Source: https://sppgway.jhuapl.edu/biblio?s=title&o=asc
Timestamp: 2019-04-24 00:27:03+00:00

Document:
Author anyAbbo, L. Abiad, Robert Afanasiev, Alexandr Alexander, N. Allegrini, F Amicis, Raffaella ’Andre, M. Andrews, G. B.Angold, N. Antiochos, S. K.ányi, M. Ao, Xianzhi Auby, I. Austin, Gerry Balat-Pichelin, Marianne Balat-Pichelin, M. Bale, Stuart D.Bale, S. D.Bale, S. Banks, Michael Barnard, Luke A.Bastian, T. S.Bastian, T. Battarbee, Markus Beebe, C. Begley, S. M.Belcher, John W.Beltoise, A. Benn, Chris R.Berg, Peter Bergner, Henry Berthomier, Matthieu Binias, Cindy Birdwell, B. Blanchet, H. Bolton, Mary Bolton, M. Bonnell, J. W.Bookbinder, J. Bookbinder, Jay A.Bookbinder, Jay Bothmer, V. Bothmer, Volker Bougeret, J.-L. Bourdin, Philippe Bowen, T. A.Boyle, M. P.Boyle, M. Brandenburg, Axel Brodu, Etienne Brodu, E. Brucker, G. J.Bruno, Roberto Burgess, D. Burgess, David Burgum, J. M.Burkpile, J. Burnham, J. A.ć, Zoran Caldwell, D. Caldwell, David Camargo, S. J.Carruth, N. Carter, Michael T.Case, Anthony W.Case, A. W.Cattell, C. A.Chandran, B. D. G.Chandran, Benjamin D. G.Charlier, K. Chaston, C. C.Cheimets, Peter Chen, Christopher H. K.Chen, Yao Chen, C. H. K.Chhiber, R Choi, M. K.Christian, E. R.Chua, Damien H.Cirtain, Jonathan W.Cirtain, J. W.Clemens, Adam Clifford, Gregory E.Clifford, Greg Connerney, J. E.Cook, W. R.Cooper, S. A.Cooper, John F.Cranmer, S. Cranmer, Steven R.Cummings, A. C.Curtis, David W.Daigneau, Peter Daigneau, P. S.Daloz, Anne S.Dalton, Greg Dasgupta, Brahmananda Dasso, S. Davies, Jackie A.Davis, A. J.de Montaudouin, Xavier de Patoul, Judith De Wit, R de Wit, T. Deca, J. Decker, R. B.Decker, R. DeForest, C. E.Deforest, C. DeJong, Eric M.Del Amo, Y. Derolez, V Desai, M. I.DeTomaso, David DeVore, Richard Diaz-Aguado, M. Diaz-Aguado, Millan Dickinson, J. Dirks, G. Djordjevic, Blagoje Do, D. H.Do, Van TuDonakowski, W. Donaskowski, Bill Drake, J. F.Driesman, A. Dubois, S. Dumas, F. Dupont, A. R.Eck, J. Effinger, M. E.Effinger, Michael el, H. ̧Elliott, Thomas Emanuel, K. émare, A. émoulin, P. énat, H. énot, V. éo-Vélez, J. C.ère, J.-Y. Ergun, Robert E.Ergun, R. Ergun, R. E.éville, Victor Farrell, W. M.Farrugia, C. J.Feldman, William C.Feng, Xueshang Fennelly, Judy Fergeau, P. Fermin, J. Fineschi, Silvano Fischer, J. Fletcher, Lyndsay Florinski, Vladimir Forsyth, R. J.Foullon, Claire Foullon, C. Fox, N. J.Fox, Nichola Fox, Nicola J.Fox, N. Freeman, M. Freeman, Mark Froidefond, Jean-Marie Fu, Shuai Gallagher, Dennis Galvin, A. B.Ganthy, Florian Gary, Peter Gary, D. Gates, Richard Gauron, Tom Gauron, T. Génot, V. Gershman, D. J.Giacalone, J. Giacalone, Joe Gilbert, Jason A.Glaser, D. Glassmeier, Karl-Heinz Goelzer, Molly L.Goetz, Keith Goetz, K. Gold, Robert E.Gold, R. E.Goldstein, Melvin Goldstein, M. Goldstein, ML Goldsten, John O.Golub, Leon Good, S. W.Gordon, Dorothy A.Gordon, D. Graham, G. A.Grey, Phares J.Grygon, Mark Guillemant, S. Guo, Jingnan Guo, Yanping Guo, Fan Gurnee, Reid Gurnee, R. S.Guth, Giora Haggerty, D. K.Hagood, Robert Hahn, Michael Halekas, Jasper Halekas, J. S.Halekas, Jasper S.Hall, Jeffrey R.Hanson, E. Hansteen, V. H.Harra, L. Harris, S. E.Harrison, Richard A.Hartle, Richard E.Harvey, P. R.Hatch, Ken Hayashi, Keiji Hayes, J. R.Hayes, L. M.He, Jiansen Heerikuisen, Jacob Hellinger, Petr Herbert, J. Heurtault, S. Hilgers, A. Hill, M. E.Hinze, J. J.Ho, George Hoffer, E. M.Hollweg, J. V.Horbury, T SHorbury, T. S.Horbury, Timothy Horbury, Timothy S.Horbury, T Horn, M. Howard, Russell A.Howard, T. A.Howard, R. A.Howes, G. G.Howes, Gregory G.Hoxie, Vaughn C.Hoxie, V. Hu, Qiang Hu, Junxiang Hull, A. Hutcheson, J. C.Hwang, Junga ínez-Oliveros, J. C.Isenberg, Philip A.Issautier, K. Janesick, James J.Jannet, G. Jaskulek, S. E.Jeffrey, Natasha L. S.Johnson, Greg Jonas, J. A.Jordan, Steven P.Jordan, Andrew P.Joyce, Colin J.Jr., K. H. WrightJr., Edward C. SittlerJude-Lemeilleur, Florence Karlsson, M. Karlsson, Magnus Karpen, Judith TKasper, J. C.Kasper, Justin C.Kecman, B. Keller, David Kellogg, P. J.Kien, Mark Kien, M. Kim, D. Kim, Sunjung Kinnison, J. Klein, Kristopher G.Klein, K. G.Klemic, J. Klimchuk, J. A.Ko, Y.-K. Kombiadou, Katerina Kong, Xiangliang Kontar, Eduard P.Korendyke, Clarence M.Korreck, K. E.Korreck, Kelly E.Koskinen, Hannu E. J.Kossin, J. P.Krasnoselskikh, V. V.Krimigis, S. M.Krucker, S. Kusterer, M. Kuznetsov, V.D. Labrador, A. W.Laitinen, Timo Lakhina, Gurbax S.Lamy, Philippe Lapenta, G. Lario, D. LaRow, T. Larson, D. E.Larson, Davin Lavraud, B. Lawrence, David J.Layman, R. S.Lazarus, A. J.Lazarus, Alan J.Le Fur, I Lee, Jaejin Leibacher, J. Leske, R. A.Li, Bo Li, Tak ChuLi, Huichao Li, B. Li, Hui Li, T. C.Li, Gang Liang, S. X.Liewer, Paulett C.Lim, Y.-K. Linker, Jon A.Linton, Mark G.Lionello, Roberto Lipatov, Alexander S.Livi, S. Livi, Roberto Lockwood, M. K.Lockwood, Mike London, S. M.Louarn, P. Ludlam, Micheal Ludlam, Michael Lugaz, é Luhmann, J. G.Lutz, M. Lynch, J. J.Lynch, Sean Lynnyk, A. MacDowall, R. J.MacNeil, Allan R.Maksimovic, M. Maksimovic, Milan Malaspina, David M.Malaspina, D. M.Malet, N Mallet, Alfred Mannucci, Anthony J.Marchand, R. Marchant, William Marchant, Will Marker, S. Markidis, S. Marshall, Cheryl J.Martin, P. Martinez-Oliveros, J. Maruca, B. A.Maruca, Bennet A.Matéo-Vélez, J.-C. Matteini, Lorenzo Matteini, L Matthaeus, W. H.Matthaeus, WH Matthaeus, H. Maurer, D. Mays, Leila Mazy, Emanuel McCauley, J. McComas, David J.McComas, D. J.McComas, D McDonald, T. McFadden, James P.McFadden, J. P.McNutt, R. L.McNutt, Ralph L.Mercer, Tony Messina, Luciana Mewaldt, R. A.Meyer-Vernet, N. Mikic, Zoran Mitchell, D. G.Miyake, Y. Moncuquet, M. Monson, S. J.Morrill, Jeff S.Motschmann, U. Mozer, F. S.Murphy, S. D.Narita, Y. Nariyuki, Y. Nelson, K. S.Nicolaou, Georgios Noble, M. W.Odom, J. Ofman, L. Oheix, J Oliverson, R. Olson, J. önni, Arttu ópez, Rodrigo A.Oran, R. Ouisse, V Owen, C. J.Owens, M. J.Owens, Mathew J.Pankow, D. Park, Sang Parker, C. W.Parker, C. Parker, E. N.Patricola, C. M.Peck, Alison B.Peddie, Andrew M.Perez, Jean C.Perrone, Denise Pevtsov, A. Phan, T. Plunkett, Simon P.Plus, Martin Plus, R. Plus, émi Plus, D. Plus, M Plus, M. Pogorelov, Nikolai Pulupa, M. Quataert, E. Quinn, T. Rae, I. J.Raines, J. M.Raines, Jim M.Rankin, J. S.Raouafi, N. Raouafi, N. E.Rasca, A. P.Raza, Nayyer Reid, Hamish A. S.Reinhart, Matthew J.Rich, Nathan Richardson, John D.Riley, P. Riley, Pete Roberts, M. Roberts, Aaron Roberts, Merrill ARobinson, Miles Rochus, Pierre L. P. M.Rochus, Pierre Rodman, Jens Rodmann, Jens Roelof, E. C.Rohner, U Rosen, Irene Rouillard, A. P.Ruffenach, A. Ruplin, S. W.Saint-Hilaire, P. Salem, Chadi Salem, C. Sans, J.-L. Sans, J.L. Saul, L Sauvaud, J.-A. Savani, N. P.Savin, Daniel W.Savoye, N. Scheer, J Schlemm, C. E.Schwadron, N. A.Schwadron, N. A.Schwadron, Nathan A.Scoccimarro, E. Seaman, Robert L.Seifert, H. Seitz, D. Sen, Abhijit Shaevitz, D. Shearer, Paul Sheppard, D. A.Shuman, S. Simier, M Singh, Nishant K.Siy, A. Skoug, Ruth M.Slagle, Amanda Slavin, J. A.Smith, Charles W.Socker, Dennis G.Sottolichio, Aldo Spence, Harlan E.Stansby, D Stansby, David Stauffer, Johnathan R.Steinberg, John T.Stenborg, Guillermo Stevens, Michael L.Stevens, K. Stevens, Michael Stevens, Ken Stevens, M. L.Stewart, R. Stewart, R.G. Stokes, M. R.Stone, E. C.Strachan, L. Strohbehn, K. Sturner, A. Summers, D. Summers, David Sundkvist, D. Swisdak, M. Szabo, Adam Szabo, A. Taylor, E. R.Taylor, Ellen R.TenBarge, J. M.Tenerani, Anna Thernisien, Arnaud F. R.Thouvenin, B. Thurn, Adam Timofeeva, M. Tiu, Chris Tower, John Tracy, Patrick J.Trut, G. Tsurutani, Bruce T.Tun, Samuel Turin, P. Turin, Paul üchner, J. Uritsky, Vadim MUsmanov, AV Usui, H. Vainio, Rami Vaivads, A. Van Duyne, Peter Van Waerbeke, Ludovic Vandegriff, J. D.Vasquez, Bernard J.Velli, M. Velli, Marco Velli, M. Velli, M. C.Venzmer, M. S.Verney, Romaric Verscharen, Daniel Vidale, P. L.von Rosenvinge, T. T.von Steiger, R. Vourlidas, Angelos Waczynski, Augustyn Walsh, A. P.Wang, Y.-M. Wang, Dennis Wang, H. Webb, Gary Weber, T. Wehner, M. Weidner, S. E.Werthimer, D. Westlake, J. H.Weygand, M. Whittlesey, Phyllis Wicks, Robert T.Wiedenbeck, M. E.Wilson, Jody K.Wilson, P. Wimmer-Schweingruber, Robert F.Winslow, Reka M.Witze, Alexandra Wright, Ken Wu, Honghong Wu, S. T.Wurz, P Wygant, J. R.Xia, Lidong Xiong, Ming Yang, Liping Yehle, Alan Yehle, A. Yoon, Peter H.ZALDIVAR, J Zank, Gary Zaslavsky, A. Zhao, M. Zhitnitsky, Ariel Zhou, Yufen Zurbuchen, T. H.Zurbuchen, Thomas H.
Authors: Stewart R.G., and Plus D.
New high-performance CMOS circuit techniques have been developed and used to build an 8K E/SUP 2/PROM with an access time of 38 ns at 5 V. Using standard CMOS/SOS technology, the device dissipates only 0.8 mW quiescent power at 5 V and 60 mW at 1 MHz. A midpoint precharge and sense technique permits operation form a supply voltage of 4-12 V.
Recent observations have shown that coronal shocks driven by coronal mass ejections can develop and accelerate particles within several solar radii in large solar energetic particle (SEP) events. Motivated by this, we present an SEP acceleration study that including the process in which a fast shock propagates through a streamer-like magnetic field with both closed and open field lines in the low corona region. The acceleration of protons is modeled by numerically solving the Parker transport equation with spatial diffusion both along and across the magnetic field. We show that particles can be sufficiently accelerated to up to several hundred MeV within 2-3 solar radii. When the shock propagates through a streamer-like magnetic field, particles are more efficiently accelerated compared. . .
We present a new data analysis method enabling the observation of magnetic field fluctuations associated with temperature anisotropy instabilities using the Ulysses spacecraft. The movement of the spacecraft away from the Sun causes the observed plasma conditions, turbulent fluctuation amplitude, magnetic field strength and important physical scales to change. We normalize wavelet power spectra of the magnetic field using local values for the proton gyroscale and large scale magnetic field fluctuation amplitude to remove the effects of varying heliocentric distance. We recover the enhancement of magnetic fluctuations where temperature anisotropy instability growth rates are large, as seen by previous studies in the ecliptic at 1 AU. This method can be applied to any spacecraft data that. . .
Authors: Goelzer Molly L., Schwadron Nathan A., and Smith Charles W.
The Solar Probe Plus mission now under construction will provide the first in situ measurements from inside the orbit of Mercury. The most critical part of that mission will be measurements from inside the Alfvén radius where the Alfvén speed exceeds the wind speed and the physics of the solar wind changes fundamentally due, in part, to the multidirectionality of wave propagation. In this region waves from both sunward and antisunward of the observation point can effect the local dynamics including the turbulent evolution, heating, and acceleration of the plasma. While the location of this point can change with solar wind conditions, we ask the question of whether there is a systematic dependence on the solar cycle that moves the average Alfvén radius to different locations depending. . .
Authors: Tracy Patrick J., Kasper Justin C., Raines Jim M., Shearer Paul, Gilbert Jason A., et al.
We analyze the heavy ion components (A >4 amu ) in collisionally young solar wind plasma and show that there is a clear, stable dependence of temperature on mass, probably reflecting the conditions in the solar corona. We consider both linear and power law forms for the dependence and find that a simple linear fit of the form Ti/Tp=(1.35 ±.02 )mi/mp describes the observations twice as well as the equivalent best fit power law of the form Ti/Tp=(mi/mp) 1.07 ±.01 . Most importantly we find that current model predictions based on turbulent transport and kinetic dissipation are in agreement with observed nonthermal heating in intermediate collisional age plasma for m /q <3.5 , but are . . .
The expansion of a coronal hole filled with a discrete number of higher density coronal plumes is simulated using a time-dependent two-dimensional code. A solar wind model including an exponential coronal heating function and a flux of Alfvén waves propagating both inside and outside the structures is taken as a basic state. Different plasma plume profiles are obtained by using different scale heights for the heating rates. Remote sensing and solar wind in situ observations are used to constrain the parameter range of the study. Time dependence due to plume ignition and disappearance is also discussed. Velocity differences of the order of ~50 km s-1, such as those found in microstreams in the high-speed solar wind, may be easily explained by slightly different heat depositio. . .
Authors: Marchand R., Miyake Y., Usui H., Deca J., Lapenta G., et al.
Five spacecraft-plasma models are used to simulate the interaction of a simplified geometry Solar Probe Plus (SPP) satellite with the space environment under representative solar wind conditions near perihelion. By considering similarities and differences between results obtained with different numerical approaches under well defined conditions, the consistency and validity of our models can be assessed. The impact on model predictions of physical effects of importance in the SPP mission is also considered by comparing results obtained with and without these effects. Simulation results are presented and compared with increasing levels of complexity in the physics of interaction between solar environment and the SPP spacecraft. The comparisons focus particularly on spacecraft floating po. . .
The Parker Solar Probe will dive into the sizzling solar corona to explore its mysteries.
Turbulence plays a key role in the conversion of the energy of large-scale fields and flows to plasma heat, impacting the macroscopic evolution of the heliosphere and other astrophysical plasma systems. Although we have long been able to make direct spacecraft measurements of all aspects of the electromagnetic field and plasma fluctuations in near-Earth space, our understanding of the physical mechanisms responsible for the damping of the turbulent fluctuations in heliospheric plasmas remains incomplete. Here we propose an innovative field-particle correlation technique that can be used to measure directly the secular energy transfer from fields to particles associated with collisionless damping of the turbulent fluctuations. Furthermore, this novel procedure yields information about th. . .
Robustly identifying the solar sources of individual packets of solar wind measured in interplanetary space remains an open problem. We set out to see if this problem is easier to tackle using solar wind measurements closer to the Sun than 1 au, where the mixing and dynamical interaction of different solar wind streams is reduced. Using measurements from the Helios mission, we examined how the proton core temperature anisotropy and cross-helicity varied with distance. At 0.3 au there are two clearly separated anisotropic and isotropic populations of solar wind that are not distinguishable at 1 au. The anisotropic population is always Alfvénic and spans a wide range of speeds. In contrast the isotropic population has slow speeds, and contains a mix of Alfvénic wind with constant mass f. . .
Authors: Malaspina David M., Ergun Robert E., Bolton Mary, Kien Mark, Summers David, et al.
The first in situ measurements of electric and magnetic fields in the near-Sun environment (< 0.25 AU from the Sun) will be made by the FIELDS instrument suite on the Solar Probe Plus mission. The Digital Fields Board (DFB) is an electronics board within FIELDS that performs analog and digital signal processing, as well as digitization, for signals between DC and 60 kHz from five voltage sensors and four search coil magnetometer channels. These nine input signals are processed on the DFB into 26 analog data streams. A specialized application-specific integrated circuit performs analog to digital conversion on all 26 analog channels simultaneously. The DFB then processes the digital data using a field programmable gate array (FPGA), generating a variety of data products, including dig. . .
Authors: Li T. C., Drake J. F., and Swisdak M.
Observations of flare-heated electrons in the corona typically suggest confinement of electrons. The confinement mechanism, however, remains unclear. The transport of coronal hot electrons into ambient plasma was recently investigated by particle-in-cell (PIC) simulations. Electron transport was significantly suppressed by the formation of a highly localized, nonlinear electrostatic potential in the form of a double layer (DL). In this work large-scale PIC simulations are performed to explore the dynamics of DLs in larger systems where, instead of a single DL, multiple DLs are generated. The primary DL accelerates return current electrons, resulting in high velocity electron beams that interact with ambient ions. This forms a Buneman unstable system that spawns more DLs. Trapping of hea. . .
Authors: Fox Nicola J., and McComas David J.
The Solar Probe Plus mission is a remarkable and historic step in the exploration of humankind. We have visited all of the planets and a number of other smaller moons and bodies; we have explored the magnetospheres, not just of Earth but also of all the planets; and we have explored our heliosphere and even flown a spacecraft beyond its boundary and into interstellar space itself. However, only with the launch of Solar Probe Plus will we actually visit our own star—the Sun—repeatedly traveling to within 9 solar radii (R S RS ) of its surface (10R S 10RS heliocentric) and directly through its corona. From here, we will at long last be able to solve the key mysteries that have puzzled scientists for over 50 years: how the corona is heated and how the so. . .
The inner magnetosphere including the radiation belt and ring current environment is replete with high-frequency fluctuations with peak intensity occurring near upper-hybrid frequency and/or multiple harmonic electron cyclotron frequencies above and below the upper-hybrid frequency. Past and contemporary spacecraft missions, including the Van Allen Probes, were designed to detect the electric field spectrum only for these high-frequency fluctuations. Making use of the recently formulated generalized theory of electromagnetic spontaneous emission in thermal magnetized plasmas, it is shown that upper-hybrid/multiple harmonic electron cyclotron emissions are characterized by a significant magnetic field component, even in the high-frequency regime. Such a prediction may potentially be test. . .
Authors: Matthaeus H., Weygand M., and Dasso S.
Single point measurement turbulence cannot distinguish variations in space and time. We employ an ensemble of one- and two-point measurements in the solar wind to estimate the space-time correlation function in the comoving plasma frame. The method is illustrated using near Earth spacecraft observations, employing ACE, Geotail, IMP-8, and Wind data sets. New results include an evaluation of both correlation time and correlation length from a single method, and a new assessment of the accuracy of the familiar frozen-in flow approximation. This novel view of the space-time structure of turbulence may prove essential in exploratory space missions such as Solar Probe Plus and Solar Orbiter for which the frozen-in flow hypothesis may not be a useful approximation.
Authors: Lario D., and Decker R. B.
A method to estimate both solar energetic particle mission-integrated fluences and solar energetic particle peak intensities for missions traveling through the innermost part of the heliosphere (r < 1 AU) is presented. By using (1) an extensive data set of particle intensities measured at 1 AU over the last three solar cycles, (2) successive launch dates for the mission traveling close to the Sun over the time interval spanned by our data set, and (3) appropriate radial dependences to extrapolate fluences and peak intensities measured at 1 AU to the heliocentric radial distance of the mission at each specific time, we generate distributions of both mission-integrated fluences and maximum peak intensities. From these distributions we extract the values of mission-integrated fluence an. . .
A method to estimate the total fluence of solar flare neutrons at a spacecraft traveling in the innermost part of the heliosphere (at heliocentric radial distances of <1 AU) is presented. The results of the neutron production and emissivity codes of Hua and Lingenfelter (1987a, 1987b) scaled to one of the largest solar neutron events ever observed at the Earth are used to derive a conservative estimate of the energy spectrum of neutrons emitted from the Sun after a large solar flare. By taking into account the survival probability of a neutron to reach a certain heliocentric distance, we evaluate the observed time-integrated spectrum of solar neutrons as a function of the heliocentric distance of the observer. By considering (1) a working relationship between the soft X-ray class of . . .
The infrared spectra of pure Mg(NH3)6Cl2 and Mg(ND3)6Cl2 were recorded from 4 000 to 50 cm-1 at 40 and — 180 °C. The observed bands are assigned. The hydrogenated compound was studied by differential thermal analysis.
The observed infrared spectral data are compared with the previously reported experimental values for other divalent metals (Co2+, Ni2+, Fe2+, Mn2+). This comparison proves that (he coordination bond is stronger for Mg than for the other metals.
L'auteur a pu obtenir les fréquences des vibrations actives en diffusion Raman du chlorure de magnésium hexa‐amminé hydrogéné et deutérié à l'état cristallisé. Toutes les vibrations attendues ont pu être observées pour la première fois pour un composé de ce type (vibrations internes et vibrations externes). L'attribution de toutes les bandes du spectre est proposée. Ces résultats, rapprochés de ceux obtenus par spectroscopie infrarouge, permettent de connaître la structure vibrationnelle complète du complexe. L'éclatement de certaines vibrations montre que les coordinats ne sont pas en rotation libre et que leur orientation donne à l'ion complexe la symétrie du groupe ponctuel D3d.

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