Source: https://sppgway.jhuapl.edu/biblio?s=author&o=asc
Timestamp: 2019-04-24 00:57:34+00:00

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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, S. D.Bale, S. Bale, Stuart D.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, Jay Bookbinder, J. Bookbinder, Jay A.Bothmer, V. Bothmer, Volker Bougeret, J.-L. Bourdin, Philippe Bowen, T. A.Boyle, M. Boyle, M. P.Brandenburg, Axel Brodu, E. Brodu, Etienne 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, Benjamin D. G.Chandran, B. D. G.Charlier, K. Chaston, C. C.Cheimets, Peter Chen, C. H. K.Chen, Christopher H. K.Chen, Yao Chhiber, R Choi, M. K.Christian, E. R.Chua, Damien H.Cirtain, J. W.Cirtain, Jonathan W.Clemens, Adam Clifford, Greg Clifford, Gregory E.Connerney, J. E.Cook, W. R.Cooper, John F.Cooper, S. A.Cranmer, S. Cranmer, Steven R.Cummings, A. C.Curtis, David W.Daigneau, P. S.Daigneau, Peter 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. DeForest, C. E.DeJong, Eric M.Del Amo, Y. Derolez, V Desai, M. I.DeTomaso, David DeVore, Richard Diaz-Aguado, Millan Diaz-Aguado, M. Dickinson, J. Dirks, G. Djordjevic, Blagoje Do, Van TuDo, D. H.Donakowski, W. Donaskowski, Bill Drake, J. F.Driesman, A. Dubois, S. Dumas, F. Dupont, A. R.Eck, J. Effinger, Michael Effinger, M. E.el, H. ̧Elliott, Thomas Emanuel, K. émare, A. émoulin, P. énat, H. énot, V. éo-Vélez, J. C.ère, J.-Y. Ergun, R. Ergun, R. E.Ergun, Robert 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, C. Foullon, Claire Fox, N. Fox, N. J.Fox, Nicola J.Fox, Nichola Freeman, Mark Freeman, M. Froidefond, Jean-Marie Fu, Shuai Gallagher, Dennis Galvin, A. B.Ganthy, Florian Gary, D. Gary, Peter Gates, Richard Gauron, Tom Gauron, T. Génot, V. Gershman, D. J.Giacalone, Joe Giacalone, J. Gilbert, Jason A.Glaser, D. Glassmeier, Karl-Heinz Goelzer, Molly L.Goetz, Keith Goetz, K. Gold, R. E.Gold, Robert E.Goldstein, M. Goldstein, ML Goldstein, Melvin 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, R. S.Gurnee, Reid 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, L. M.Hayes, J. R.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. S.Horbury, Timothy Horbury, Timothy S.Horbury, T Horbury, T SHorn, M. Howard, T. A.Howard, R. A.Howard, Russell A.Howes, Gregory G.Howes, G. 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., Edward C. SittlerJr., K. H. WrightJude-Lemeilleur, Florence Karlsson, Magnus Karlsson, M. Karpen, Judith TKasper, Justin C.Kasper, J. C.Kecman, B. Keller, David Kellogg, P. J.Kien, Mark Kien, M. Kim, Sunjung Kim, D. 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, Hui Li, T. C.Li, Bo Li, Gang Li, Tak ChuLi, Huichao Li, B. 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, Sean Lynch, J. J.Lynnyk, A. MacDowall, R. J.MacNeil, Allan R.Maksimovic, Milan Maksimovic, M. Malaspina, D. M.Malaspina, David M.Malet, N Mallet, Alfred Mannucci, Anthony J.Marchand, R. Marchant, Will Marchant, William Marker, S. Markidis, S. Marshall, Cheryl J.Martin, P. Martinez-Oliveros, J. Maruca, B. A.Maruca, Bennet A.Matéo-Vélez, J.-C. Matteini, L Matteini, Lorenzo Matthaeus, WH Matthaeus, W. H.Matthaeus, H. Maurer, D. Mays, Leila Mazy, Emanuel McCauley, J. McComas, David J.McComas, D McComas, D. J.McDonald, T. McFadden, J. P.McFadden, James P.McNutt, Ralph L.McNutt, R. 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. Parker, E. N.Parker, C. W.Patricola, C. M.Peck, Alison B.Peddie, Andrew M.Perez, Jean C.Perrone, Denise Pevtsov, A. Phan, T. Plunkett, Simon P.Plus, D. Plus, M Plus, M. Plus, Martin Plus, R. Plus, émi Pogorelov, Nikolai Pulupa, M. Quataert, E. Quinn, T. Rae, I. J.Raines, Jim M.Raines, J. 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, Pete Riley, P. Roberts, Merrill ARoberts, M. Roberts, Aaron Robinson, Miles Rochus, Pierre Rochus, Pierre L. P. M.Rodman, Jens Rodmann, Jens Roelof, E. C.Rohner, U Rosen, Irene Rouillard, A. P.Ruffenach, A. Ruplin, S. W.Saint-Hilaire, P. Salem, C. Salem, Chadi 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, Nathan A.Schwadron, N. A.Schwadron, N. 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, K. Stevens, Ken Stevens, Michael Stevens, M. L.Stevens, Michael L.Stewart, R. Stewart, R.G. Stokes, M. R.Stone, E. C.Strachan, L. Strohbehn, K. Sturner, A. Summers, David Summers, D. Sundkvist, D. Swisdak, M. Szabo, A. Szabo, Adam Taylor, Ellen R.Taylor, E. 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, Paul Turin, P. 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, Marco Velli, M. C.Velli, M. Velli, M. 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, H. Wang, Y.-M. Wang, Dennis 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, A. Yehle, Alan Yoon, Peter H.ZALDIVAR, J Zank, Gary Zaslavsky, A. Zhao, M. Zhitnitsky, Ariel Zhou, Yufen Zurbuchen, Thomas H.Zurbuchen, T. H.
Authors: Abbo L., Ofman L., Antiochos S. K., Hansteen V. H., Harra L., et al.
While it is certain that the fast solar wind originates from coronal holes, where and how the slow solar wind (SSW) is formed remains an outstanding question in solar physics even in the post-SOHO era. The quest for the SSW origin forms a major objective for the planned future missions such as the Solar Orbiter and Solar Probe Plus. Nonetheless, results from spacecraft data, combined with theoretical modeling, have helped to investigate many aspects of the SSW. Fundamental physical properties of the coronal plasma have been derived from spectroscopic and imaging remote-sensing data and in situ data, and these results have provided crucial insights for a deeper understanding of the origin and acceleration of the SSW. Advanced models of the SSW in coronal streamers and other structures ha. . .
Alfvénic fluctuations are very common features in the solar wind and are found especially within the main portion of fast-wind streams while the slow wind usually is less Alfvénic and more variable. In general, the fast and slow winds show many differences, which span from the large-scale structure to small-scale phenomena, including also a different turbulent behaviour. Recent studies, however, have shown that even the slow wind can sometimes be highly Alfvénic, with fluctuations as large as those of the fast wind. This study is devoted to presenting many facets of this Alfvénic slow solar wind, including for example the study of the source regions and their connection to coronal structures, large-scale properties, and microscale phenomena and also impact on the spectral features. . . .
Authors: Balat-Pichelin M., Eck J., and Sans J.L.
The Solar Probe Plus (SP+) mission will approach the Sun as close as 9.5 solar radii in order to understand the origin of the solar corona heating and the acceleration of the solar wind. Submitted to such extreme environmental conditions, a thermal protection system is considered to protect the payload of the SP+ spacecraft. Carbon-based materials are good candidate to fulfill this role and critical point remains the equilibrium temperature reached at perihelion by the heat shield. In this paper, experimental results obtained for the solar absorptivity α, the total hemispherical emissivity ɛ and its ratio α/ɛ, conditioning the equilibrium temperature of the thermal protection system, are presented for different kinds of carbon materials heated at . . .
Authors: Balat-Pichelin M., Eck J., Heurtault S., and énat H.
In the frame of future exploration missions such as Solar Probe Plus (NASA) and PHOIBOS (ESA), research was carried out to study pyrolytic BN material envisaged as coating for their heat shields. The physico-chemical behavior of CVD pBN at very high temperature with or without hydrogen ions and VUV (Vacuum Ultra-Violet) irradiations was studied in high vacuum together with the in situ measurement of the thermal radiative properties conditioning the thermal equilibrium of the heat shield. Experimental results obtained on massive pBN samples are presented through in situ mass spectrometry and mass loss rate, and post-test microstructural characterization by XRD, SEM, AFM and nano-indentation techniques, some of them leading to mechanical properties. It could be concluded that synergistic . . .
Authors: Bale S. D., Goetz K., Harvey P. R., Turin P., Bonnell J. W., et al.
NASA's Solar Probe Plus (SPP) mission will make the first in situ measurements of the solar corona and the birthplace of the solar wind. The FIELDS instrument suite on SPP will make direct measurements of electric and magnetic fields, the properties of in situ plasma waves, electron density and temperature profiles, and interplanetary radio emissions, amongst other things. Here, we describe the scientific objectives targeted by the SPP/FIELDS instrument, the instrument design itself, and the instrument concept of operations and planned data products.
NASA has launched a mission to study the Sun’s atmosphere and solar wind that will come far closer to our star than any other craft before.
The solar and space physics community has recently completed its second decadal survey under the auspices of the National Research Council. An integrated strategy for ground and space based studies of the Sun and space physics has been recommended, with specific recommendations made regarding new instrumentation, programs, and facilities. The ground based component of these recommendations is briefly reviewed here: the Advanced Technology Solar Telescope (ATST), the Frequency Agile Solar Radiotelescope (FASR), and the Coronal Solar Magnetism Observatory (COSMO). Although not considered as part of the decadal portfolio, but of which the community should nevertheless be aware, are the Atacama Large Millimeter/submillimeter Array (ALMA) and the Jansky Very Large Array (VLA). Several additi. . .
Authors: Binias Cindy, Do Van Tu, Jude-Lemeilleur Florence, Plus Martin, Froidefond Jean-Marie, et al.
Solar and stellar dynamos shed small-scale and large-scale magnetic helicity of opposite signs. However, solar wind observations and simulations have shown that some distance above the dynamo both the small-scale and large-scale magnetic helicities have reversed signs. With realistic simulations of the solar corona above an active region now being available, we have access to the magnetic field and current density along coronal loops. We show that a sign reversal in the horizontal averages of the magnetic helicity occurs when the local maximum of the plasma beta drops below unity and the field becomes nearly fully force free. Hence, this reversal is expected to occur well within the solar corona and would not directly be accessible to in situ measurements with the Parker Solar Probe or . . .
Authors: Brodu E., and Balat-Pichelin M.
For application to the Solar Probe Plus mission (NASA), the behavior and the thermo-optical performance at very high temperatures (range 1100–2200 K) of candidate passive thermal control materials was assessed. On one hand, a pyrolytic boron nitride coating (130 μm 130 μm thick) was proved to be stable at high temperatures up to 2200 K in vacuum, as well as proved, via total and spectral emissivity measurements at high temperatures, to be able to effectively turn an initially selective solar absorber substrate (carbon/carbon composite) into a solar reflector. On the other hand, chemical vapor deposition coatings made of refractory metals with highly textured surfaces were proved to be able to significantly reduce the temperature of a metall. . .
Authors: Brucker G. J., Herbert J., Stewart R., and Plus D.
This paper reports on the transient photocurrent measurements made with test structures fabricated on sapphire substrates, and the computer simulation model which was developed to use the test results. Predictions of logic upset for a 4 K RAM CMOS/SOS compared with measured upset rates showed agreement within a factor of 2. The test structure results indicate that the sapphire photoconductance is 6.3 x 10 to the -19th mhos/(rads/s)-micron. The use of this value in the present simulation model will increase the predicted upset rate, and thus, increase the disagreement by more than a factor of two.
Authors: Case A. W., Kasper J. C., Daigneau P. S., Caldwell D., Freeman M., et al.
The NASA Solar Probe Plus (SPP) mission will be the first spacecraft to pass through the sub-Alfvénic solar corona. The objectives of the mission are to trace the flow of energy that heats and accelerates the solar corona and solar wind, to determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind, and to explore mechanisms that accelerate and transport energetic particles. The Solar Wind Electrons, Alphas, and Protons (SWEAP) Investigation instrument suite on SPP will measure the bulk solar wind conditions in the inner heliosphere. SWEAP consists of the Solar Probe Cup (SPC), a sun-pointing Faraday Cup, and the Solar Probe ANalyzers (SPAN), a set of 3 electrostatic analyzers that will reside in the penumbra of SPP's thermal protection syst. . .
Authors: Chandran Benjamin D. G.
Simple estimates of the number of Coulomb collisions experienced by the interplanetary plasma to the point of observation, I.e., the “collisional age”, can be usefully employed in the study of non-thermal features of the solar wind. Usually these estimates are based on local plasma properties at the point of observation. Here we improve the method of estimation of the collisional age by employing solutions obtained from global three-dimensional magnetohydrodynamics simulations. This enables evaluation of the complete analytical expression for the collisional age without using approximations. The improved estimation of the collisional timescale is compared with turbulence and expansion timescales to assess the relative importance of collisions. The collisional age computed using the . . .
Chemical thrusters are widely used in spacecraft for attitude control and orbital manoeuvres. They create an exhaust plume of neutral gas which produces ions via photoionization and charge exchange. Measurements of local plasma properties will be affected by perturbations caused by the coupling between the newborn ions and the plasma. A model of neutral expansion has been used in conjunction with a fully three-dimensional hybrid code to study the evolution and ionization over time of the neutral cloud produced by the firing of a mono-propellant hydrazine thruster as well as the interactions of the resulting ion cloud with the ambient solar wind. Results are presented which show that the plasma in the region near to the spacecraft will be perturbed for an extended period of time with the. . .
The Solar Probe Plus ( SPP) mission will explore the Sun's corona and innermost solar wind starting in 2018. The spacecraft will also come close to a number of Mercury-crossing asteroids with perihelia less than 0.3 AU. At small heliocentric distances, these objects may begin to lose mass, thus becoming "active asteroids" with comet-like comae or tails. This paper assembles a database of 97 known Mercury-crossing asteroids that may be encountered by SPP, and it presents estimates of their time-dependent visible-light fluxes and mass loss rates. Assuming a similar efficiency of sky background subtraction as was achieved by STEREO , we find that approximately 80 % of these asteroids are bright enough to be observed by the Wide-field Imager for SPP (WISPR). A model of gas/dust mass loss fr. . .
Authors: Daloz Anne S., Camargo S. J., Kossin J. P., Emanuel K., Horn M., et al.
A realistic representation of the North Atlantic tropical cyclone tracks is crucial as it allows, for example, explaining potential changes in U.S. landfalling systems. Here, the authors present a tentative study that examines the ability of recent climate models to represent North Atlantic tropical cyclone tracks. Tracks from two types of climate models are evaluated: explicit tracks are obtained from tropical cyclones simulated in regional or global climate models with moderate to high horizontal resolution (1°–0.25°), and downscaled tracks are obtained using a downscaling technique with large-scale environmental fields from a subset of these models. For both configurations, tracks are objectively separated into four groups using a cluster technique, leading to a zonal and a merid. . .
Knowledge of the electron density distribution in the solar corona put constraints on the magnetic field configurations for coronal modeling and on initial conditions for solar wind modeling. We work with polarized SOHO/LASCO-C2 images from the last two recent minima of solar activity (1996-1997 and 2008-2010), devoid of coronal mass ejections. The goals are to derive the 4D electron density distributions in the corona by applying a newly developed time-dependent tomographic reconstruction method and to compare the results between the two solar minima and with two magnetohydrodynamic models. First, we confirm that the values of the density distribution in thermodynamic models are more realistic than in polytropic ones. The tomography provides more accurate distributions in the polar reg. . .
Authors: DeForest C. E., Howard T. A., and McComas D. J.
The tenuous supersonic solar wind that streams from the top of the corona passes through a natural boundary—the Alfvén surface—that marks the causal disconnection of individual packets of plasma and magnetic flux from the Sun itself. The Alfvén surface is the locus where the radial motion of the accelerating solar wind passes the radial Alfvén speed, and therefore any displacement of material cannot carry information back down into the corona. It is thus the natural outer boundary of the solar corona and the inner boundary of interplanetary space. Using a new and unique motion analysis to separate inbound and outbound motions in synoptic visible-light image sequences from the COR2 coronagraph on board the STEREO-A spacecraft, we have identified inbound wave motion in the outer co. . .
Authors: Dubois S., Savoye N., émare A., Plus M., Charlier K., et al.
The origin and composition of sediment organic matter (SOM) were investigated together with its spatial distribution in the Arcachon Bay - a macrotidal lagoon that shelters the largest Zostera noltii meadow in Europe - using elemental and isotopic ratios. Subtidal and intertidal sediments and primary producers were both sampled in April 2009. Their elemental and isotopic compositions were assessed. Relative contributions of each source to SOM were estimated using a mixing model. The SOM composition tended to be homogeneous over the whole ecosystem and reflected the high diversity of primary producers in this system. On average, SOM was composed of 25% of decayed phanerogams, 19% of microphytobenthos, 20% of phytoplankton, 19% of river SPOM and 17% of macroalgae. There was no evidence of. . .
Authors: Eck J., Sans J.-L., and Balat-Pichelin M.
The aim of the Solar Probe Plus (SP+) mission is to understand how the solar corona is heated and how the solar wind is accelerated. To achieve these goals, in situ measurements are necessary and the spacecraft has to approach the Sun as close as 9.5 solar radii. This trajectory induces extreme environmental conditions such as high temperatures and intense Vacuum Ultraviolet radiation (VUV). To protect the measurement and communication instruments, a heat shield constituted of a carbon material is placed on the top of the probe. In this study, the physical and chemical behavior of carbon materials is experimentally investigated under high temperatures (1600-2100 K), high vacuum (10-4 Pa) and VUV radiation in conditions near those at perihelion for SP+. Thanks to several in si. . .
Authors: el H. ̧, Motschmann U., üchner J., Narita Y., and Nariyuki Y.
The evolution of the ion-scale plasma turbulence in the inner heliosphere is studied by associating the plasma parameters for hybrid-code turbulence simulations to the radial distance from the Sun via a Solar wind model based mapping procedure. Using a mapping based on a one-dimensional solar wind expansion model, the resulting ion-kinetic scale turbulence is related to the solar wind distance from the Sun. For this purpose the mapping is carried out for various values of ion beta that correspond to the heliocentric distance. It is shown that the relevant normal modes such as ion cyclotron and ion Bernstein modes will occur first at radial distances of about 0.2-0.3 AU, i.e., near the Mercury orbit. This finding can be used as a reference, a prediction to guide the in situ measurements . . .
Authors: Ergun R. E., Malaspina D. M., Bale S. D., McFadden J. P., Larson D. E., et al.
A three-dimensional, self-consistent code is employed to solve for the static potential structure surrounding a spacecraft in a high photoelectron environment. The numerical solutions show that, under certain conditions, a spacecraft can take on a negative potential in spite of strong photoelectron currents. The negative potential is due to an electrostatic barrier near the surface of the spacecraft that can reflect a large fraction of the photoelectron flux back to the spacecraft. This electrostatic barrier forms if (1) the photoelectron density at the surface of the spacecraft greatly exceeds the ambient plasma density, (2) the spacecraft size is significantly larger than local Debye length of the photoelectrons, and (3) the thermal electron energy is much larger than the characterist. . .
The fast solar wind shows a wide spectrum of transverse magnetic and velocity field perturbations. These perturbations are strongly correlated in the sense of Alfvén waves propagating mostly outward, from the Sun to the interplanetary medium. They are likely to be fundamental to the acceleration and the heating of the solar wind. However, the precise origin of the broadband spectrum is unknown to date. Typical periods of chromospheric Alfvén waves are limited to a few minutes, and any longer period perturbations should be strongly reflected at the transition region. In this work, we show that minute long Alfvénic fluctuations are unstable to the parametric instability. Parametric instability enables an inverse energy cascade by exciting several-hour-long periods of Alfvénic fluctuat. . .
Authors: Fox N. J., Velli M. C., Bale S. D., Decker R., Driesman A., et al.
Solar Probe Plus (SPP) will be the first spacecraft to fly into the low solar corona. SPP's main science goal is to determine the structure and dynamics of the Sun's coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Understanding these fundamental phenomena has been a top-priority science goal for over five decades, dating back to the 1958 Simpson Committee Report. The scale and concept of such a mission has been revised at intervals since that time, yet the core has always been a close encounter with the Sun. The mission design and the technology and engineering developments enable SPP to meet its science objectives to: (1) Trace the flow of energy that heats and accelerates the sola. . .

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