scholarly journals The solar WIND and suprathermal ion composition investigation on the WIND spacecraft

1995 ◽  
Vol 71 (1-4) ◽  
pp. 79-124 ◽  
Author(s):  
G. Gloeckler ◽  
H. Balsiger ◽  
A. B�rgi ◽  
P. Bochsler ◽  
L. A. Fisk ◽  
...  
Keyword(s):  
Solar Wind ◽  
Ion Composition ◽  
Wind Spacecraft

The solar wind interaction with Mars: Consideration of Phobos 2 mission observations of an ion composition boundary on the dayside

1991 ◽  
Vol 96 (A7) ◽  
pp. 11165 ◽  
Author(s):  
T. K. Breus ◽  
A. M. Krymskii ◽  
R. Lundin ◽  
E. M. Dubinin ◽  
J. G. Luhmann ◽  
...  
Keyword(s):  
Solar Wind ◽  
Ion Composition ◽  
Solar Wind Interaction

Solar Wind Ion Composition

1968 ◽  
Vol 20 (8) ◽  
pp. 393-395 ◽  
Author(s):  
S. J. Bame ◽  
A. J. Hundhausen ◽  
J. R. Asbridge ◽  
I. B. Strong
Keyword(s):  
Solar Wind ◽  
Ion Composition

scholarly journals Experimental and numerical investigation of plasma parameters in the magnetosheath

2018 ◽  
Vol 145 ◽  
pp. 03003
Author(s):  
Polya Dobreva ◽  
Monio Kartalev ◽  
Olga Nitcheva ◽  
Natalia Borodkova ◽  
Georgy Zastenker
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Numerical Investigation ◽  
Euler Equations ◽  
Ideal Gas ◽  
Bow Shock ◽  
Plasma Parameters ◽  
Wind Spacecraft ◽  
The Magnetic Field ◽  
Good Agreement

We investigate the behaviour of the plasma parameters in the magnetosheath in a case when Interball-1 satellite stayed in the magnetosheath, crossing the tail magnetopause. In our analysis we apply the numerical magnetosheath-magnetosphere model as a theoretical tool. The bow shock and the magnetopause are self-consistently determined in the process of the solution. The flow in the magnetosheath is governed by the Euler equations of compressible ideal gas. The magnetic field in the magnetosphere is calculated by a variant of the Tsyganenko model, modified to account for an asymmetric magnetopause. Also, the magnetopause currents in Tsyganenko model are replaced by numericaly calulated ones. Measurements from WIND spacecraft are used as a solar wind monitor. The results demonstrate a good agreement between the model-calculated and measured values of the parameters under investigation.

scholarly journals 3-D reconstructions of the early-November 2004 CDAW geomagnetic storms: analysis of Ooty IPS speed and density data

2009 ◽  
Vol 27 (12) ◽  
pp. 4479-4489 ◽  
Author(s):  
M. M. Bisi ◽  
B. V. Jackson ◽  
J. M. Clover ◽  
P. K. Manoharan ◽  
M. Tokumaru ◽  
...  
Keyword(s):  
Solar Wind ◽  
Geomagnetic Storms ◽  
Interplanetary Space ◽  
Tomographic Reconstruction ◽  
Three Dimensional ◽  
Reconstruction Technique ◽  
The Sun ◽  
Wide Range ◽  
Digital Resolution ◽  
Wind Spacecraft

Abstract. Interplanetary scintillation (IPS) remote-sensing observations provide a view of the solar wind covering a wide range of heliographic latitudes and heliocentric distances from the Sun between ~0.1 AU and 3.0 AU. Such observations are used to study the development of solar coronal transients and the solar wind while propagating out through interplanetary space. They can also be used to measure the inner-heliospheric response to the passage of coronal mass ejections (CMEs) and co-rotating heliospheric structures. IPS observations can, in general, provide a speed estimate of the heliospheric material crossing the observing line of site; some radio antennas/arrays can also provide a radio scintillation level. We use a three-dimensional (3-D) reconstruction technique which obtains perspective views from outward-flowing solar wind and co-rotating structure as observed from Earth by iteratively fitting a kinematic solar wind model to these data. Using this 3-D modelling technique, we are able to reconstruct the velocity and density of CMEs as they travel through interplanetary space. For the time-dependent model used here with IPS data taken from the Ootacamund (Ooty) Radio Telescope (ORT) in India, the digital resolution of the tomography is 10° by 10° in both latitude and longitude with a half-day time cadence. Typically however, the resolutions range from 10° to 20° in latitude and longitude, with a half- to one-day time cadence for IPS data dependant upon how much data are used as input to the tomography. We compare reconstructed structures during early-November 2004 with in-situ measurements from the Wind spacecraft orbiting the Sun-Earth L1-Point to validate the 3-D tomographic reconstruction results and comment on how these improve upon prior reconstructions.

Implantation of ions escaping the atmosphere of Mars within the regolith of Phobos, and Phobos’ surface ion weathering

2020 ◽  
Author(s):  
Quentin Nénon ◽  
Andrew R Poppe ◽  
Ali Rahmati ◽  
James P McFadden
Keyword(s):  
Solar Wind ◽  
Atomic Oxygen ◽  
The Moon ◽  
Ion Composition ◽  
Atmospheric Escape ◽  
The Past ◽  
Lunar Samples ◽  
Singly Charged

<p>Mars has lost and is losing its atmosphere into space. Strong evidences of this come from the observation of planetary singly charged heavy ions (atomic oxygen, molecular oxygen, carbon dioxide ions) by Mars Express and MAVEN. Phobos, the closest moon of Mars, orbits only 6,000 kilometers above the red planet’s surface and is therefore a unique vantage point of the planetary atmospheric escape, with the escaping ions being implanted within the regolith of Phobos and altering the properties of the moon’s surface.</p> <p>In this presentation, we aggregate all ion observations gathered in-situ close to the orbit of Phobos by three ion instruments onboard MAVEN, from 2015 to 2019, to constrain the long-term averaged ion environment seen by the Martian moon at all longitudes along its orbit. In particular, the SupraThermal and Thermal Ion Composition (STATIC) instrument onboard MAVEN distinguishes between solar wind and planetary ions. The newly constrained long-term ion environment seen by Phobos is combined with numerical simulations of ion transport and effects in matter.</p> <p>This way, we find that planetary ions are implanted on the near side of Phobos (pointing towards Mars) inside the uppermost tens of nanometers of regolith grains. The composition of near-side grains that may be sampled by future Phobos sample return missions is therefore not only contaminated by planetary ions, as seen in lunar samples with the terrestrial atmosphere, but may show a unique record of the past atmosphere of Mars.</p> <p>The long-term fluxes of planetary ions precipitating onto Phobos are so intense that these ions weather the moon’s surface as much as or more than solar wind ions. In particular, Martian ions accelerate the long-term sputtering and amorphization of the near side regolith by a factor of 2. Another implication is that ion weathering is highly asymmetric between the near side and far side of Phobos.</p>

Solar Wind Ion Composition

1970 ◽  
Vol 75 (31) ◽  
pp. 6354-6359 ◽  
Author(s):  
T. E. Holzer ◽  
W. I. Axford
Keyword(s):  
Solar Wind ◽  
Ion Composition

scholarly journals Composition of quasi-stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer

2000 ◽  
Vol 105 (A12) ◽  
pp. 27217-27238 ◽  
Author(s):  
R. von Steiger ◽  
N. A. Schwadron ◽  
L. A. Fisk ◽  
J. Geiss ◽  
G. Gloeckler ◽  
...  
Keyword(s):  
Solar Wind ◽  
Ion Composition ◽  
Wind Flows

Evidence of an ion composition boundary (protonopause) in bi-ion fluid simulations of solar wind mass loading

1994 ◽  
Vol 21 (20) ◽  
pp. 2255-2258 ◽  
Author(s):  
Konard Sauer ◽  
Alexander Bogdanov ◽  
Klaus Baumgärtel
Keyword(s):  
Solar Wind ◽  
Mass Loading ◽  
Ion Composition
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