scholarly journals Solar wind proton flux latitudinal variations: Comparison between Ulysses in situ data and indirect measurements from interstellar Lyman α mapping

1997 ◽  
Vol 102 (A4) ◽  
pp. 7051-7062 ◽  
Author(s):  
Tuula Summanen ◽  
Rosine Lallement ◽  
Eric Quémerais
Keyword(s):  
Solar Wind ◽  
Proton Flux ◽  
Solar Wind Proton ◽  
Indirect Measurements ◽  
In Situ Data ◽  
Latitudinal Variations

scholarly journals Solar wind dynamics around a comet

2018 ◽  
Vol 620 ◽  
pp. A35 ◽  
Author(s):  
E. Behar ◽  
B. Tabone ◽  
M. Saillenfest ◽  
P. Henri ◽  
J. Deca ◽  
...  
Keyword(s):  
Solar Wind ◽  
Electric Field ◽  
Three Dimensional ◽  
Solar Wind Proton ◽  
In Situ Data ◽  
Collisionless Plasmas ◽  
Rosetta Mission ◽  
Proton Dynamics ◽  
Good Agreement

Aims. We aim at analytically modelling the solar wind proton trajectories during their interaction with a partially ionised cometary atmosphere, not in terms of bulk properties of the flow but in terms of single particle dynamics. Methods. We first derive a generalised gyromotion, in which the electric field is reduced to its motional component. Steady-state is assumed, and simplified models of the cometary density and of the electron fluid are used to express the force experienced by individual solar wind protons during the interaction. Results. A three-dimensional (3D) analytical expression of the gyration of two interacting plasma beams is obtained. Applying it to a comet case, the force on protons is always perpendicular to their velocity and has an amplitude proportional to 1/r2. The solar wind deflection is obtained at any point in space. The resulting picture presents a caustic of intersecting trajectories, and a circular region is found that is completely free of particles. The particles do not lose any kinetic energy and this absence of deceleration, together with the solar wind deflection pattern and the presence of a solar wind ion cavity, is in good agreement with the general results of the Rosetta mission. Conclusions. The qualitative match between the model and the in situ data highlights how dominant the motional electric field is throughout most of the interaction region for the solar wind proton dynamics. The model provides a simple general kinetic description of how momentum is transferred between these two collisionless plasmas. It also shows the potential of this semi-analytical model for a systematic quantitative comparison to the data.

Comparison of Heliospheric In Situ Data with the Quasi‐steady Solar Wind Models

2008 ◽  
Vol 674 (2) ◽  
pp. 1158-1166 ◽  
Author(s):  
S. T. Lepri ◽  
S. K. Antiochos ◽  
P. Riley ◽  
L. Zhao ◽  
T. H. Zurbuchen
Keyword(s):  
Solar Wind ◽  
In Situ Data

Solar Wind Interaction With Jupiter's Magnetosphere: A Statistical Study of Galileo In Situ Data and Modeled Upstream Solar Wind Conditions

2019 ◽  
Vol 124 (12) ◽  
pp. 10170-10199 ◽  
Author(s):  
Marissa F. Vogt ◽  
Szilard Gyalay ◽  
Elena A. Kronberg ◽  
Emma J. Bunce ◽  
William S. Kurth ◽  
...  
Keyword(s):  
Solar Wind ◽  
Statistical Study ◽  
Solar Wind Interaction ◽  
In Situ Data ◽  
Upstream Solar Wind

Forecasting the Dst index from L5 in-situ data using PREDSTORM: accuracy and applicability

2020 ◽  
Author(s):  
Rachel Bailey ◽  
Christian Moestl ◽  
Martin Reiss ◽  
Andreas Weiss ◽  
Ute Amerstorfer ◽  
...  
Keyword(s):  
Solar Wind ◽  
High Speed ◽  
Dst Index ◽  
Wind Speeds ◽  
In Situ Data ◽  
L1 Data ◽  
Earth Environment ◽  
Speed Solar Wind ◽  
Using Data

<p>STEREO-B and STEREO-A are both important proxies for potential solar wind monitors at the Sun-Earth L5 point. In this study, measurements from STEREO-B are used to determine how well the Dst index in particular can be predicted using data measured near the L5 point. This is useful for determining the geoeffectivity of storms resulting from high-speed solar wind streams. Observed solar wind speeds are first mapped to the near-Earth environment as if they had been measured at L1, and the Dst is predicted from the data using a solar wind-to-Dst model. We find that Dst predicted from L5 data performs better than a recurrence model assuming the solar wind conditions repeat every 27 days, although not as well as when predicted from L1 data. The newly developed approach is currently implemented in the PREDSTORM software package to provide a real-time Dst forecast using STEREO-A data.</p>

Solar wind proton flux extremes and their association with pseudostreamers

2013 ◽  
Author(s):  
Liang Zhao ◽  
Sarah E. Gibson ◽  
Lennard A. Fisk
Keyword(s):  
Solar Wind ◽  
Proton Flux ◽  
Solar Wind Proton

Observation of Dust Generated Hydrogen in the Solar Vicinity

1980 ◽  
Vol 91 ◽  
pp. 155-158
Author(s):  
H. J. Fahr ◽  
H. W. Ripken ◽  
G. Lay
Keyword(s):  
Solar Wind ◽  
Neutral Hydrogen ◽  
Interplanetary Dust ◽  
Proton Flux ◽  
Zodiacal Light ◽  
Solar Wind Proton ◽  
Density Profiles ◽  
Spectral Separation ◽  
Spectral Profiles ◽  
Dust Distribution

Solar wind protons impinging on interplanetary dust grains are trapped, deionized, and subsequently desorbed. The steady state distribution of desorbed neutral hydrogen inside of 0.4 AU can be deduced by observation of resonantly scattered solar 121.6 nm radiation. Calculated integral intensities and spectral profiles are given, showing the clear spectral separation of the different radiation components. Given a specific solar wind proton flux, the interplanetary dust distribution can be determined. Conversely, dust density profiles from zodiacal light measurements can be used to deduce solar wind proton fluxes at heliocentric distances of 0.4 to 0.15 AU. Observations of latitudinal and short-term temporal proton flux variations seem feasible.

scholarly journals Influence of the CME orientation on the ICME propagation

2021 ◽  
Author(s):  
Karmen Martinić ◽  
Mateja Dumbović ◽  
Bojan Vršnak
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Weather Forecasting ◽  
Flux Rope ◽  
Meridional Plane ◽  
Space Weather Forecasting ◽  
In Situ Data ◽  
Time Period ◽  
Ambient Solar Wind

<p>Beyond certain distance the ICME propagation becomes mostly governed by the interaction of the ICME and the ambient solar wind. Configuration of the interplanetary magnetic field and features of the related ambient solar wind in the ecliptic and meridional plane are different. Therefore, one can expect that the inclination of the CME flux rope axis i.e. tilt, influences the propagation of the ICME itself. In order to study the relation between the tilt parameter and the ICME propagation we investigated isolated Earth-impacting CME-ICME evets in the time period from 2006. to 2014. We determined the CME tilt in the “near-Sun” environment from the 3D reconstruction of the CME, obtained by the Graduated Cylindrical Shell model using coronagraphic images provided by the STEREO and SOHO missions. We determined the tilt of the ICME in the “near-Earth” environment using in-situ data. We constrained our study to CME-ICME events that show no evidence of rotation while propagating, i.e. have a similar tilt in the “near-Sun” and “near-Earth” environment. We present preliminary results of our study and discuss their implications for space-weather forecasting using the drag-based(ensemble) [DB(E)M] model of heliospheric propagation.</p>

scholarly journals Association of solar wind proton flux extremes with pseudostreamers

2013 ◽  
Vol 118 (6) ◽  
pp. 2834-2841 ◽  
Author(s):  
L. Zhao ◽  
S. E. Gibson ◽  
L. A. Fisk
Keyword(s):  
Solar Wind ◽  
Proton Flux ◽  
Solar Wind Proton

scholarly journals The heliospheric magnetic flux, solar wind proton flux, and cosmic ray intensity during the coming solar minimum

Space Weather ◽  
2014 ◽  
Vol 12 (7) ◽  
pp. 499-507 ◽  
Author(s):  
Charles W. Smith ◽  
K. G. McCracken ◽  
Nathan A. Schwadron ◽  
Molly L. Goelzer
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Solar Minimum ◽  
Cosmic Ray ◽  
Proton Flux ◽  
Solar Wind Proton ◽  
Cosmic Ray Intensity
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