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1.
Comparing space proton event data obtained during 1970-1980 with their identified Ha flare signatures we discover a peculiar correlation between them,according to which weak and small Ha flares can also produce proton events, and we reveal a characteristic “triangle” distribution of Ha flares accompanying proton events. In order to explain such feature of proton events, we accept the acceleration mechanism by DC electric field. To deduce the parallel electric field we use the electric current helicity (or force-free parameter α) determined by the Huairou vector magnetograph. A comparison of E|| with E⊥ shows that the former is negligible in flaring sites. We show that in the flaring current sheet ion-anisotropy is generated, and it, in turn, gives rise to ion-anisotropic instability which competes with electric acceleration to give one possibility: the acceleration by DC electric field or annihilation of the built-up energy. The competition of DC acceleration and ionanisotropic instability annihilation in the current sheet gives a possible explanation for the above-mentioned “triangle” character of the distribution.  相似文献   

2.
We present a statistical study of decimetric type Ⅲ radio bursts,coronal mass ejections(CMEs),and Hα flares observed in the period from July 2000 to March2005.In total,we investigated 395 decimetric type Ⅲ radio burst events,21% of which showed apparent correlation to CMEs that were associated with Hα flares.We noticed that the Hα flares which were strongly associated with CMEs were gradual events,and82% of them took place before CMEs appeared in the field of view of LASCO C2;that most of the CME-associated radio bursts started in the frequency range around750 MHz with a frequency drifting rate of several hundred MHz s-1,of which both positive and negative ones were recognized; and that the correlation of type Ⅲ radio bursts to CMEs without associated flares is fairly vague,less than 9%.  相似文献   

3.
White-light(WL) flares have been observed and studied for more than a century since their first discovery. However, some fundamental physics behind the brilliant emission remains highly controversial.One of the important facts in addressing the flare energetics is the spatio-temporal correlation between the WL emission and the hard X-ray(HXR) radiation, presumably suggesting that energetic electrons are the energy sources. In this study, we present a statistical analysis of 25 strong flares(≥M5) observed simultaneously by the Helioseismic and Magnetic Imager(HMI), on board the Solar Dynamics Observatory(SDO),and the Reuven Ramaty High Energy Solar Spectroscopic Imager(RHESSI). Among these events, WL emission was detected by SDO/HMI in 13 flares, associated with HXR emission. To quantitatively describe the strength of WL emission, equivalent area(EA) is defined as the integrated contrast enhancement over the entire flaring area. Our results show that the EA is inversely proportional to the HXR power-law index,indicating that stronger WL emission tends to be associated with a larger population of high energy electrons. However, no obvious correlation is found between WL emission and flux of non-thermal electrons at50 ke V. For the other group of 13 flares without detectable WL emission, the HXR spectra are softer(larger power-law index) than those flares with WL emission, especially for the X-class flares in this group.  相似文献   

4.
The fast rotation of sunspot group 5395 ( first, it exhibited inverse clockwise rotation, then clockwise rotation, the rotative angle was the lagrest 1-2 days before proton flare.) the stronger emission of SVC and the spectral maximun (near 8800MHz) of both the SVC and peak fluxes of the bursts et al are close correlated with occurrence of proton flares. Flares often generated in the regions of emerging or disappearing of new magnetic flux with opposite polarity, of the faster and more complex variation of the gradient and configuration of magnetic field, and of the neck and tail of magnetic gulf.  相似文献   

5.
Temporal and spectral characteristics of X-ray emission from 60 flares of intensity ≥C class observed by the Solar X-ray Spectrometer(SOXS) during 2003–2011 are presented. We analyze the X-ray emission observed in four and three energy bands by the Si and Cadmium-Zinc-Telluride(CZT)detectors, respectively. The number of peaks in the intensity profile of the flares varies between 1 and 3. We find moderate correlation(R ≈0.2) between the rise time and the peak flux of the first peak of the flare irrespective of energy band, which is indicative of its energy-independent nature. Moreover, the magnetic field complexity of the flaring region is found to be highly anti-correlated(R = 0.61) with the rise time of the flares while positively correlated(R = 0.28) with the peak flux of the flare. The time delay between the peak of the X-ray emission in a given energy band and that in 25–30 keV decreases with increasing energy, suggesting conduction cooling is dominant in the lower energies. Analysis of 340 spectra from 14 flares reveals that the peak of differential emission measure(DEM) evolution is delayed by 60–360 s relative to that of the temperature, and this time delay is inversely proportional to the peak flux of the flare. We conclude that temporal and intensity characteristics of flares are dependent on energy as well as the magnetic field configuration of the active region.  相似文献   

6.
Major solar flare events have been utilised to study the latitudinal frequency distribution of solar flares in northern and southern hemispheres for the period of 1986 to 2003. A statistical analysis has been performed to obtain the correlation between Coronal Mass Ejections (CMEs) and Forbush decrease (Fds) of cosmic ray intensity. Almost the same flares distribution in both hemispheres is found in association with CMEs. In a further analysis, it is noted that a larger number of CME-associated solar flares located in the northern hemisphere are found to be more effective in producing Forbush decreases.  相似文献   

7.
It has long been recognized that among Lhe solar radio bursts TypcⅡand strong Typc Ⅳ emissions are associated with proton flares or proton cvents. Howcver, rccent observotions show that solar cnergetic protons reaching the Earth arc preferentially profuced by long-duration, multiple-peak events as shown in Type Ⅳ_u/Ⅳ_(dm)  相似文献   

8.
Inspired by the finding that the large waiting time of solar flares presents a power-law distribution, we investigate the waiting time distribution (WTD) of coronal mass ejections (CMEs). SOHO/LASCO CME observations from 1996 to 2003 are used in this study. It is shown that the observed CMEs have a similar power-law behavior to the flares, with an almost identical power-law index. This strongly supports the viewpoint that solar flares and CMEs are different manifestations of the same physical process. We have also investigated separately the WTDs of fast-type and slow-type CMEs and found that their indices are identical, which imply that both types of CME may originate from the same physical mechanism.  相似文献   

9.
To investigate the dependence of large gradual solar energetic particle(SEP) events on the associated flares and coronal mass ejections(CMEs), the correlation coefficients(CCs) between peak intensities of E 10 MeV(I_(10)), E 30 MeV(I_(30)) and E 50 MeV(I_(50)) protons and soft X-ray(SXR) emission of associated flares and the speeds of associated CMEs in the three longitudinal areas W0–W39, W40–W70(hereafter the well connected region) and W71–W90 have been calculated.Classical correlation analysis shows that CCs between SXR emission and peak intensities of SEP events always reach their largest value in the well connected region and then decline dramatically in the longitudinal area outside the well connected region, suggesting that they may contribute to the production of SEPs in large SEP events. Both classical and partial correlation analyses show that SXR fluence is a better parameter describing the relationship between flares and SEP events. For large SEP events with source location in the well connected region, the CCs between SXR fluence and I_(10), I_(30) and I_(50) are0.58±0.12, 0.80±0.06 and 0.83±0.06 respectively, while the CCs between CME speed and I_(10), I_(30) and I_(50) are 0.56±0.12, 0.52±0.13 and 0.48±0.13 respectively. The partial correlation analyses show that in the well connected region, both CME shock and SXR fluence can significantly affect I_(10), but SXR peak flux makes no additional contribution. For E 30 MeV protons with source location in the well connected region, only SXR fluence can significantly affect I_(30), and the CME shock makes a small contribution to I_(30), but SXR peak flux makes no additional contribution. For E 50 MeV protons with source location in the well connected region, only SXR fluence can significantly affect I_(50), but both CME shock and SXR peak flux make no additional contribution. We conclude that these findings provide statistical evidence that for SEP events with source locations in the well connected region, a CME shock is only an effective accelerator for E 30 MeV protons. However, flares are not only effective accelerators for E 30 MeV protons, but also for E 30 MeV protons, and E 30 MeV protons may be mainly accelerated by concurrent flares.  相似文献   

10.
We study RXTE PCA data for the high mass X-ray binary source SMC X-1 between 2003–10 and 2003–12 when the source was in its high states.The source is found to be frequently bursting which can be seen as flares in lightcurves that occur at a rate of one every 800 s, with an average of 4–5 Type Ⅱ X-ray bursts per hour.We note that typically a burst was short, lasting for a few tens of seconds in addition to a few long bursts spanning more than a hundred seconds that were also observed.The flares apparently occupied 2.5% of the total observing time of 225.5 ks.We note a total of 272 flares with mean FWHM of the flare ～21 s.The rms variability and aperiodic variability are independent of flares.As observed, the pulse profiles of the lightcurves do not change their shape, implying that there is no change in the geometry of an accretion disk due to a burst.The hardness ratio and rms variability of lightcurves exhibit no correlation with the flares.The flare fraction shows a positive correlation with the peak-to-peak ratio of the primary and secondary peaks of the pulse profile.The observed hardening or softening of the spectrum cannot be correlated with the flaring rate but may be due to the interstellar absorption of X-rays as evident from the change in hydrogen column density(n_H).It is found that the luminosity of the source increases with the flaring rate.Considering that the viscous timescale is equal to the mean recurrence time of flares, we fixed the viscosity parameter α～ 0.16.  相似文献   

11.
We propose a magnetic confinement nuclear fusion mechanism for the evolution of a solar flare in the solar atmosphere.The mechanism agrees with two observed characteristics of explosive flares and coronal mass ejections(CMEs) that have proved to be very difficult to explain with previous mechanisms:the huge enrichments of3 He and the high energy gamma ray radiation.The twisted magnetic flux rope is a typical structure during the solar flares,which is closely related to the solar active region that magnetic fields have almost complete control over the plasma.Consequently,the plasma inside the flux rope is heated to more than 1.0×107 K by an adiabatic compression process,and then the thermonuclear fusion can take place in the flux rope accompanied with high energy gamma rays.We utilize the time-dependent ideal 2.5-dimensional magnetohydrodynamic(MHD) simulation to demonstrate the physical mechanism for producing flares,which reveals three stages of flare development with the process of magnetic energy conversion and intense release during the solar flares and CMEs in the solar atmosphere.Furthermore,we discuss the relationship between magnetic reconnection and solar eruptions.  相似文献   

12.
The cosmic ray Forbush Decreases (FDs) are frequently related to the solar flares. Statistically, only the bright flares of importance 3 and that of importance 2 but with duration ≥1.5 hours can significantly disturb the cosmic ray intensity. The flares located near the solar central meridian can cause the larger FDs than that located at the limb. In this paper it is found that a SF flare located at the limb, having long duration and being strong X-ray burst enough or accompanying by a energetic event having quite long duration, can also produce the obvious FDs.  相似文献   

13.
X-ray flares are the most common phenomena in the afterglow phase of gamma-ray bursts(GRBs) in the Swift era,and are known as a canonical component in X-ray afterglows.In this work,we constrain the Lorentz factor of X-ray flares with an updated sample.We extensively search for X-ray light curves showing flare and jet break simultaneously.A smooth broken power law function is used to fit the jet breaks in 11 GRBs.We also use a smooth broken power law function to fit the profile of X-ray flares,and the total number of the flares is 20.We obtain the lower and upper limits of Lorentz factor(Γ_X) with the timescale,half-opening angle and mean luminosity of the X-ray flares for interstellar medium(ISM) and wind cases.The lower limits on Γ_X range from tens to a few hundred,and the upper limits are mainly about a few hundred.We also apply the limited Lorentz factor to test correlations of Γ_0-E_(γ,iso) and Γ_0-L_(γ,iso) for GRBs,and find X-ray flares in the ISM case are much more consistent with those of prompt emission than the wind case in a statistical sense for both correlations.X-ray flares are almost consistent with the trend in the correlations of Γ_0-E__(γ,iso)(L_(γ,iso)) for prompt GRBs,indicating X-ray flares and prompt bursts may have the same physical origin.  相似文献   

14.
We report on an archival X-ray observation of the eclipsing RS CVn binary XY UMa(P_(orb) ≈0.48 d). In two Chandra ACIS observations spanning 200 ks and almost five orbital periods, three flares occurred. We find no evidence for eclipses in the X-ray flux. The flares took place around times of primary eclipse, with one flare occurring shortly( 0.125 P_(orb)) after a primary eclipse, and the other two happening shortly( 0.05 P_(orb)) before a primary eclipse. Two flares occurred within roughly one orbital period(?φ≈1.024 P_(orb)) of each other. We analyze the light curve and spectra of the system, and investigate coronal length scales during both quiescence and flares, as well as the timing of the flares. We explore the possibility that the flares are orbit-induced by introducing a small orbital eccentricity, which is quite challenging for this close binary.  相似文献   

15.
We reported recently some rapid changes of sunspot structure in white-light(WL) associated with major flares.We extend the study to smaller events and present here results of a statistical study of this phenomenon.In total,we investigate 403 events from 1998 May 9 to 2004 July 17,including 40 X-class,174 M-class,and 189 C-class flares.By monitoring the structure of the flaring active regions using the WL observations from the Transition Region and Coronal Explorer(TRACE),we find that segments in the outer sunspot structure decayed rapidly right after many flares;and that,on the other hand,the central part of sunspots near the flare-associated magnetic neutral line became darkened.These rapid and permanent changes are evidenced in the time profiles of WL mean intensity and are not likely resulted from the flare emissions.Our study further shows that the outer sunspot structure decay as well as the central structure darkening are more likely to be detected in larger solar flares.For X-class flares,over 40% events show distinct sunspot structure change.For M-and C-class flares,this percentage drops to 17% and 10%,respectively.The results of this statistical study support our previously proposed reconnection picture,i.e.,the flare-related magnetic fields evolve from a highly inclined to a more vertical configuration.  相似文献   

16.
Three particularly complex radio bursts (2001 October 19, 2001 April 10 and 2003 October 26) obtained with the spectrometers (0.65-7.6GHz) at the National Astronomical Observatories, Chinese Academy of Sciences (NAOC, Beijing and Yunnan) and other in- struments (NoRH, TRACE and SXT) are presented. They each have two groups of peaks occurring in different frequency ranges (broad-band microwave and narrow-band decimeter wavelengths). We stress that the second group of burst peaks that occurred in the late phase of the flares and associated with post-flare loops may be homologous radio bursts. We think that they are driven by the post-flare loops. In contrast to the time profiles of the radio bursts and the images of coronal magnetic polarities, we are able to find that the three events are caused by the active regions including main single-bipole magnetic structures, which are associated with multipole magnetic structures during the flare evolutions. In particular, we point out that the later decimetric radio bursts are possibly the radio counterparts of the homologous flares (called "homologous radio bursts" by us), which are also driven by the single-bipole mag- netic structures. By examining the evolutions of the magnetic polarities of sources (17GHz), we could presume that the drivers of the homologous radio bursts are new and/or recurring appearances/disappearances of the magnetic polarities of radio sources, and that the triggers are the magnetic reconnections of single-bipole configurations.  相似文献   

17.
It has been found for a long time, with analysing the variation of the relative number of sunspot, that there exist the periodicity of 11 years in solar activity. With the deepening research of the varied solar active phenomena, a series of periodicities with different periods have been also found in solar activity. For example, there is the periodicity of about 80 days for the occurrence, rate of proton flares for solar activity cycles 19 and 20 found by Ai and Fan ci:i at 1974. Recently a periodicity of about 152 days of the occurrence rate of solar flares has been proposed by some authors. a3'5>7:i The existence of this periodicity hsa been proved in the various solar flares. In this paper using the data of solar microwave bursts from January 1986 to December 1988, a Fourier analysis of the occurrence rate of solar microwave bursts has been made. There was no periodicity for the occurrence rate of solar microwave bursts of about 152 days found. This is a new result for solar cycle 22 in the first thr  相似文献   

18.
Five segments of sheared magnetic polarity inversion lines with their positions relative to the main spots in AR 5395 are indentified. The observational' results of fine structure of sunspots and the chromospheric filaments associated with the identified sheared ineversion lines show that (1) magnetic shear is intimately tied to 5 spot and spiral spots, (2) the sheared field over the inversion line usually contains a chromospheric filament, (3) orientation of fibrils in the filament lying over a sheared inversion line are often evidently not perpendicular to the inversion line, (4) twisting sometimes occurs in some filaments tracing sheared lines. The inverstigation of the flares in AR 5395 observed with 26cm solar telescope during 9-16 March shows that (1) all of the flares with optical importance≥ 1 or X-ray class≥M1 occur quite near the sheared inversion lines, (2) a 3N/ X1.2 flare on 13 March, the largest one, occured on both sides of the segment A, the longest and most complicated sheared inversi  相似文献   

19.
We conducted photometric and spectroscopic observations of Ross 15 in order to further study the flare properties of this less observed flare star.A total of 28 B-band flares are detected in 128 hr of photometric observations,leading to a total flare rate of 0.22-0.040.04 h-1,more accurate than that provided by previous work.We give the energy range of the B-band flare(1029.5-1031.5 erg) and the flare frequency distribution(FFD) for the star.Within the same energy range,the FFD is lower than that of GJ 1243(M4)and YZ CMi(M4.5),roughly in the middle of those of three M5-type stars and higher than the average FFDs of spectral types> M6.We performed,for the first time for Ross 15,simultaneous high-cadence spectroscopic and photometric observations,resulting in detection of the most energetic flare in our sample.The intensity enhancements of the continuum and Balmer lines with significant correlations between them are detected during the flare,which is the same as those of other deeply studied flare stars with similar spectral type.  相似文献   

20.
To investigate the possible solar source of high-energy protons, correlation coefficients between the peak intensities of E ≥ 100 MeV protons, I100, and the peak flux and fluence of solar soft X-ray(SXR) emission, and coronal mass ejection(CME) linear speed in the three longitudinal areas W0–W39, W40–W70 and W71–W90 have been calculated respectively. Classical correlation analysis shows that the correlation coefficients between CME speeds and I100 in the three longitudinal areas are0.28±0.21, 0.35±0.21 and 0.04±0.30 respectively. The classical correlation coefficients between I100 and SXR peak flux in the three longitudinal areas are 0.48±0.17, 0.72±0.13 and 0.02±0.30 respectively, while the correlation coefficients between I100 and SXR fluence in the three longitudinal areas are 0.25±0.21, 0.84±0.07 and 0.10±0.30 respectively. Partial correlation analysis shows that for solar proton events with source location in the well connected region(W40–W70), only SXR fluence can significantly affect the peak intensity of E ≥ 100 MeV protons, but SXR peak flux has little influence on the peak intensities of E ≥ 100 MeV protons; moreover, CME speed has no influence on the peak intensities of E ≥ 100 MeV protons. We conclude that these findings provide statistical evidence that E ≥ 100 MeV protons may be mainly accelerated by concurrent flares.  相似文献   

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