Solar Parameters for Modeling the Interplanetary Background

Bzowski, M.; Sokół, J. M.; Tokumaru, M.; Fujiki, K.; Quémerais, Éric; Lallement, R.; Ferron, S.; Bochsler, P.; McComas, D. J.

doi:10.1007/978-1-4614-6384-9_3

Cited by 71 publications

(47 citation statements)

References 197 publications

(222 reference statements)

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“…In this respect, the total SW flux exactly follows the 1/r 2 scaling due to the continuity conditions, as discussed by Bzowski et al (2012). This happens because most of the PUIs are created due to charge-exchange and thus are not new members of the SW population.…”

Section: Discussionmentioning

confidence: 69%

“…With this information, one might be able to follow the idea presented by Bzowski et al (2012) and independently calculate the profiles of SW density.…”

Section: Discussionmentioning

confidence: 99%

“…The data from the epoch before IMP-8 are from various experiments and could not be reliably brought to a common calibration with the IMP-8/Wind system because of the lack of overlap between the measurement time intervals. Our analysis starts in 1985, when IMP-8 was already in operation (see also the review by Bzowski et al, 2012).…”

Section: In Situ In-ecliptic Measurements Collected From Various Spacmentioning

confidence: 99%

“…Our procedure takes as a baseline absolute calibration of the OMNI 2 data set both in speed and density in the ecliptic plane and the absolute calibration of Ulysses measurements for density and speed out-of-ecliptic and interplanetary scintillation observations, interpreted by the tomography modeling for speed out-of-ecliptic. Up to now, no global, continuous measurements of SW density as a function of heliographic latitude have been available and this quantity has to be obtained using indirect methods (see Bzowski et al, 2012).…”

Section: Data Processing and Model Descriptionmentioning

confidence: 99%

“…Regular measurements of its parameters began in the early 1960s, and data from many spacecraft are now available, obtained using various observation and data processing techniques (see for review Bzowski et al, 2012). Shortly after the discovery of the solar wind (SW hereafter), the question of whether or not it is spherically symmetric was put forward.…”

Section: Introductionmentioning

confidence: 99%

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Heliolatitude and Time Variations of Solar Wind Structure from in situ Measurements and Interplanetary Scintillation Observations

et al. 2012

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The 3D structure of the solar wind and its evolution in time are needed for heliospheric modeling and interpretation of energetic neutral atoms observations. We present a model to retrieve the solar wind structure in heliolatitude and time using all available and complementary data sources. We determine the heliolatitude structure of solar wind speed on a yearly time grid over the past 1.5 solar cycles based on remote-sensing observations of interplanetary scintillations, in situ out-of-ecliptic measurements from Ulysses, and in situ in-ecliptic measurements from the OMNI 2 database. Since in situ out-of-ecliptic information on the solar wind density structure is not available apart from the Ulysses data, we derive correlation formulae between the solar wind speed and density and use the information on the solar wind speed from interplanetary scintillation observations to retrieve the 3D structure of the solar wind density. With the variations of solar wind density and speed in time and heliolatitude available, we calculate variations in solar wind flux, dynamic pressure, and charge-exchange rate in the approximation of stationary H atoms.

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Section: Discussionmentioning

confidence: 69%

“…With this information, one might be able to follow the idea presented by Bzowski et al (2012) and independently calculate the profiles of SW density.…”

Section: Discussionmentioning

confidence: 99%

Section: In Situ In-ecliptic Measurements Collected From Various Spacmentioning

confidence: 99%

Section: Data Processing and Model Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Heliolatitude and Time Variations of Solar Wind Structure from in situ Measurements and Interplanetary Scintillation Observations

et al. 2012

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Possible modification of the cooling index of interstellar helium pickup ions by electron impact ionization in the inner heliosphere

et al. 2014

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Interstellar neutrals penetrating into the inner heliosphere are ionized by photoionization, charge exchange with solar wind ions, and electron impact ionization. These processes comprise the first step in the evolution of interstellar pickup ion (PUI) distributions. Typically, PUI distributions have been described in terms of velocity distribution functions that cool adiabatically under solar wind expansion, with a cooling index of 3/2. Recently, the cooling index has been determined experimentally in observations of He PUI distributions with Advanced Composition Explorer (ACE)/Solar Wind Ion Composition Spectrometer and found to vary substantially over the solar cycle. The experimental determination of the cooling index depends on the knowledge of the ionization rates and their spatial variation. Usually, ionization rates increase with 1/r 2 as neutral particles approach the Sun, which is not exactly true for electron impact ionization, because the electron temperature increases with decreasing distance from the Sun due to the complexity of its distributions and different radial gradients in temperature. This different dependence on distance may become important in the study of the evolution of PUI distributions and is suspected as one of the potential reasons for the observed variation of the cooling index. Therefore, we investigate in this paper the impact of electron ionization on the variability of the cooling index. We find that the deviation of the electron ionization rate from the canonical 1/r 2 behavior of other ionization processes plays only a minor role.

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Time‐of‐flight mass spectrographs—From ions to neutral atoms

et al. 2016

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After their introduction to space physics in the mid 1980s time‐of‐flight (TOF) spectrographs have become a main staple in spaceborne mass spectrometry. They have largely replaced magnetic spectrometers, except when extremely high mass resolution is required to identify complex molecules, for example, in the vicinity of comets or in planetary atmospheres. In combination with electrostatic analyzers and often solid state detectors, TOF spectrographs have become key instruments to diagnose space plasma velocity distributions, mass, and ionic charge composition. With a variety of implementation schemes that also include isochronous electric field configurations, TOF spectrographs can respond to diverse science requirements. This includes a wide range in mass resolution to allow the separation of medium heavy isotopes or to simply provide distributions of the major species, such as H, He, and O, to obtain information on source tracers or mass fluxes. With a top‐hat analyzer at the front end, or in combination with deflectors for three‐axis stabilized spacecraft, the distribution function of ions can be obtained with good time resolution. Most recently, the reach of TOF ion mass spectrographs has been extended to include energetic neutral atoms. After selecting the arrival direction with mechanical collimation, followed by conversion to ions, adapted TOF sensors form a new branch of the spectrograph family tree. We review the requirements, challenges, and implementation schemes for ion and neutral atom spectrographs, including potential directions for the future, while largely avoiding overlap with complementary contributions in this special issue.

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Solar Parameters for Modeling the Interplanetary Background

Cited by 71 publications

References 197 publications

Heliolatitude and Time Variations of Solar Wind Structure from in situ Measurements and Interplanetary Scintillation Observations

Heliolatitude and Time Variations of Solar Wind Structure from in situ Measurements and Interplanetary Scintillation Observations

Possible modification of the cooling index of interstellar helium pickup ions by electron impact ionization in the inner heliosphere

Time‐of‐flight mass spectrographs—From ions to neutral atoms

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