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1.
Large-scale Coronal Heating, Clustering of Coronal Bright Points, and Concentration of Magnetic Flux
By combining quiet-region Fe XII coronal images from SOHO/EIT with magnetograms from NSO/Kitt Peak and from SOHO/MDI, we show that the population of network coronal bright points and the magnetic flux content of the network are both markedly greater under the bright half of the large-scale quiet corona than under the dim half. These results (1) support the view that the heating of the entire corona in quiet regions and coronal holes is driven by fine-scale magnetic activity (microflares, explosive events, spicules) seated low in the magnetic network, and (2) suggest that this large-scale modulation of the magnetic flux and coronal heating is a signature of giant convection cells. This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
2.
A. W. Hood 《Space Science Reviews》1999,87(1-2):79-92
Theories and observations of energy input, heating and acceleration mechanisms in the low corona were presented and discussed. The main topics of discussion were large-scale solar wind simulations, theoretical heating mechanisms, observational constraints, confronting theory with observations and observational issues. This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
3.
The heliospheric counterparts of coronal mass ejections (CMEs) at the Sun, interplanetary coronal mass ejections (ICMEs),
can be identified in situ based on a number of magnetic field, plasma, compositional and energetic particle signatures as
well as combinations thereof. We summarize these signatures and their implications for understanding the nature of these structures
and the physical properties of coronal mass ejections. We conclude that our understanding of ICMEs is far from complete and
formulate several challenges that, if addressed, would substantially improve our knowledge of the relationship between CMEs
at the Sun and in the heliosphere. 相似文献
4.
Leon Ofman 《Space Science Reviews》2005,120(1-2):67-94
Coronal holes have been identified as source regions of the fast solar wind, and MHD wave activity has been detected in coronal
holes by remote sensing, and in situ in fast solar wind streams. I review some of the most suggestive wave observations, and
discuss the theoretical aspects of MHD wave heating and solar wind acceleration in coronal holes. I review the results of
single fluid 2.5D MHD, as well as multi-fluid 2.5D MHD models of waves in coronal holes, the heating, and the acceleration
of the solar wind be these waves. 相似文献
5.
A two dimensional model of the transition region and the lower corona, based on the idea that the magnetic flux is strongly
concentrated at the boundaries of the supergranular convection cells, has been proposed by Gabriel in 1976. The plasma moves
along the open magnetic field lines, which define the the so-called "funnel," and eventually builds up the solar wind.
Based on a two dimensional funnel model we investigate the stationary plasma flow at its central line, taking heat conduction,
radiative losses, and a heating function into account. The derived height profiles of the plasma properties within the funnel
are presented.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
6.
Steven R. Spangler 《Space Science Reviews》2005,121(1-4):189-200
I discuss a method for determining the strength and spatial structure of the coronal magnetic field by observations of the
Faraday rotation of a radio galaxy which is in conjunction with the Sun. Given a knowledge of the plasma density in the outer
corona, and the magnetic field sector structure (both independently available), the strength of the coronal field can be determined,
as well as the magnitude of spatial variations on scales of 1000 km to several solar radii. Such knowledge is crucial for
testing computational models of the solar corona, which are prominently featured in this meeting. Results are presented from
observations with the Very Large Array radio telescope of the radio galaxy 3C228 on August 16, 2003, when the line of sight
to the source was at heliocentic distances of 7.1−6.2R
⊙. The observations are consistent with a coronal magnetic field which is proportional to the inverse square of the distance
in the range 6 ≤ r ≤ 10R
⊙, and has a value of 39 mG at 6.2R
⊙. The Faraday rotation is uniform across the source, indicating an absence of strong plasma inhomogeneity on spatial scales
up to 35,000 km. 相似文献
7.
Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity,
magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs
as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their
emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article
we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing
observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the
inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour
high-latitude activity. 相似文献
8.
The possibility of remote diagnostics of coronal structures with impulsively-generated short-period fast magnetoacoustic wave
trains is demonstrated. An initially broad-band, aperiodic fast magnetoacoustic perturbation guided by a 1D plasma inhomogeneity
develops into a quasi-periodic wave train with a well-pronounced frequency and amplitude modulation. The quasi-periodicity
results from the geometrical dispersion of the modes, determined by the transverse profile of the loop, and hence contains
information about the profile. Wavelet images of the wave train demonstrate that their typical spectral signature is of a
“crazy tadpole’’ shape: a narrow spectrum tail precedes a broad-band head. The instantaneous period of the oscillations in
the wave train decreases gradually with time, with a mean value of several seconds for typical coronal values. The period
and the spectral amplitude evolution are determined by the steepness of the transverse density profile and the density contrast
ratio in the loop, which offers a tool for estimation of the sub-resolution structuring of the corona. 相似文献
9.
Nat Gopalswamy 《Space Science Reviews》2006,124(1-4):145-168
Interplanetary coronal mass ejections (ICMEs) originating from closed field regions on the Sun are the most energetic phenomenon
in the heliosphere. They cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles. ICMEs
are the interplanetary manifestations of CMEs typically remote-sensed by coronagraphs. This paper summarizes the observational
properties of ICMEs with reference to the ordinary solar wind and the progenitor CMEs. 相似文献
10.
R. F. Wimmer-Schweingruber N. U. Crooker A. Balogh V. Bothmer R. J. Forsyth P. Gazis J. T. Gosling T. Horbury A. Kilchenmann I. G. Richardson J. D. Richardson P. Riley L. Rodriguez R. von Steiger P. Wurz T. H. Zurbuchen 《Space Science Reviews》2006,123(1-3):177-216
While interplanetary coronal mass ejections (ICMEs) are understood to be the heliospheric counterparts of CMEs, with signatures
undeniably linked to the CME process, the variability of these signatures and questions about mapping to observed CME features
raise issues that remain on the cutting edge of ICME research. These issues are discussed in the context of traditional understanding,
and recent results using innovative analysis techniques are reviewed. 相似文献
11.
Coronal hole boundaries are the interfaces between regions where the coronal magnetic field contains a significant component
which is open into the heliosphere and regions where the field is primarily closed. It is pointed out that there are constraints
on the magnetic field which opens into the heliosphere that must be satisfied in the corona: it must come into pressure equilibrium
in the high corona, and the component of the field which connects to the polar regions of the Sun must differentially rotate.
A model is presented in which satisfying these constraints determines which field lines are open and which are closed, and
thus where the polar coronal hole boundaries occur. Some of the consequences of this model are discussed.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
12.
D. Dobrzycka L. Strachan M. P. Miralles J. L. Kohl L. D. Gardner P. Smith M. Guhathakurta R. Fisher 《Space Science Reviews》1999,87(1-2):177-180
We compared the H I Lyα polar coronal hole profiles obtained during the three Spartan 201 flights (in 1993, 1994, and 1995)
and during the more recent UVCS/SOHO mission. We found that at 2.1 R⊙ there are no significant variations of the line shape over the several years of the descending phase of the solar cycle.
However, there may be some evidence for the 1.8 R⊙ profiles being broader towards solar minimum. The profiles at 2.1 R⊙ are different from profiles obtained at 1.8 R⊙; they have clearly narrower cores and wide wings. We fitted the profiles with single and/or multiple Gaussian functions and
calculated their typical 1/e half widths.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
13.
We derive electron temperature and density as a function of height up to 0.2 R⊙ above the limb in polar coronal holes, using five EUV data sets recorded by the SOHO Coronal Diagnostic Spectrometer between July 1997 and February 1998. Radial T and N distributions, averaged in a 2° to 10° range of position angles, are the same above the North and South coronal holes. They do not show any time variability over a period of seven months. Polar plumes are found to have lower electron temperature and higher density than the interplume lanes. The electron density slope suggests that the proton temperatures are twice as high as the electron temperatures. This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
14.
L. Golub 《Space Science Reviews》2006,124(1-4):23-33
We provide a brief overview of present-day studies of inner corona dynamics, with examples of mass ejections (CME), flares
and active region dynamics. While the names of the topics have not changed in several decades, the internal details and the
language used to express the nature of the problem have changed considerably. We conclude with a short discussion of the contribution
to studies of coronal dynamics to be expected from the Atmospheric Imager Assembly (AIA) on the Solar Dynamics Observatory. 相似文献
15.
Yihua Yan 《Space Science Reviews》2005,121(1-4):213-221
The coronal magnetic field configuration is important for understanding the energy storage and release processes that account
for flares and/or CMEs. Here we present a model which is based on the work for potential magnetic field problems that only
applies the condition at infinity with the boundary condition on the solar surface specified. We also discuss some recent
progress on general force-free field models. For some event analyses, we have employed MDI/SOHO longitudinal magnetogram insected
into the synoptic magnetogram to obtain whole boundary condition over the solar surface. Globally, the extrapolated global
magnetic field structures effectively demonstrate the case for the disk signature of the radio CMEs and the evolution of the
radio sources during the CME/flare processes. 相似文献
16.
An equatorial coronal hole has been observed on 18 and 19 October 1996 with SOHO-CDS and with the Nancąy Radioheliograph (RH).
The CDS EUV line intensities are used to determine the coronal hole Differential Emission Measure (DEM); in turn this is used
to compute the radio brightness temperature Tb at the observed frequencies, leaving the coronal electron temperature and density as free parameters. EUV line intensities,
calculated from the derived models, show a good agreement with EUV observations.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
17.
An analytical solution is presented for linear force fields within a spherical shell, representing the solar corona. Allowing for a global magnetic helicity, we find magnetic fields over the entire corona with realistic inner boundary conditions obtained from transformation and extrapolation of photospheric magnetograms and considering alternative outer boundary conditions. Such fields are found for the well known coronal hole extension event of August 1996. This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
18.
R. Esser 《Space Science Reviews》1999,87(1-2):93-104
Summarized below are the discussions of working group 3 on "Coronal hole boundaries and interactions with adjacent regions"
which took place at the 7th SOHO workshop in Northeast Harbor, Maine, USA, 28 September to 1 October 1998. A number of recent
observational and theoretical results were presented during the discussions to shed light on different aspects of coronal
hole boundaries. The working group also included presentations on streamers and coronal holes to emphasis the difference between
the plasma properties in these regions, and to serve as guidelines for the definition of the boundaries. Observations, particularly
white light observations, show that multiple streamers are present close to the solar limb at all times. At some distance
from the sun, typically below 2 R, these streamers merge into a relatively narrow sheet as seen, for example, in LASCO and
UVCS images. The presence of multiple current sheets in interplanetary space was also briefly addressed. Coronal hole boundaries
were defined as the abrupt transition from the bright appearing plasma sheet to the dark coronal hole regions. Observations
in the inner corona seem to indicate a transition of typically 10 to 20 degrees, whereas observations in interplanetary space,
carried out from Ulysses, show on one hand an even faster transition of less than 2 degrees which is in agreement with earlier
Helios results. On the other hand, these observations also show that the transition happens on different scales, some of which
are significantly larger.
The slow solar wind is connected to the streamer belt/plasma sheet, even though the discussions were still not conclusive
on the point where exactly the slow solar wind originates. Considered the high variability of plasma characteristics in slow
wind streams, it seems most likely that several types of coronal regions produce slow solar wind, such as streamer stalks,
streamer legs and open field regions between active regions, and maybe even regions just inside of the coronal holes. Observational
and theoretical studies presented during the discussions show evidence that each of these regions may indeed contribute to
the solar slow wind.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
19.
Spectra from the Coronal Diagnostic Spectrometer on board SOHO are used to compare density and temperature in coronal hole
and quiet Sun regions.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
20.
P. Lemaire K. Bocchialini V. Aletti D. Hassler K. Wilhelm 《Space Science Reviews》1999,87(1-2):249-252
The analysis of data taken by SUMER near disk center, where a small coronal hole is observed in EIT images, is performed.
From the measurements of Doppler non-thermal velocities and intensities, we search for the diagnostics and the signature of
small scale structures in the coronal hole using transition region lines. Transition region lines in the range of 7 × 104 K to 2.5 × 105 K have a non-thermal velocity excess of 4.0 to 5.5 km s-1 relative to the contiguous quiet Sun. While the average intensity is lower in the coronal hole than in the quiet area, this
result shows an increase of turbulence at the base of the high speed solar wind.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献