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1.
Recent papers have suggested that the slow solar wind is a super-position of material which is released by reconnection from
large coronal loops. This reconnection process is driven by large-scale motions of solar magnetic flux driven by the non-radial
expansion of the solar wind from the differentially rotating photosphere into more rigidly rotating coronal holes.
The elemental composition of the slow solar wind material is observed to be fractionated and more variable than the fast solar
wind from coronal holes. Recently, it has also been reported that fractionation also occurs in 3He/4He. This may be interpreted
in the frame-work of an existing model for fractionation on large coronal loops in which wave-particle interactions preferentially
heat ions thereby modifying their scale-heights.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
2.
Steven R. Cranmer 《Space Science Reviews》2012,172(1-4):145-156
The origins of the hot solar corona and the supersonically expanding solar wind are still the subject of much debate. This paper summarizes some of the essential ingredients of realistic and self-consistent models of solar wind acceleration. It also outlines the major issues in the recent debate over what physical processes dominate the mass, momentum, and energy balance in the accelerating wind. A key obstacle in the way of producing realistic simulations of the Sun-heliosphere system is the lack of a physically motivated way of specifying the coronal heating rate. Recent models that assume the energy comes from Alfvén waves that are partially reflected, and then dissipated by magnetohydrodynamic turbulence, have been found to reproduce many of the observed features of the solar wind. This paper discusses results from these models, including detailed comparisons with measured plasma properties as a function of solar wind speed. Some suggestions are also given for future work that could answer the many remaining questions about coronal heating and solar wind acceleration. 相似文献
3.
Jean-Loup Bertaux Erkki Kyrölä Eric Quemerais Rosine Lallement Walter Schmidt Tuula Summanen Jorge Costa Teemu Mäkinen 《Space Science Reviews》1999,87(1-2):129-132
SWAN is the first space instrument dedicated to the monitoring of the latitude distribution of the solar wind by the Lyman
alpha method. The distribution of interstellar H atoms in the solar system is determined by their destruction during ionization
charge-exchange with solar wind protons. Maps of sky Ly-α emission have been recorded regularly since launch. The upwind maximum
emission region deviates strongly from the pattern that would be expected from a solar wind that is constant with latitude.
It is divided in two lobes by a depression aligned with the solar equatorial plane, called the Lyman-alpha groove, due to
enhanced ionization along the neutral sheet where the slow and dense solar wind is concentrated. The groove (or the anisotropy)
is more pronounced in 1997 than in 1996, but it then decreases between 1997 and 1998.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
4.
Christopher T. Russell 《Space Science Reviews》1975,17(2-4):435-447
The Third Solar Wind Conference was convened from March 25 to 29,1974 at the Asilomar Conference Grounds, Pacific Grove, California. The conference consisted of nine sessions dealing with solar abundances; the history and evolution of the solar wind; the structure and dynamics of the solar wind; the structure and dynamics of the solar corona; macroscopic and microscopic properties of the solar wind; cosmic rays as a probe of the solar wind; spatial gradients; stellar winds; and interactions with objects in the solar wind. This paper summarizes the invited and contributed talks presented at the conference.Institute of Geophysics and Planetary Physics Publication Number 1354-51. 相似文献
5.
Three ways of the energy transfer in the Earth's magnetosphere are studied. The solar wind MHD generator is an unique energy
source for all magnetospheric processes. Field-aligned currents directly transport the energy and momentum of the solar wind
plasma to the Earth's ionosphere. The magnetospheric lobe and plasma sheet convection generated by the solar wind is another
magnetospheric energy source. Plasma sheet particles and cold ionospheric polar wind ions are accelerated by convection electric
field. After energetic particle precipitation into the upper atmosphere the solar wind energy is transferred into the ionosphere
and atmosphere. This way of the energy transfer can include the tail lobe magnetic field energy storage connected with the
increase of the tail current during the southward IMF. After that the magnetospheric substorm occurs. The model calculations
of the magnetospheric energy give possibility to determine the ground state of the magnetosphere, and to calculate relative
contributions of the tail current, ring current and field-aligned currents to the magnetospheric energy. The magnetospheric
substorms and storms manifest that the permanent solar wind energy transfer ways are not enough for the covering of the solar
wind energy input into the magnetosphere. Nonlinear explosive processes are necessary for the energy transmission into the
ionosphere and atmosphere. For understanding a relation between substorm and storm it is necessary to take into account that
they are the concurrent energy transferring ways.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
6.
R. Wieler 《Space Science Reviews》1998,85(1-2):303-314
Lunar soil and certain meteorites contain noble gases trapped from the solar wind at various times in the past. The progress
in the last decade to decipher these precious archives of solar history is reviewed. The samples appear to contain two solar
noble gas components with different isotopic composition. The solar wind component resides very close to grain surfaces and
its isotopic composition is identical to that of present-day solar wind. Experimental evidence seems by now overwhelming that
somewhat deeper inside the grains there exists a second, isotopically heavier component. To explain the origin of this component
remains a challenge, because it is much too abundant to be readily reconciled with the known present day flux of solar particles
with energies above those of the solar wind. The isotopic composition of solar wind noble gases may have changed slightly
over the past few Ga, but such a change is not firmly established. The upper limit of ~5% per Ga for a secular increase of
the 3He/4He ratio sets stringent limits on the amount of He that may have been brought from the solar interior to the surface
(cf. Bochsler, 1992). Relative abundances of He, Ne, and Ar in present-day solar wind are the same as the long term average
recorded in metallic Fe grains in meteorites within error limits of some 15-20%. Xe, and to a lesser extent Kr, are enriched
in the solar wind similar to elements with a first ionisation potential < 10 eV, although Kr and Xe have higher FIPs. This
can be explained if the ionisation time governs the FIP effect (Geiss and Bochsler, 1986).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
7.
The consequences of the interaction between the solar wind and the local interstellar medium for the wind region enclosed by the heliospheric shock are reviewed. After identifying the principal mechanisms to influence the dynamics of the solar wind, an approach allowing the simultaneous incorporation of neutral atoms, pick-up ions, cosmic rays and energetic electrons into a multifluid model of the expanding wind plasma is outlined. The effects of these particle species are discussed in detail, with special emphasis on the electron component which behaves more like a quasi-static hot gas rather than an expanding fluid. This electron gas is effectively trapped within a three-dimensional trough of a circumsolar electric potential whose outer fringes are possibly determined by the density distribution of anomalous cosmic rays. The electrons are proven to be a globally structered component of great importance for the solar wind momentum flow contributing to a triggering of the solar wind dynamics by asymmetric interstellar boundary conditions. Finally, the consequences for the relative motion of the Sun and the local interstellar medium as well as for the solar system as a whole are described. 相似文献
8.
A. Balogh V. Bothmer N.U. Crooker R.J. Forsyth G. Gloeckler A. Hewish M. Hilchenbach R. Kallenbach B. Klecker J.A. Linker E. Lucek G. Mann E. Marsch A. Posner I.G. Richardson J.M. Schmidt M. Scholer Y.-M. Wang R.F. Wimmer-Schweingruber M.R. Aellig P. Bochsler S. Hefti Z. Mikić 《Space Science Reviews》1999,89(1-2):141-178
Corotating Interaction Regions (CIRs) form as a consequence of the compression of the solar wind at the interface between
fast speed streams and slow streams. Dynamic interaction of solar wind streams is a general feature of the heliospheric medium;
when the sources of the solar wind streams are relatively stable, the interaction regions form a pattern which corotates with
the Sun. The regions of origin of the high speed solar wind streams have been clearly identified as the coronal holes with
their open magnetic field structures. The origin of the slow speed solar wind is less clear; slow streams may well originate
from a range of coronal configurations adjacent to, or above magnetically closed structures. This article addresses the coronal
origin of the stable pattern of solar wind streams which leads to the formation of CIRs. In particular, coronal models based
on photospheric measurements are reviewed; we also examine the observations of kinematic and compositional solar wind features
at 1 AU, their appearance in the stream interfaces (SIs) of CIRs, and their relationship to the structure of the solar surface
and the inner corona; finally we summarise the Helios observations in the inner heliosphere of CIRs and their precursors to
give a link between the optical observations on their solar origin and the in-situ plasma observations at 1 AU after their
formation. The most important question that remains to be answered concerning the solar origin of CIRs is related to the origin
and morphology of the slow solar wind.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
9.
10.
Daniel B. Reisenfeld Roger C. Wiens Bruce L. Barraclough John T. Steinberg Marcia Neugebauer Jim Raines Thomas H. Zurbuchen 《Space Science Reviews》2013,175(1-4):125-164
We describe the Genesis mission solar-wind sample collection period and the solar wind conditions at the L1 point during this 2.3-year period. In order to relate the solar wind samples to solar composition, the conditions under which the samples were collected must be understood in the context of the long-term solar wind. We find that the state of the solar wind was typical of conditions over the past four solar cycles. However, Genesis spent a relatively large fraction of the time in coronal-hole flow as compared to what might have been expected for the declining phase of the solar cycle. Data from the Solar Wind Ion Composition Spectrometer (SWICS) on the Advanced Composition Explorer (ACE) are used to determine the effectiveness of the Genesis solar-wind regime selection algorithm. The data collected by SWICS confirm that the Genesis algorithm successfully separated and collected solar wind regimes having distinct solar origins, particularly in the case of the coronal hole sample. The SWICS data also demonstrate that the different regimes are elementally fractionated. When compared with Ulysses composition data from the previous solar cycle, we find a similar degree of fractionation between regimes as well as fractionation relative to the average photospheric composition. The Genesis solar wind samples are under long-term curation at NASA Johnson Space Center so that as sample analysis techniques evolve, pristine solar wind samples will be available to the scientific community in the decades to come. This article and a companion paper (Wiens et al. 2013, this issue) provide post-flight information necessary for the analysis of the Genesis array and foil solar wind samples and the Genesis solar wind ion concentrator samples, and thus serve to complement the Space Science Review volume, The Genesis Mission (v. 105, 2003). 相似文献
11.
Burnett D.S. Barraclough B.L. Bennett R. Neugebauer M. Oldham L.P. Sasaki C.N. Sevilla D. Smith N. Stansbery E. Sweetnam D. Wiens R.C. 《Space Science Reviews》2003,105(3-4):509-534
The Genesis Discovery mission will return samples of solar matter for analysis of isotopic and elemental compositions in terrestrial
laboratories. This is accomplished by exposing ultra-pure materials to the solar wind at the L1 Lagrangian point and returning
the materials to Earth. Solar wind collection will continue until April 2004 with Earth return in Sept. 2004. The general
science objectives of Genesis are to (1) to obtain solar isotopic abundances to the level of precision required for the interpretation
of planetary science data, (2) to significantly improve knowledge of solar elemental abundances, (3) to measure the composition
of the different solar wind regimes, and (4) to provide a reservoir of solar matter to serve the needs of planetary science
in the 21st century. The Genesis flight system is a sun-pointed spinner, consisting of a spacecraft deck and a sample return
capsule (SRC). The SRC houses a canister which contains the collector materials. The lid of the SRC and a cover to the canister
were opened to begin solar wind collection on November 30, 2001. To obtain samples of O and N ions of higher fluence relative
to background levels in the target materials, an electrostatic mirror (‘concentrator’) is used which focuses the incoming
ions over a diameter of about 20 cm onto a 6 cm diameter set of target materials. Solar wind electron and ion monitors (electrostatic
analyzers) determine the solar wind regime present at the spacecraft and control the deployment of separate arrays of collector
materials to provide the independent regime samples.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
12.
The goal of Working Group 1 was to discuss constraints on solar wind models. The topics for discussion, outlined by Eckart
Marsch in his introduction, were: (1) what heats the corona, (2) what is the role of waves, (3) what determines the solar
wind mass flux, (4) can stationary, multi-fluid models describe the fast and slow solar wind, or (5) do we need time dependent
fluid models, kinetic models, and/or MHD models to describe solar wind acceleration.
The discussion in the working group focused on observations of "temperatures" in the corona, mainly in coronal holes, and
whether the observations of line broadening should be interpreted as thermal broadening or wave broadening. Observations of
the coronal electron density and the flow speed in coronal holes were also discussed. There was only one contribution on observations
of the distant solar wind, but we can place firm constraints on the solar wind particle fluxes and asymptotic flow speeds
from observations with Ulysses and other spacecraft. Theoretical work on multi-fluid models, higher-order moment fluid models,
and MHD models of the solar wind were also presented.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
13.
On the Slow Solar Wind 总被引:1,自引:0,他引:1
A theory for the origin of the slow solar wind is described. Recent papers have demonstrated that magnetic flux moves across
coronal holes as a result of the interplay between the differential rotation of the photosphere and the non-radial expansion
of the solar wind in more rigidly rotating coronal holes. This flux will be deposited at low latitudes and should reconnect
with closed magnetic loops, thereby releasing material from the loops to form the slow solar wind. It is pointed out that
this mechanism provides a natural explanation for the charge states of elements observed in the slow solar wind, and for the
presence of the First-Ionization Potential, or FIP, effect in the slow wind and its absence in fast wind. Comments are also
provided on the role that the ACE mission should have in understanding the slow solar wind.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
14.
Coronal holes are the coolest and darkest regions of the upper solar atmosphere, as observed both on the solar disk and above the solar limb. Coronal holes are associated with rapidly expanding open magnetic fields and the acceleration of the high-speed solar wind. During the years of the solar minima, coronal holes are generally confined to the Sun??s polar regions, while at solar maxima they can also be found at lower latitudes. Waves, observed via remote sensing and detected in-situ in the wind streams, are most likely responsible for the wind and several theoretical models describe the role of MHD waves in the acceleration of the fast solar wind. This paper reviews the observational evidences of detection of propagating waves in these regions. The characteristics of the waves, like periodicities, amplitude, speed provide input parameters and also act as constraints on theoretical models of coronal heating and solar wind acceleration. 相似文献
15.
Alexeev Igor I. Belenkaya Elena S. Bobrovnikov Sergey Yu. Kalegaev Vladimir V. 《Space Science Reviews》2003,107(1-2):7-26
A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological
conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component
normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the
solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented.
In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition
of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of
the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and
the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the
magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe
the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux
structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the
observational data for September 24–26, 1998 magnetic storm (Dst
min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
16.
E. Marsch 《Space Science Reviews》1999,87(1-2):1-24
There are three major types of solar wind: The steady fast wind originating on open magnetic field lines in coronal holes,
the unsteady slow wind coming probably from the temporarily open streamer belt and the transient wind in the form of large
coronal mass ejections. The majority of the models is concerned with the fast wind, which is, at least during solar minimum,
the normal mode of the wind and most easily modeled by multi-fluid equations involving waves. The in-situ constraints imposed
on the models, mainly by the Helios (in ecliptic) and Ulysses (high-latitude) interplanetary measurements, are extensively
discussed with respect to fluid and kinetic properties of the wind. The recent SOHO observations have brought a wealth of
new information about the boundary conditions for the wind in the inner solar corona and about the plasma conditions prevailing
in the transition region and chromospheric sources of the wind plasma. These results are presented, and then some key questions
and scientific issues are identified.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
17.
The solar wind evolves as it moves outward due to interactions with both itself and with the circum-heliospheric interstellar medium. The speed is, on average, constant out to 30 AU, then starts a slow decrease due to the pickup of interstellar neutrals. These neutrals reduce the solar wind speed by about 20% before the termination shock (TS). The pickup ions heat the thermal plasma so that the solar wind temperature increases outside 20–30 AU. Solar cycle effects are important; the solar wind pressure changes by a factor of 2 over a solar cycle and the structure of the solar wind is modified by interplanetary coronal mass ejections (ICMEs) near solar maximum. The first direct evidences of the TS were the observations of streaming energetic particles by both Voyagers 1 and 2 beginning about 2 years before their respective TS crossings. The second evidence was a slowdown in solar wind speed commencing 80 days before Voyager 2 crossed the TS. The TS was a weak, quasi-perpendicular shock which transferred the solar wind flow energy mainly to the pickup ions. The heliosheath has large fluctuations in the plasma and magnetic field on time scales of minutes to days. 相似文献
18.
Gloeckler G. Cain J. Ipavich F.M. Tums E.O. Bedini P. Fisk L.A. Zurbuchen T.H. Bochsler P. Fischer J. Wimmer-Schweingruber R.F. Geiss J. Kallenbach R. 《Space Science Reviews》1998,86(1-4):497-539
The Solar Wind Ion Composition Spectrometer (SWICS) and the Solar Wind Ions Mass Spectrometer (SWIMS) on ACE are instruments
optimized for measurements of the chemical and isotopic composition of solar and interstellar matter. SWICS determines uniquely
the chemical and ionic-charge composition of the solar wind, the thermal and mean speeds of all major solar wind ions from
H through Fe at all solar wind speeds above 300 km s−1 (protons) and 170 km s−1 (Fe+16), and resolves H and He isotopes of
both solar and interstellar sources. SWICS will measure the distribution functions of both the interstellar cloud and dust
cloud pickup ions up to energies of 100 keV e−1. SWIMS will measure the chemical, isotopic and charge state composition of
the solar wind for every element between He and Ni. Each of the two instruments uses electrostatic analysis followed by a
time-of-flight and, as required, an energy measurement. The observations made with SWICS and SWIMS will make valuable contributions
to the ISTP objectives by providing information regarding the composition and energy distribution of matter entering the magnetosphere.
In addition, SWICS and SWIMS results will have an impact on many areas of solar and heliospheric physics, in particular providing
important and unique information on: (i) conditions and processes in the region of the corona where the solar wind is accelerated;
(ii) the location of the source regions of the solar wind in the corona; (iii) coronal heating processes; (iv) the extent
and causes of variations in the composition of the solar atmosphere; (v) plasma processes in the solar wind; (vi) the acceleration
of particles in the solar wind; (vii) the physics of the pickup process of interstellar He in the solar wind; and (viii) the
spatial distribution and characteristics of sources of neutral matter in the inner heliosphere.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
19.
A. Fedorov A. Opitz J.-A. Sauvaud J. G. Luhmann D. W. Curtis D. E. Larson 《Space Science Reviews》2011,161(1-4):49-62
The IMPACT SWEA instruments on board the twin STEREO spacecraft detect the solar wind electrons with energies between 1 and 2000 eV. The instruments provide 3-dimensional velocity distributions, pitch angle distributions and solar wind properties at two vantage points in the ecliptic at 1 AU. A few days after launch suppression of the low energy solar wind electrons was detected, which makes data analysis challenging and causes a significant loss of information below 50 eV. This paper describes the methods used to both understand the nature of the problem and to recover the most information about the low energy solar wind electrons from the measured datasets. These include numerical simulations, in-flight calibration results, and data reconstruction methods that allow the calculation of solar wind parameter proxies with minor limitations. 相似文献
20.
R. Kallenbach F.M. Ipavich H. Kucharek P. Bochsler A.B. Galvin J. Geiss F. Gliem G. Gloeckler H. Grünwaldt S. Hefti M. Hilchenbach D. Hovestadt 《Space Science Reviews》1998,85(1-2):357-370
Using the high-resolution mass spectrometer CELIAS/MTOF on board SOHO we have measured the solar wind isotope abundance ratios
of Si, Ne, and Mg and their variations in different solar wind regimes with bulk velocities ranging from 330 km/s to 650 km/s.
Data indicate a small systematic depletion of the heavier isotopes in the slow solar wind on the order of (1.4±1.3)% per amu
(2σ-error) compared to their abundances in the fast solar wind from coronal holes. These variations in the solar wind isotopic
composition represent a pure mass-dependent effect because the different isotopes of an element pass the inner corona with
the same charge state distribution. The influence of particle mass on the acceleration of minor solar wind ions is discussed
in the context of theoretical models and recent optical observations with other SOHO instruments.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献