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1.
We analyze the properties of the electric-current distribution over the cross sections of fairly dense coronal magnetic flux tubes in which the plasma pressure exceeds the magnetic pressure, so that the equilibrium is maintained by the ambient magnetic field. If the plasma is fully ionized, the distributions of the longitudinal and azimuthal currents over the cross section of the loop have the same spatial scale as the pressure distribution. However, even a small number of neutral atoms in the corona (with a mass fraction of the order of 10?5, taking into account the partial ionization of helium) substantially modifies the current distribution over the tube cross section: in this case, a considerable fraction of the full current flowing along the tube is concentrated in a thin region near the axis with a radius of the order of (10?2–10?3)r 0 (where r 0 is the characteristic scale of the plasma-pressure distribution over the tube), thus forming a sort of a jet current. This comes about because the pattern of the conductivity anisotropy is substantially modified in the presence of ion-atom collisions in the magnetoactive plasma of the tube, and the Cowling conductivity dominates over the Hall and Pedersen conductivities. The high current density near the axis of the tube can ensure heating of the plasma to coronal temperatures via Joule dissipation. 相似文献
2.
We examine plasma heating due to the dissipation of acoustic waves excited in coronal magnetic loops by parametric resonance
with the five-minute oscillations in the velocity of the photospheric convection. The energy of acoustic waves excited in
the coronal magnetic loop, rate of dissipation of acoustic waves, and rate of heating of the coronal plasma are determined.
The maximum temperature predicted for the apex of the loop is calculated as a function of the velocity of photospheric oscillations,
length of the loop, and electric current in the loop. It is shown that the mechanism proposed can explain the origin of quasi-stationary
X-ray loops with temperatures of 3–6 MK. The lengths of these loops are resonant for acoustic waves excited by the five-minute
photospheric oscillations. The use of the proposed mechanism to explain heating of the X-ray loops expected to be on stars
of late spectral types is discussed. 相似文献
3.
Quasi-periodic modulations of the microwave emission from solar outbursts at 37 GHz are studied based on 17 events observed in 1989–2000 at the Metsähovi Observatory. Low-frequency modulations with periods of ~5 min were found in approximately 90% of the observed microwave outbursts. The most likely origin of this modulation is modulation of the current flowing along a closed coronal magnetic loop due to the five-minute oscillations of the photospheric-convection velocity. In approximately 70% of the cases, oscillations with periods ~10 min were observed simultaneously with the five-minute oscillations in the same events. In 30% of the cases, simultaneous modulation of the microwave emission by three low-frequency signals with periods of 3, 5, and 10 min was observed. One possible origin of these “double” and “triple” modulations is parametric excitation of acoustic oscillations with periods of 10 and 3 min in a closed coronal magnetic loop as a result of coupling with the five-minute photospheric oscillations. This can occur when the period of the natural acoustic oscillations of the closed magnetic loop is about 10 min (the resonance condition). Since the ten-minute oscillations are excited more easily than the three-minute oscillations at the parametric instability, the latter are observed less frequently. For the same reason, the observed linewidth of the ten-minute oscillations is considerably greater than that of the three-minute oscillations. 相似文献
4.
5.
The excitation of the ballooning instability by the eigenoscillations of coronal loops is analyzed using the energy method. The second variation of the potential energy for the case of a plasma—plasma boundary is obtained via the linearized ideal MHD equations. It is shown that the eigenmodes of a magnetic tube and of a toroidal coronal loop coincide in a first approximation. The bending oscillations of the loops are able to excite the ballooning instability when β ? 1. The effects of the instability in solar coronal loops are discussed. 相似文献
6.
I. Yu. Grigor’eva M. A. Livshits G. V. Rudenko I. I. Mysh’yakov 《Astronomy Reports》2013,57(8):611-621
Data on small active regions on the Sun collected over three years (2007–2009) are analyzed. Under very quiescent conditions (a low X-ray background level), the shapes of the coronal loops of some active regions correspond fairly well to the shapes of magnetic-field lines calculated in a potential approximation. This is true of several active regions (e.g., the group AR 10999 in June 2008) in which no flares more powerful than B3 were observed. The radio emission of this active region detected by the RATAN-600 telescope was very weak and virtually no polarization was detected. Subflares were observed in most groups. It is demonstrated using AR 10933 (January 2007) as an example that a growth in the soft X-ray emission by up to factors of ten simultaneous with an increase in the radio flux is characteristic for such active regions. A source with the opposite polarization developed to the Northwest of the main spot in AR 10933. A series of SOHO/MDI (and also Hinode) magnetograms shows the emergence of new magnetic flux before the development of this polarized source, which continued for several hours on January 8, 2007. The current density at surfaces located at various heights is estimated based on observations of the total vector magnetic field (Hinode data) and a non-linear, force-free magnetic-field extrapolation. The height-integrated current becomes appreciably stronger at two nodes above a field neutral line, near the location of the main emerging flux. This supports the idea that the emergence of new magnetic flux is a key factor in the evolution of active regions at all stages of their existence. The development of this picture could help in elucidating the inter-relationship between current enhancements, plasma heating, and particle acceleration, in both weak active regions and strong activity complexes. 相似文献
7.
Episodic observations of coronal holes were carried out simultaneously in several spectral lines during the 2002–2005 observational seasons. An analysis of eighteen time series is used to obtain the amplitude—spectral properties of oscillatory wave motions of the solar plasma at the bases of coronal holes. It is found that the amplitudes of the 5-min and 3-min line-of-sight velocity oscillations increase in coronal holes. Low-frequency (1–2 mHz) oscillations are concentrated at the boundaries of the chromospheric network, while the 3-mHz and 5-mHz oscillations dominate in the network cells. Clear indications of propagating waves have been found at the bases of coronal holes. The 3 mHz phase velocities are 45 ± 5 km/s and 80–100 km/s for the equatorial and polar coronal holes, respectively. 相似文献
8.
Synoptic maps of the intensity of the λ530.5 nm FeXIV green coronal line and maps of computed coronal magnetic fields for the period 1977–2001 are compared. For quantitative comparisons, the correlation coefficients r for the correlation between these two parameters at corresponding points of the synoptic maps are calculated. This coefficient exhibits cyclic variations in the spot-formation zone, ±30° and the zone above 30° and is in antiphase in these two zones. In the low-latitude zone, the correlation coefficient is always positive, reaches its maximum at activity minimum, and strongly decreases by activity maximum. Above 30°, r reaches maximum positive values at activity maximum and then gradually decreases, passing through zero near the beginning of the phase of activity minimum and becoming negative during this phase. A Fourier analysis of r as a function of time reveals a wavelike variation with a period close to 1.3 yr (known also from helioseismological data for the tachoclinic region of magnetic-field generation), as well as a pronounced wave with a period of about 5 yr. The latitude dependence of r seems to be related to variations in the contributions from local, large-scale, and global fields. Our analysis suggests an approach to studying the complex problem of mechanisms for coronal heating. 相似文献
9.
The magnetic fields of solar active regions are analyzed using a method based on comparing the spatial structures of the reconstructed magnetic field and of the radio emission of the active region. Two approaches are used: comparing the radio size of the active region and the corresponding size calculated using the reconstructed magnetic field, and comparing the radio spectra that are observed and calculated using the reconstructed magnetic field. Overall, the calculated sizes and spectra correspond fairly well to the observational data, making it possible to estimate physical parameters of the emitting region, such as the electron density and temperature. 相似文献
10.
A model for the generation of solar millisecond radio spikes via a maser cyclotron resonance is proposed. The model takes into account the large-scale inhomogeneity of the magnetic field and small-scale inhomogeneities of the coronal plasma. The efficiency of the energy transformation from a electron beam into maser radiation is estimated. Appropriate parameters of the magnetic field inhomogeneity and the plasma turbulence are found. 相似文献
11.
Two impulsive limb coronal mass ejections (CMEs), one of which was accompanied by an active prominence and the other by a flare, are analyzed using AIA/SDO solar data. The analysis leads to the conclusion that, in both cases, the sources of the CME formation were magnetic tubes rising from beneath the photosphere at high velocity. One or more arch structures can be located in the path of the magnetic tube, which it influences and drags along with it. The arch structures may then participate in the formation of the future CME, whose main basis is the magnetic tube itself. 相似文献
12.
O. G. Badalyan 《Astronomy Reports》2013,57(3):222-232
The relationship between the brightness in the FeXIV 530.3 nm coronal green line and magnetic fields on various scales in the corona is studied quantitatively. The cross-correlations of the corresponding synoptic maps for 1977–2001 have been calculated. Maps of the brightness of the coronal green line are constructed using daily monitoring data. Maps of the magnetic field are constructed separately for fields on large and small spatial scales, based on computations in a potential approximation using photospheric observations for distances of 1.1R ⊙ carried out at the Wilcox Solar Observatory. The correlations between the brightness in the coronal green line and the magnetic-field strengths on various scales as a function of latitude have a cyclic character. The correlation coefficients in the spot-formation zone are positive. Here, the green-line brightness corresponds mainly to the strength of small-scale fields, corresponding to the sizes of large active regions and activity complexes. The correlation coefficients are sign-variable above 40° latitude, and reach their greatest positive and negative values at the cyclemaximum and minimum. Larger-scale fields influence the green-line brightness at higher latitudes and near the phase of the cycle minimum. The results obtained can be used to investigate mechanisms for heating the corona. The relationship between the results obtained and the subsurface and deep solar dynamos are also discussed. 相似文献
13.
The fundamental possibility of reliably removing the π ambiguity from the transverse magnetic field detected in solar vector magnetographic measurements, independent of the location of the vector magnetograms on the solar disk is demonstrated. The corrected magnetograms are then used as boundary conditions for the reconstruction of the three-dimensional magnetic field. The calculated field lines agree well with observed non-potential magnetic loops. The π ambiguity is removed using a modified Metropolis algorithm adapted to a spherical geometry. The spatial configuration of the magnetic field is calculated in a nonlinear force-free approximation using an optimization method. Tests of the new algorithm for resolving the π ambiguity are demonstrated for various model cases and comparisons with results of the NPFC method. 相似文献
14.
V. D. Shchepkin D. I. Vainshtein R. A. Dautov V. M. Vinokurov 《Physics and Chemistry of Minerals》1980,6(4):269-281
Double nuclear magnetic resonance (DNMR) with Jeener's pulsed sequence on proton and fluorine frequencies was used to investigate the electric quadrupole interactions of (i) 23Na in Na2Cd(SO4)2·2H2O, B 2 0 =±218.5±1 kHz, B 2 2 =±98±5 kHz, (ii) of 23Na, which enter the crystal, CaF2: Na+ (0.07 wt. %) B 2 0 =±85.7±0.5 kHz, trigonal position, and (iii) 23Na which are near the foreign atom in NaF:Ca2+ (0.02 wt.%) B 2 0 =±86.7±0.5 kHz, tetragonal position. Some details of DNMR experiments are analyzed. The conditions for maximum transfer of a Zeeman energy to a dipole-dipole reservoir are described for multispin systems and some crystal hydrates. The angular dependence of the Hamiltonian containing the spherical tensor operators of second rank was obtained for all possible orientations of a local coordinate system relative to a laboratory system. 相似文献
15.
The presence of additional plasma streams with enhanced density in bright rays of the solar coronal-streamer belt is demonstrated. The streams have steep fronts, whose widths δ≈0.10R⊙ (where R⊙ is the solar radius) are comparable to the spatial resolution of the LASCO C3 instrument of the SOHO satellite. The additional streams are similar to streams of the slow, quasi-steady solar wind in the streamer belt in terms of their plasma density, directional velocity, and lifetime and are apparently one of the main sources of the slow solar wind. 相似文献
16.
Chiaki Uyeda Akira Tsuchiyama Takamitu Yamanaka Muneyuki Date 《Physics and Chemistry of Minerals》1993,20(2):82-85
The harmonic oscillations of large diamagnetic mineral samples induced by a magnetic field is reported, for single crystals of quartz, corundum, and calcite. It was seen for the first time that the period of oscillation, , was proportional to the reciprocal of the magnetic field, H, where the restoring force of the string suspending the crystal became negligible in the high magnetic field. Accordingly, the value of diamagnetic anisotropy, , could be measured from the — H curve with a sensitivity of 5 × 10–10 emu/cc. The values were 5.50 × 10–9 emu/cc for quartz, 4.20 × 10–9 emu/cc for corundum, 9.9 × 10–8 emu/cc for calcite, and 8.8 × 10–8 emu/cc for polycrystalline talc piled with the (001) planes aligned parallel. Significant field-induced rotations were observed for the suspended crystals. When the field was applied along the direction of the diamagnetic hard axis of the stationary crystal, the crystal gradually rotated with increasing field, so that the direction of the hard-axis was perpendicular to the applied field. The field-induced energy has a the maximum value when the field is applied along the diamagnetic hard axis. This reorientation of the crystal occurs because the torque due to the field-induced anisotropic energy exceeds that of the restoring force in high magnetic fields. 相似文献
17.
The origin of high magnetic remanence in fault pseudotachylites: Theoretical considerations and implication for coseismic electrical currents 总被引:2,自引:0,他引:2
E.C. Ferr M.S. Zechmeister J.W. Geissman N. MathanaSekaran K. Kocak 《Tectonophysics》2005,402(1-4):125
Several examples of fault-related pseudotachylites display a significantly higher initial magnetic susceptibility than their granitic host rock (10:1 to 20:1). These higher values are attributed to the presence of fine magnetic particles formed during melt quenching. The hysteresis properties of the particles indicate a single domain (SD) to pseudo single domain (PSD) magnetic grain size. The Curie temperature (Tc) of the magnetic particles is close to 580 °C.The natural remanent magnetization (NRM) of these pseudotachylites is also significantly higher than that of the host rock (up to 300:1). Such anomalously high remanence cannot be explained by a magnetization acquired in the Earth's magnetic field, regardless of pseudotachylite age.Ground lightning and other strong electric pulses can cause anomalously high NRM intensities. A ground lightning explanation seems unlikely to explain the systematically high NRM intensities, particularly in the case of recently exposed samples that have been collected from active quarries. Alternatively, high NRM intensities could be explained by earthquake lightning (EQL), a seismic phenomenon occasionally reported in connection with large magnitude earthquakes (M > 6.0).The coseismic electrical properties of the pseudotachylite vein–host rock system are characterized by (1) a core of molten material (high conductivity), (2) vapor-rich margins of thermally and mechanically fractured host rocks (low conductivity) and (3) moderately fractured to undeformed host rock (normal conductivity). Such a core conductor bordered by insulating margins is potentially responsible for the propagation of EQL pulses.The coseismic thermal history of pseudotachylite veins has been modeled in 2-D using conductive heat transfer equations. It shows that EQL can be recorded only during a brief time interval (less than 1 min) for a given vein thickness and host-rock temperatures. If the vein is too thick or if the host rock is too hot, the pseudotachylite remains above Tc after the electric pulse has lapsed. 相似文献
18.
A. I. Efimov L. N. Samoznaev V. K. Rudash I. V. Chasheĭ M. K. Bird D. Plettemeier 《Astronomy Reports》2007,51(8):687-694
Measurements of frequency fluctuations in radio signals generated by the GALILEO spacecraft from January 6 to 11, 1997 are presented and analyzed. The passage of a coronal mass ejection observed by the SOHO/LASCO coronagraph on January 6, 1997 through the radio-communication path between the spacecraft and a ground station was recorded. Radio sounding was carried out at a carrier frequency of 2295 MHz at a heliocentric distance of about 32 solar radii, with the signal being received at three ground stations. As the mass ejection intersected the propagation path, the mean frequency of the signal increased and several-hour-long frequency fluctuations were enhanced. A spectral analysis of the frequency fluctuations shows that the regime and level of plasma turbulence are substantially different in different sections of the quiet solar wind and the disturbed plasmoid. A correlation between the intensity and temporal spectrum of the frequency fluctuations is found. The plasma density in the leading part of the coronal mass ejection exceeds the mean background value by more than an order of magnitude. Our correlation analysis of the frequency fluctuations recorded simultaneously at two widely separated measuring points shows that two flow components with different velocities—the quiet solar wind and a perturbed stream—crossed the communication path. The radio-sounding data are compared with observations of the coronal mass ejection by the SOHO/LASCO coronagraph and plasma measurements near the Earth’s orbit using the WIND satellite. A pronounced correlation is found between the variations in the mean frequency of the sounding signal and the plasma density in near-Earth space. 相似文献
19.
It is proposed that the formation of the morphology of solar magnetic cavities and of the topology of their magnetic fields at a certain stage of their evolution (a decay of a quasi-uniform, rotating, magnetized cylindrical layer into rings, followed by their deformation and the generation of internal fine structure etc.) can be attributed to the excitation of a shear-centrifugal-resonance instability. The calculations show the existence of two families of unstable modes: resonance-gyroscopic modes due to the rotation of the layer and fast magneto acoustic waves propagating outside the layer and resonating in phase with intra-layer perturbations. Both families contain a large number of unstable waveguide harmonics, with the superposition and interaction of these harmonics being responsible for the extremely complex structure of coronal cavities. 相似文献
20.