?" Proceedings of the International Astronomical Union 2, S239 (August 2006): 364–69. http://dx.doi.org/10.1017/s1743921307000737.

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AbstractWe investigate the possibility of detecting deep convection in the Sun by computing travel-time shifts induced by convective flows interacting with propagating waves. The convection zone is modeled using a velocity profile taken from an Anelastic convection simulation. We present results obtained from a ray calculation of travel-time shifts. We compare these results with a full 3D calculation of the wave-flow interaction.

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36

Zhang, Shuang Nan. "Similar phenomena at different scales: black holes, the Sun, γ-ray bursts, supernovae, galaxies and galaxy clusters." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 41–62. http://dx.doi.org/10.1017/s1743921307009842.

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AbstractMany similar phenomena occur in astrophysical systems with spatial and mass scales different by many orders of magnitudes. For examples, collimated outflows are produced from the Sun, proto-stellar systems, gamma-ray bursts, neutron star and black hole X-ray binaries, and supermassive black holes; various kinds of flares occur from the Sun, stellar coronae, X-ray binaries and active galactic nuclei; shocks and particle acceleration exist in supernova remnants, gamma-ray bursts, clusters of galaxies, etc. In this report I summarize briefly these phenomena and possible physical mechanisms responsible for them. I emphasize the importance of using the Sun as an astrophysical laboratory in studying these physical processes, especially the roles magnetic fields play in them; it is quite likely that magnetic activities dominate the fundamental physical processes in all of these systems.As a case study, I show that X-ray lightcurves from solar flares, black hole binaries and gamma-ray bursts exhibit a common scaling law of non-linear dynamical properties, over a dynamical range of several orders of magnitudes in intensities, implying that many basic X-ray emission nodes or elements are inter-connected over multi-scales. A future high timing and imaging resolution solar X-ray instrument, aimed at isolating and resolving the fundamental elements of solar X-ray lightcurves, may shed new lights onto the fundamental physical mechanisms, which are common in astrophysical systems with vastly different mass and spatial scales. Using the Sun as an astrophysical laboratory, “Applied Solar Astrophysics” will deepen our understanding of many important astrophysical problems.

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37

Thompson, D. J., D. L. Bertsch, D. J. Morris, and R. Mukherjee. "Energetic gamma ray experiment telescope high‐energy gamma ray observations of the Moon and quiet Sun." Journal of Geophysical Research: Space Physics 102, A7 (January 1997): 14735–40. http://dx.doi.org/10.1029/97ja01045.

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38

Lin, R. P., D. W. Curtis, J. H. Primbsch, P. R. Harvey, W. K. Levedahl, D. M. Smith, R. M. Pelling, F. Duttweiler, and K. Hurley. "A long-duration balloon payload for hard X-ray and gamma-ray observations of the sun." Solar Physics 113, no. 1-2 (January 1987): 333–45. http://dx.doi.org/10.1007/bf00147720.

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39

Sattarov, I., A. S. Hojaev, C. T. Sherdonov, and O. V. Ladenkov. "Relation of the X-ray bright point number to the X-ray background on the sun." Astronomical & Astrophysical Transactions 20, no. 3 (September 2001): 509–13. http://dx.doi.org/10.1080/10556790108213591.

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40

M. M. Schmitt, J. H. "X-ray Emission from Single Stars." Symposium - International Astronomical Union 219 (2004): 187–98. http://dx.doi.org/10.1017/s0074180900182117.

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During the last two decades a new field in stellar astrophysics emerged: Stellar X-ray astronomy. With the advent of soft X-ray imagery X-ray emission was found from many thousands of solar-like stars. I will summarize the most important X-ray properties of cool stars and how they compare to the Sun.

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41

Grefenstette, Brian W., Lindsay Glesener, Säm Krucker, Hugh Hudson, Iain G. Hannah, David M. Smith, Julia K. Vogel, et al. "THE FIRST FOCUSED HARD X-RAY IMAGES OF THE SUN WITHNuSTAR." Astrophysical Journal 826, no. 1 (July 18, 2016): 20. http://dx.doi.org/10.3847/0004-637x/826/1/20.

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Simon, A., S. J. Quinn, A. Spyrou, A. Battaglia, I. Beskin, A. Best, B. Bucher, et al. "SuN: Summing NaI(Tl) gamma-ray detector for capture reaction measurements." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 703 (March 2013): 16–21. http://dx.doi.org/10.1016/j.nima.2012.11.045.

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Ingelman, G., and M. Thunman. "High energy neutrino production by cosmic ray interactions in the Sun." Physical Review D 54, no. 7 (October 1, 1996): 4385–92. http://dx.doi.org/10.1103/physrevd.54.4385.

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Pevtsov, Alexei A., and Loren W. Acton. "Soft X‐Ray Luminosity and Photospheric Magnetic Field in Quiet Sun." Astrophysical Journal 554, no. 1 (June 10, 2001): 416–23. http://dx.doi.org/10.1086/321342.

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Saint-Hilaire, Pascal, Säm Krucker, Steven Christe, and Robert P. Lin. "THE X-RAY DETECTABILITY OF ELECTRON BEAMS ESCAPING FROM THE SUN." Astrophysical Journal 696, no. 1 (April 21, 2009): 941–52. http://dx.doi.org/10.1088/0004-637x/696/1/941.

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Kuhar, Matej, Säm Krucker, Lindsay Glesener, Iain G. Hannah, Brian W. Grefenstette, David M. Smith, Hugh S. Hudson, and Stephen M. White. "NuSTAR Detection of X-Ray Heating Events in the Quiet Sun." Astrophysical Journal 856, no. 2 (March 30, 2018): L32. http://dx.doi.org/10.3847/2041-8213/aab889.

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Khan, J. I., H. S. Hudson, and Z. Mouradian. "Soft X-ray analysis of a loop flare on the Sun." Astronomy & Astrophysics 416, no. 1 (February 26, 2004): 323–32. http://dx.doi.org/10.1051/0004-6361:20034274.

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Balter, M. "X-RAY SCIENCE: French 'Sun' to Rise at Site Near Paris." Science 289, no. 5486 (September 15, 2000): 1859b—1859. http://dx.doi.org/10.1126/science.289.5486.1859b.

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Verma, V. K., and M. C. Pande. "Longitudinal distribution of the hard X-ray bursts on the Sun." Solar Physics 99, no. 1-2 (September 1985): 285–89. http://dx.doi.org/10.1007/bf00157313.

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BARWICK, S., F. HALZEN, and P. B. PRICE. "THE SEARCH FOR NEUTRINO SOURCES BEYOND THE SUN." International Journal of Modern Physics A 11, no. 19 (July 30, 1996): 3393–413. http://dx.doi.org/10.1142/s0217751x96001620.

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Abstract:

It is hoped that in the near future, neutrino astronomy, born with the identification of thermonuclear fusion in the sun and the particle processes controlling the fate of a nearby supernova, will reach throughout and beyond our galaxy and make measurements relevant to cosmology, astrophysics, cosmic-ray physics and particle physics. The construction of a high-energy neutrino telescope requires a huge volume of very transparent, deeply buried material, such as ocean water or ice, which acts as the medium for detecting the particles. The AMANDA1 muon and neutrino telescope, now operating four strings of photomultiplier tubes buried in deep ice at the South Pole, is scheduled to be expanded to a ten-string array. The data collected over the first two years cover the three basic modes in which such instruments are operated: (i) the burst mode which monitors the sky for supernovae, (ii) the detection of electromagnetic showers initiated by PeV-energy cosmic electron neutrinos, and (iii) muon trajectory reconstruction for neutrino and gamma-ray astronomy. We speculate on the possible architectures of kilometer-scale instruments, using early data as a guideline.

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