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1.
We present results derived from the analysis of an equatorial streamer structure as observed by the UVCS instrument aboard
SOHO. From observations of the H I Lyα and Lyβ lines we infer the density and temperature of the plasma. We develop a preliminary
axisymmetric, magnetostatic model of the corona which includes the effects of gas pressure gradients on the magnetic structure.
We infer a coronal plasma β > 1 in the closed field regions and near the cusp of the streamer. We add to the model a parallel
velocity field assuming mass flux conservation along magnetic flux tubes. We then compute the Lyα emissivity and the line-of-sight
integrals to obtain images of Lyα intensity, taking into account projection effects and Doppler dimming. The images we obtain
from this preliminary model are in good general agreement with the UVCS observations, both qualitatively and quantitatively.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
2.
J. L. Kohl L. D. Gardner L. Strachan R. Fisher M. Guhathakurta 《Space Science Reviews》1995,72(1-2):29-38
Spartan 201 is a shuttle deployed spacecraft that is scheduled to perform ultraviolet spectroscopy and white light polarimetry of the extended solar corona during two 40 hour missions to occur in September 1994 and August 1995. The spectroscopy is done with an ultraviolet coronal spectrometer which measures the intensity and spectral line profile of HI Ly up to heliocentric heights of 3.5 solar radii. It also measures the intensities of the OVI doublet at 1032 and 1037 Å and of Fe XII at 1242 Å. The HI Ly line profile measurements are used to determine the random velocity distribution of coronal protons along the line-of-sight. The absolute HI Ly intensities can be used together with electron densities from the white light coronagraph to estimate electron temperatures from hydrogen ionization balance calculations, and bulk outflow velocities from models of Doppler dimmed resonant scattering. Intensities of minor ion lines are used to determine coronal abundances and outflow velocities of O5+. Ultraviolet spectroscopy of extended coronal regions from the 11 April 1993 mission of Spartan 201 are discussed. 相似文献
3.
Recent SOHO/UVCS observations indicate that the perpendicular proton and ion temperatures are much larger than electron temperatures.
In the present study we simulate numerically the solar wind flow in a coronal hole with the two-fluid approach. We investigate
the effects of electron and proton temperatures on the solar wind acceleration by nonlinear waves. In the model the nonlinear
waves are generated by Alfvén waves with frequencies in the 10-3 Hz range, driven at the base of the coronal hole. The resulting electron and proton flow profile exhibits density and velocity
fluctuations. The fluctuations may steepen into shocks as they propagate away from the sun. We calculate the effective proton
temperature by combining the thermal and wave velocity of the protons, and find qualitative agreement with the proton kinetic
temperature increase with height deduced from the UVCS Ly-α observations by Kohl et al. (1998).
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
4.
We analyzed UVCS/SOHO data and compared the H I Lyα (121.6 nm) and O VI (103.2 nm, 103.7 nm) emission in the polar and equatorial
coronal holes. We found that the emission lines have similar characteristics in these two types of coronal holes. Both types
show evidence for superradially diverging boundaries. The latitudinal distribution of the O VI line ratio may indicate that
the equatorial coronal hole has O+5 outflow velocities lower than in the polar coronal holes.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
5.
R. M. Suleiman J.L. Kohl A. V. Panasyuk A. Ciaravella S.R. Cranmer L.D. Gardner R. Frazin R. Hauck P.L. Smith G. Noci 《Space Science Reviews》1999,87(1-2):327-330
The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) has been used to measure
spectral line profiles for H I Lyα in the south polar coronal hole at projected heliocentric heights from 3.5 to 6.0 R⊙ during 1998 January 5–11. Observations from 1.5 to 2.5 R⊙ were made for comparison. The H I Lyα profile is the only one observable with UVCS above 3.5 R⊙ in coronal holes. Within this region the outflowing coronal plasma becomes nearly collisionless and the ionization balance
is believed to become frozen.
In this paper, the 1/e half widths of the coronal velocity distributions are provided for the observed heights. The velocity
distributions include all motions contributing to the velocities along the line of sight (LOS). The observations have been
corrected for instrumental effects and interplanetary H I Lyα. The half widths were found to increase with projected heliographic
height from 1.5 to 2.5 R⊙ and decrease with height from 3.5 to 5 R⊙.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
6.
Steven R. Cranmer 《Space Science Reviews》2002,101(3-4):229-294
Coronal holes are the lowest density plasma components of the Sun's outer atmosphere, and are associated with rapidly expanding magnetic fields and the acceleration of the high-speed solar wind. Spectroscopic and polarimetric observations of the extended corona, coupled with interplanetary particle and radio sounding measurements going back several decades, have put strong constraints on possible explanations for how the plasma in coronal holes receives its extreme kinetic properties. The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) spacecraft has revealed surprisingly large temperatures, outflow speeds, and velocity distribution anisotropies for positive ions in coronal holes. We review recent observations, modeling techniques, and proposed heating and acceleration processes for protons, electrons, and heavy ions. We emphasize that an understanding of the acceleration region of the wind (in the nearly collisionless extended corona) is indispensable for building a complete picture of the physics of coronal holes. 相似文献
7.
M. P. Miralles L. Strachan L. D. Gardner P. L. Smith J. L. Kohl M. Guhathakurta R. R. Fisher 《Space Science Reviews》1999,87(1-2):277-281
The Spartan 201 flights from 1993 to 1995 provided us with observations in H I Lyman-α of several coronal hole/streamer boundaries
and adjacent streamers during the declining phase of the current solar cycle: Analysis of the latitudinal dependence of the
line intensities clearly shows that there is a boundary region at the coronal hole/streamer interface where the H I Lyman-α
intensity reaches a minimum value. Similar results are also found in UVCS/SOHO observations. We also discuss differences in
the coronal hole/streamer boundaries for different types of streamers and their changes over the three year period of Spartan
201 observations.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
8.
A technique to derive the coronal density irregularity factor
, wheren is the electron density, has been proposed by Fineschi and Romoli (1993). This technique will exploit the unique UVCS capability of cotemporal and cospatial measurements of both UV line radiation and K-coronal polarized brightness,pB.The ratio of the measured H I Lyman (Ly-) line intensity to the resonant-scattering dominated H I Lyman (Ly-) intensity can be used to extract the collisional component of the Ly-. This component yields an estimate of
. The quantity
is then obtained from the UVCS white-light K-coronal measurements.We present simulated observations of the UVCS for coronal atmosphere models with different filling factors and electron density profiles, and for different coronal structures (e.g., coronal holes, streamers). These simulations will show how the proposed technique may be used to probe inhomogeneities of the solar corona. 相似文献
9.
Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models
of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation
of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending
on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies
with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum
between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is
rapid, even for minor ions like O5+, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This
indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
10.
Robert F. Wimmer-Schweingruber Rudolf Von Steiger Johannes Geiss George Gloeckler Fred M. Ipavich Berend Wilken 《Space Science Reviews》1998,85(1-2):387-396
Recent observations with UVCS on SOHO of high outflow velocities of O5+ at low coronal heights have spurred much discussion about the dynamics of solar wind acceleration. On the other hand, O6+ is the most abundant oxygen charge state in the solar wind, but is not observed by UVCS or by SUMER because this helium-like
ion has no emission lines falling in the wave lengths observable by these instruments. Therefore, there is considerable interest
in observing O5+ in situ in order to understand the relative importance of O5+ with respect to the much more abundant O6+. High speed streams are the prime candidates for the search for O5+ because all elements exhibit lower freezing-in temperatures in high speed streams than in the slow solar wind. The Ulysses
spacecraft was exposed to long time periods of high speed streams during its passage over the polar regions of the Sun. The
Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is capable of resolving this rare oxygen charge state. We present
the first measurement of O5+ in the solar wind and compare these data with those of the more abundant oxygen species O6+ and O7+. We find that our observations of the oxygen charge states can be fitted with a single coronal electron temperature in the
range of 1.0 to 1.2 MK assuming collisional ionization/recombination equilibrium with an ambient Maxwellian electron gas.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
11.
We investigated the UV emission expected from solar coronal transients, selecting some spectral lines which will be observed with the UVCS spectrocoronagraph onboard the SOHO spacecraft. The line intensities were calculated starting from a representative, simplified model of coronal transient. We discuss how the considered intensities depend on the physical parameters of the examined structures. This work is aimed to give a contribution in defining and preparing the future observations of coronal transients and coronal mass ejections by the UVCS/SOHO. 相似文献
12.
L. Ofman M. Romoli G. Noci G. Poletto J. L. Kohl R. A. Howard C. St. Cyr C. E. Deforest 《Space Science Reviews》1999,87(1-2):287-290
In recent UVCS/SOHO White Light Channel (WLC) observations we found quasi-periodic variations in the polarized brightness
(pB) in the polar coronal holes at heliocentric distances of 1.9 to 2.45 solar radii. The motivation for the observation is
the 2.5D MHD model of solar wind acceleration by nonlinear waves, that predicts compressive fluctuations in coronal holes.
In February 1998 we performed new observations using the UVCS/WLC in the coronal hole and obtained additional data. The new
data corroborate our earlier findings with higher statistical significance. The new longer observations show that the power
spectrum peaks in the 10–12 minute range. These timescales agree with EIT observations of brightness fluctuations in polar
plumes. We performed preliminary LASCO/C2 observations in an effort to further establish the coronal origin of the fluctuations.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
13.
S. Patsourakos J.-C. Vial J.-R. Gabryl S. Koutchmy U. Schühle 《Space Science Reviews》1999,87(1-2):291-294
Polar coronal holes represent the most convincing site from which the high-speed solar wind originates. Here we report high-accuracy Doppler shifts measured in the O VI (1037.6 Å) line obtained by SUMER on SOHO inside an interplume region within the south polar coronal hole. We infer limits on the outflow velocity and draw hints about the flow geometry. 相似文献
14.
The profiles of the Lyα line at 1215.6 Å and of the O VI doublet at 1031.9 Å and 1037.6 Å in the extended solar corona have been analyzed vs. latitude and radial direction, performing observations with the Ultraviolet Coronagraph Spectrometer (UVCS) on board the ESA-NASA solar satellite SOHO (Solar and Heliospheric Observatory). The results show that these lines behave differently with latitude: the H I Ly α line has larger full width at half maximum (FWHM) values in the streamer region and narrower values towards the pole, while the FWHM of O VI lines has a minimum at the center of the streamer and slightly increases towards the polar regions. We briefly discuss the impact of the results on coronal heating theories. 相似文献
15.
SOHO/UVCS data indicate that minor ions in the corona are heated more than hydrogen, and that coronal heating results in T⊥ larger than T‖. Analogous behavior has been known from in situ measurements in solar wind for many years. Here we compare and contrast two
mechanisms which have been proposed to account for the above behavior: ion-cyclotron resonance and gravity damping.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
16.
This paper contains a summary of the topics treated in the working group on abundance variations in the solar atmosphere and
in the solar wind. The FIP bias (overabundance of particles with low First Ionization Potentials over photospheric abundances)
in coronal holes and coronal hole associated solar wind amounts to values between 1 and 2. The FIP bias in the slow solar
wind is typically a factor 4, consistent with optical observations in streamers. In order to distinguish between different
theoretical models which make an attempt to explain the FIP bias, some observable parameters must be provided. Unfortunately,
many models are deficient in this respect. In addition to FIP fractionation, gravitational settling of heavy elements has
been found in the core of long lived streamers. The so-called electron 'freeze in' temperatures derived from in situ observed
ionization states of minor ions in the fast wind are significantly higher than the electron temperatures derived from diagnostic
line ratios observed in polar coronal holes. The distinction between conditions in plumes and interplume lanes needs to be
further investigated. The 'freeze in' temperatures for the slow solar wind are consistent with the electron temperatures derived
for streamers.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
17.
18.
The spectroscopic observations of the Ultraviolet Coronagraph Spectrometer (UVCS), on board the SOHO observatory, allow the study and the full characterization of the expansion of the solar atmosphere by means of measurements of the outflow speeds and the physical properties of the wind, directly in the region where the solar plasma is heated and accelerated: the extended corona. During solar minimum, when the magnetic configuration of the corona is rather simple, the open magnetic fields emerging from the wide polar coronal holes channel toward the heliosphere both the fast and the slow wind. The fast wind flows along flux tubes with lower areal divergence than the slow wind which is guided by flux tubes characterized by non-monotonic areal expansion functions. Differences in the physical properties, such as kinetic temperature, electron density, composition and density fluctuations, of the fast and slow wind in the corona are discussed. 相似文献
19.
The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) has observed the extended solar corona between 1 and 10 R· for more
than two years. We review spectroscopic and polarimetric measurements made in coronal holes, equatorial streamers, and coronal
mass ejections, as well as selected non-solar targets. UVCS/SOHO has provided a great amount of empirical information about
the physical processes that heat and accelerate the solar wind, and about detailed coronal structure and evolution.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
20.
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