Source: https://sppgway.jhuapl.edu/biblio
Timestamp: 2019-04-24 00:42:37+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, M. Balat-Pichelin, Marianne Bale, S. Bale, Stuart D.Bale, S. 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, M. Bolton, Mary Bonnell, J. W.Bookbinder, J. Bookbinder, Jay A.Bookbinder, Jay 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, A. W.Case, Anthony 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, Gregory E.Clifford, Greg 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, ML Goldstein, Melvin Goldstein, M. Goldsten, John O.Golub, Leon Good, S. W.Gordon, D. Gordon, Dorothy A.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, J. S.Halekas, Jasper S.Halekas, Jasper 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, Timothy S.Horbury, T Horbury, T SHorbury, T. S.Horbury, Timothy Horn, M. Howard, T. A.Howard, R. A.Howard, Russell A.Howes, Gregory G.Howes, G. G.Hoxie, V. Hoxie, Vaughn C.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, Andrew P.Jordan, Steven P.Joyce, Colin J.Jr., K. H. WrightJr., Edward C. SittlerJude-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, K. G.Klein, Kristopher 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, Davin Larson, D. E.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, T. C.Li, Bo Li, Gang Li, Tak ChuLi, Huichao Li, B. Li, Hui Liang, S. X.Liewer, Paulett C.Lim, Y.-K. Linker, Jon A.Linton, Mark G.Lionello, Roberto Lipatov, Alexander S.Livi, Roberto Livi, S. 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, 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. 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, 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, 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, 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, David Stansby, D Stauffer, Johnathan R.Steinberg, John T.Stenborg, Guillermo Stevens, Michael Stevens, M. L.Stevens, Michael L.Stevens, K. Stevens, Ken 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, M. C.Velli, M. Velli, M. Velli, Marco 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: Wu Honghong, Verscharen Daniel, Wicks Robert T., Chen Christopher H. K., He Jiansen, et al.
Kinetic Alfvén waves (KAWs) are the short-wavelength extension of the magnetohydrodynamics Alfvén-wave branch in the case of highly oblique propagation with respect to the background magnetic field. Observations of space plasma show that small-scale turbulence is mainly KAW-like. We apply two theoretical approaches, a collisional two-fluid theory and a collisionless linear kinetic theory, to obtain predictions for the KAW polarizations depending on β p (the ratio of the proton thermal pressure to the magnetic pressure) at the ion gyroscale in terms of fluctuations in density, bulk velocity, and pressure. We perform a wavelet analysis of Magnetospheric Multiscale magnetosheath measurements and compare the observations with both the. . .
Authors: Le Fur I, De Wit R, Plus M, Oheix J, Derolez V, et al.
ABSTRACT: Since the mid-20th century, Mediterranean lagoons have been affected by eutrophication, leading to significant changes in primary producers. In the early 2000s, management actions have been implemented to reduce nutrient inputs with the aim to achieve a good ecological status as requested by the EU water framework directive. As a result of these actions, a sharp decline in nutrient loads has been recorded in several lagoons leading to an oligotrophication of the water column. The analyses of a long-term data set (1998-2015) of 21 polyhaline and euhaline lagoons with contrasting trophic status allowed us to infer a general scheme for the changes in macrophyte assemblages during the oligotrophication process. Placing hypertrophic and oligotrophic conditions end to end, we inferr. . .
Authors: Stenborg Guillermo, Stauffer Johnathan R., and Howard Russell A.
To test a technique to be used on the white-light imager onboard the recently launched Parker Solar Probe mission, we performed a numerical differentiation of the brightness profiles along the photometric axis of the F-corona models that are derived from STEREO Ahead Sun Earth Connection Heliospheric Investigation observations recorded with the HI-1 instrument between 2007 December and 2014 March. We found a consistent pattern in the derivatives that can be observed from any S/C longitude between about 18° and 23° elongation with a maximum at about 21°. These findings indicate the presence of a circumsolar dust density enhancement that peaks at about 23° elongation. A straightforward integration of the excess signal in the derivative space indicates that the brightness increase over. . .
Authors: Owens Mathew J., Lockwood Mike, Barnard Luke A., and MacNeil Allan R.
In situ spacecraft observations provide much-needed constraints on theories of solar wind formation and release, particularly the highly variable slow solar wind, which dominates near-Earth space. Previous studies have shown an association between local inversions in the heliospheric magnetic field (HMF) and solar wind released from the vicinity of magnetically closed coronal structures. We here show that in situ properties of inverted HMF are consistent with the same hot coronal source regions as the slow solar wind. We propose that inverted HMF is produced by solar wind speed shear, which results from interchange reconnection between a coronal loop and open flux tube, and introduces a pattern of fast─slow─fast wind along a given HMF flux tube. This same loop-opening process is tho. . .
Authors: Graham G. A., Rae I. J., Owen C. J., and Walsh A. P.
Strahl is the strongly field-aligned, beam-like population of electrons in the solar wind. Strahl width is observed to increase with distance from the Sun, and hence strahl electrons must be subject to in-transit scattering effects. Different energy relations have been both observed and modeled for both strahl width and the width increase with radial distance. Thus, there is much debate regarding what mechanism(s) scatter strahl. In this study, we use a novel method to investigate strahl evolution within 1 au by estimating the distance traveled by the strahl along the interplanetary magnetic field (IMF). We do this by implementing methods developed in previous studies, which make use of the onset of solar energetic particles at ̃1 au. Thus, we are able to obtain average strahl broadeni. . .
Using the recently extended 2D improved Particle Acceleration and Transport in the Heliosphere (iPATH) model, we model an example gradual solar energetic particle event as observed at multiple locations. Protons and ions that are energized via the diffusive shock acceleration mechanism are followed at a 2D coronal mass ejection-driven shock where the shock geometry varies across the shock front. The subsequent transport of energetic particles, including cross-field diffusion, is modeled by a Monte Carlo code that is based on a stochastic differential equation method. Time intensity profiles and particle spectra at multiple locations and different radial distances, separated in longitudes, are presented. The results shown here are relevant to the upcoming Parker Solar Probe mission.
In the near future, Parker Solar Probe and Solar Orbiter will provide the first comprehensive in-situ measurements of the solar wind in the inner heliosphere since the Helios mission in the 1970s. We describe a reprocessing of the original Helios ion distribution functions to provide reliable and reproducible data to characterise the proton core population of the solar wind in the inner heliosphere. A systematic fitting of bi-Maxwellian distribution functions was performed to the raw Helios ion distribution function data to extract the proton core number density, velocity, and temperatures parallel and perpendicular to the magnetic field. We present radial trends of these derived proton parameters, forming a benchmark to which new measurements in the inner heliosphere will be compared. . . .
Authors: Winslow Reka M., Schwadron Nathan A., Lugaz é, Guo Jingnan, Joyce Colin J., et al.
Interplanetary coronal mass ejections (ICMEs) often cause Forbush decreases (Fds) in the flux of galactic cosmic rays (GCRs). We investigate how a single ICME, launched from the Sun on 2014 February 12, affected GCR fluxes at Mercury, Earth, and Mars. We use GCR observations from MESSENGER at Mercury, ACE/LRO at the Earth/Moon, and MSL at Mars. We find that Fds are steeper and deeper closer to the Sun, and that the magnitude of the magnetic field in the ICME magnetic ejecta as well as the “strength” of the ICME sheath both play a large role in modulating the depth of the Fd. Based on our results, we hypothesize that (1) the Fd size decreases exponentially with heliocentric distance, and (2) that two-step Fds are more common closer to the Sun. Both hypotheses will be directly verifia. . .
Authors: Xiong Ming, Davies Jackie A., Feng Xueshang, Li Bo, Yang Liping, et al.
Deep-space exploration of the inner heliosphere is in an unprecedented golden age, with the recent and forthcoming launches of the Parker Solar Probe (PSP) and Solar Orbiter (SolO) missions, respectively. In order to both predict and understand the prospective observations by PSP and SolO, we perform forward MHD modeling of the 3D inner heliosphere at solar minimum, and synthesize the white-light (WL) emission that would result from Thomson scattering of sunlight from the coronal and heliospheric plasmas. Both solar rotation and spacecraft trajectory should be considered when reconstructing quiescent large-scale solar-wind streams from PSP and SolO WL observations. When transformed from a static coordinate system into a corotating one, the elliptical orbit of PSP becomes a multiwinding . . .
Spacecraft observations have shown that the proton temperature in the solar wind falls off with radial distance more slowly than expected for an adiabatic prediction. Usually, previous studies have been focused on the evolution of the solar-wind plasma by using the bulk speed as an order parameter to discriminate different regimes. In contrast, here, we study the radial evolution of pure and homogeneous fast streams (i.e. well-defined streams of coronal-hole plasma that maintain their identity during several solar rotations) by means of re-processed particle data, from the HELIOS satellites between 0.3 and 1 au. We have identified 16 intervals of unperturbed high-speed coronal-hole plasma, from three different sources and measured at different radial distances. The observations show tha. . .
Authors: Tsurutani Bruce T., Lakhina Gurbax S., Sen Abhijit, Hellinger Petr, Glassmeier Karl-Heinz, et al.
Solar wind turbulence within high-speed streams is reviewed from the point of view of embedded single nonlinear Alfvén wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase-steepen, with a right-hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of "wave breaking" and the latter that of "period doubling." Interplanetary nonlinear Alfvén waves, which are arc polarized, have a 180° foreshortened front and with an elongated trailing edge. Alfvén waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable fe. . .
We report the presence of intermittent, short discrete enhancements in plasma speed in the near-Sun high-speed solar wind. Lasting tens of seconds to minutes in spacecraft measurements at 0.3 au, speeds inside these enhancements can reach 1000 km s-1, corresponding to a kinetic energy up to twice that of the bulk high-speed solar wind. These events, which occur around 5 per cent of the time, are Alfvénic in nature with large magnetic field deflections and are the same temperature as the surrounding plasma, in contrast to the bulk fast wind which has a well-established positive speed-temperature correlation. The origin of these speed enhancements is unclear but they may be signatures of discrete jets associated with transient events in the chromosphere or corona. Such large s. . .
Solar coronal jets are small, transient, collimated ejections most easily observed in coronal holes (CHs). The upcoming Parker Solar Probe (PSP) mission provides the first opportunity to encounter CH jets in situ near the Sun and examine their internal structure and dynamics. Using projected mission orbital parameters, we have simulated PSP encounters with a fully three-dimensional magnetohydrodynamic (MHD) model of a CH jet. We find that three internal jet regions, featuring different wave modes and levels of compressibility, have distinct identifying signatures detectable by PSP. The leading Alfvén wave front and its immediate wake are characterized by trans-Alfvénic plasma flows with mild density enhancements. This front exhibits characteristics of a fast switch-on MHD shock, whose. . .
In this work we advocate for the idea that two seemingly unrelated 80-year-old mysteries—the nature of dark matter and the high temperature of the million degree solar corona—may have resolutions that lie within the same physical framework. The current paradigm is that the corona is heated by nanoflares, which were originally proposed as miniature versions of the observed solar flares. It was recently suggested that the nanoflares could be identified as annihilation events of the nuggets from the axion quark nugget (AQN) dark matter model. This model was invented as an explanation of the observed ratio Ωdark̃Ωvisible, based only on cosmological and particle physics considerations. In this new paradigm, the AQN particles moving through the coronal plasma and . . .
Authors: Venzmer M. S., and Bothmer V.
Context. The Parker Solar Probe (PSP; formerly Solar Probe Plus) mission will be humanitys first in situ exploration of the solar corona with closest perihelia at 9.86 solar radii (R☉) distance to the Sun. It will help answer hitherto unresolved questions on the heating of the solar corona and the source and acceleration of the solar wind and solar energetic particles. The scope of this study is to model the solar-wind environment for PSPs unprecedented distances in its prime mission phase during the years 2018 to 2025. The study is performed within the Coronagraphic German And US SolarProbePlus Survey (CGAUSS) which is the German contribution to the PSP mission as part of the Wide-field Imager for Solar PRobe. Aim. We present an empirical solar-wind model for the inner hel. . .
Authors: Reid Hamish A. S., and Kontar Eduard P.
A component of space weather, electron beams are routinely accelerated in the solar atmosphere and propagate through interplanetary space. Electron beams interact with Langmuir waves resulting in type III radio bursts. They expand along the trajectory and, using kinetic simulations, we explore the expansion as the electrons propagate away from the Sun. Specifically, we investigate the front, peak, and back of the electron beam in space from derived radio brightness temperatures of fundamental type III emission. The front of the electron beam travels at speeds from 0.2c to 0.7c, significantly faster than the back of the beam, which travels at speeds between 0.12c and 0.35c. The difference in speed between the front and the back elongates the electron beam in time. The rate of beam elonga. . .
In situ measurements of the fast solar wind reveal non-thermal distributions of electrons, protons, and minor ions extending from 0.3 au to the heliopause. The physical mechanisms responsible for these non-thermal properties and the location where these properties originate remain open questions. Here, we present spectroscopic evidence, from extreme ultraviolet spectroscopy, that the velocity distribution functions (VDFs) of minor ions are already non-Gaussian at the base of the fast solar wind in a coronal hole, at altitudes of <1.1 R ☉. Analysis of Fe, Si, and Mg spectral lines reveals a peaked line-shape core and broad wings that can be characterized by a kappa VDF. A kappa distribution fit gives very small kappa indices off-limb of κ ≈ 1.9-2.5, indicating either (. . .

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