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1.
The bootstrap method is used to determine errors of basic attributes of coronal mass ejections (CMEs) visually identified in images obtained by the Solar and Heliospheric Observatory (SOHO) mission’s Large Angle and Spectrometric Coronagraph (LASCO) instruments. The basic parameters of CMEs are stored, among others, in a database known as the SOHO/LASCO CME catalog and are widely employed for many research studies. The basic attributes of CMEs (e.g. velocity and acceleration) are obtained from manually generated height-time plots. The subjective nature of manual measurements introduces random errors that are difficult to quantify. In many studies the impact of such measurement errors is overlooked. In this study we present a new possibility to estimate measurements errors in the basic attributes of CMEs. This approach is a computer-intensive method because it requires repeating the original data analysis procedure several times using replicate datasets. This is also commonly called the bootstrap method in the literature. We show that the bootstrap approach can be used to estimate the errors of the basic attributes of CMEs having moderately large numbers of height-time measurements. The velocity errors are in the vast majority small and depend mostly on the number of height-time points measured for a particular event. In the case of acceleration, the errors are significant, and for more than half of all CMEs, they are larger than the acceleration itself. 相似文献
2.
Halo coronal mass ejections (HCMEs) are responsible of the most severe geomagnetic storms. A prediction of their geoeffectiveness
and travel time to Earth’s vicinity is crucial to forecast space weather. Unfortunately, coronagraphic observations are subjected
to projection effects and do not provide true characteristics of CMEs. Recently, Michalek (Solar Phys.
237, 101, 2006) developed an asymmetric cone model to obtain the space speed, width, and source location of HCMEs. We applied this technique
to obtain the parameters of all front-sided HCMEs observed by the SOHO/LASCO experiment during a period from the beginning
of 2001 until the end of 2002 (solar cycle 23). These parameters were applied for space weather forecasting. Our study finds
that the space speeds are strongly correlated with the travel times of HCMEs to Earth’s vicinity and with the magnitudes related
to geomagnetic disturbances. 相似文献
3.
We report on the coronal hole (CH) influence on the 54 magnetic cloud (MC) and non-MC associated coronal mass ejections (CMEs) selected for studies during the Coordinated Data Analysis Workshops (CDAWs) focusing on the question if all CMEs are flux ropes. All selected CMEs originated from source regions located between longitudes 15E?–?15W. Xie, Gopalswamy, and St. Cyr (2013, Solar Phys., doi: 10.1007/s11207-012-0209-0 ) found that these MC and non-MC associated CMEs are on average deflected towards and away from the Sun–Earth line, respectively. We used a CH influence parameter (CHIP) that depends on the CH area, average magnetic field strength, and distance from the CME source region to describe the influence of all on-disk CHs on the erupting CME. We found that for CHIP values larger than 2.6 G the MC and non-MC events separate into two distinct groups where MCs (non-MCs) are deflected towards (away) from the disk center. Division into two groups was also observed when the distance to the nearest CH was less than 3.2×105 km. At CHIP values less than 2.6 G or at distances of the nearest CH larger than 3.2×105 km the deflection distributions of the MC and non-MCs started to overlap, indicating diminishing CH influence. These results give support to the idea that all CMEs are flux ropes, but those observed to be non-MCs at 1 AU could be deflected away from the Sun–Earth line by nearby CHs, making their flux rope structure unobservable at 1 AU. 相似文献
4.
We investigated a set of 54 interplanetary coronal mass ejection (ICME) events whose solar sources are very close to the disk center (within ±?15° from the central meridian). The ICMEs consisted of 23 magnetic-cloud (MC) events and 31 non-MC events. Our analyses suggest that the MC and non-MC ICMEs have more or less the same eruption characteristics at the Sun in terms of soft X-ray flares and CMEs. Both types have significant enhancements in ion charge states, although the non-MC structures have slightly lower levels of enhancement. The overall duration of charge-state enhancement is also considerably smaller than that in MCs as derived from solar wind plasma and magnetic signatures. We find very good correlation between the Fe and O charge-state measurements and the flare properties such as soft X-ray flare intensity and flare temperature for both MCs and non-MCs. These observations suggest that both MC and non-MC ICMEs are likely to have a flux-rope structure and the unfavorable observational geometry may be responsible for the appearance of non-MC structures at 1 AU. We do not find any evidence for an active region expansion resulting in ICMEs lacking a flux-rope structure because the mechanism of producing high charge states and the flux-rope structure at the Sun is the same for MC and non-MC events. 相似文献
5.
A total of 293 measurements of respiration rate were made on planktonic crustaceans collected in different seasons from the
Inland Sea of Japan. The relationship between the rate of oxygen consumption (R,μl O2 indiv.−1 hr−1) and body dry weight (W, mg indiv.−1), as expressed by a power function (R=aW
b
, or logR=loga+b logW), was established as a function of temperature (T, °C). The slope of the regression equation (b) was not significantly affected by seasonal temperature variation, but the intercept of the equation (loga) was strongly influenced by temperature. The equation describing this general relation is logR=(0.0444T−0.333)+0.713 logW. 相似文献
6.
A large set of limb coronal mass ejections (CMEs) are used to determine the accurate relationship between radial (V
rad) and expansion (V
exp) speeds of CMEs. It is demonstrated that this relation is exceptionally well described by the function f(w)=1/2(1+cot w), representing a full cone model for the CME with a half-width, w. We also demonstrate that for extremely fast CMEs (V
exp>3000 km s−1), it is better to use the approximation V
rad≈V
LE. This implies that such CMEs expand spherically above the solar surface. 相似文献
7.
M. L. Mays O. C. St. Cyr E. Quémerais S. Ferron J.-L. Bertaux S. Yashiro R. Howard 《Solar physics》2007,241(1):113-125
In this study, the possibility that coronal mass ejections (CMEs) may be observed in neutral Lyman-α emission was investigated.
An observing campaign was initiated for SWAN (Solar Wind ANisotropies), a Lyman-α scanning photometer on board the Solar and
Heliospheric Observatory (SOHO) dedicated to monitoring the latitude distribution of the solar wind from its imprints on the
interstellar sky background. This was part of SOHO Joint Observing Program (JOP) 159 and was an exploratory investigation
as it was not known how, or even if, CMEs interact with the solar wind and interstellar neutral hydrogen at this distance
(≈60 and 120 R
S). The study addresses the lack of methods for tracking CMEs beyond the field-of-view of current coronagraphs (30 R
S). In our first method we used LASCO, white-light coronagraphs on SOHO, and EIT, an extreme ultraviolet imaging telescope
also on SOHO, to identify CME candidates which, subject to certain criteria, should have been observable in SWAN. The criteria
included SWAN observation time and location, CME position angle, and extrapolated speed. None of the CME candidates that we
discuss were identified in the SWAN data. For our second method we analyzed all of the SWAN data for 184 runs of the observing
campaign, and this has yielded one candidate CME detection. The candidate CME appears as a dimming of the background Lyman-α
intensity representing ≈10% of the original intensity, moving radially away from the Sun. Multiple candidate CMEs observed
by LASCO and EIT were found which may have caused this dimming. Here we discuss the campaign, data analysis technique and
statistics, and the results. 相似文献
8.
Large-scale, wave-like disturbances in extreme-ultraviolet (EUV) and type II radio bursts are often associated with coronal mass ejections (CMEs). Both phenomena may signify shock waves driven by CMEs. Taking EUV full-disk images at an unprecedented cadence, the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory has observed the so-called EIT waves or large-scale coronal propagating fronts (LCPFs) from their early evolution, which coincides with the period when most metric type II bursts occur. This article discusses the relation of LCPFs as captured by AIA with metric type II bursts. We show examples of type II bursts without a clear LCPF and fast LCPFs without a type II burst. Part of the disconnect between the two phenomena may be due to the difficulty in identifying them objectively. Furthermore, it is possible that the individual LCPFs and type II bursts may reflect different physical processes and external factors. In particular, the type II bursts that start at low frequencies and high altitudes tend to accompany an extended arc-shaped feature, which probably represents the 3D structure of the CME and the shock wave around it, and not just its near-surface track, which has usually been identified with EIT waves. This feature expands and propagates toward and beyond the limb. These events may be characterized by stretching of field lines in the radial direction and may be distinct from other LCPFs, which may be explained in terms of sudden lateral expansion of the coronal volume. Neither LCPFs nor type II bursts by themselves serve as necessary conditions for coronal shock waves, but these phenomena may provide useful information on the early evolution of the shock waves in 3D when both are clearly identified in eruptive events. 相似文献
9.
N. Gopalswamy S. Akiyama S. Yashiro G. Michalek R.P. Lepping 《Journal of Atmospheric and Solar》2009,71(8-9):1005-1009
10.
We study the kinematical characteristics and 3D geometry of a large-scale coronal wave that occurred in association with the
26 April 2008 flare-CME event. The wave was observed with the EUVI instruments aboard both STEREO spacecraft (STEREO-A and
STEREO-B) with a mean speed of ∼ 240 km s−1. The wave is more pronounced in the eastern propagation direction, and is thus, better observable in STEREO-B images. From
STEREO-B observations we derive two separate initiation centers for the wave, and their locations fit with the coronal dimming
regions. Assuming a simple geometry of the wave we reconstruct its 3D nature from combined STEREO-A and STEREO-B observations.
We find that the wave structure is asymmetric with an inclination toward East. The associated CME has a deprojected speed
of ∼ 750±50 km s−1, and it shows a non-radial outward motion toward the East with respect to the underlying source region location. Applying
the forward fitting model developed by Thernisien, Howard, and Vourlidas (Astrophys. J. 652, 763, 2006), we derive the CME flux rope position on the solar surface to be close to the dimming regions. We conclude that the expanding
flanks of the CME most likely drive and shape the coronal wave. 相似文献