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Local helioseismic techniques, such as ring analysis and time-distance helioseismology, have already shown that large-scale
flows near the surface converge towards major active regions. Ring analysis has further demonstrated that at greater depths
some active regions exhibit strong outflows. A critique leveled at the ring-analysis results is that the Regularized Least
Squares (RLS) inversion kernels on which they are based have negative sidelobes near the surface. Such sidelobes could result
in a surface inflow being misidentified as a diverging outflow at depth. In this paper we show that the Optimally Located
Averages (OLA) inversion technique, which produces kernels without significant sidelobes, generates flows markedly similar
to the RLS results. Active regions are universally zones of convergence near the surface, while large complexes evince strong
outflows deeper down. 相似文献
2.
Haber D.A. Hindman B.W. Toomre J. Bogart R.S. Thompson M.J. Hill F. 《Solar physics》2000,192(1-2):335-350
We report on large-scale horizontal flows in the solar convection zone and their variability in time and space using a local-helioseismology technique known as ring-diagram analysis. By performing this analysis on a dense mosaic of individual regions on the solar disk, i.e., a `Dense-Pack' sampling, and repeating the analysis periodically on several time scales, we are able to assess the variation of horizontal flows from day-to-day, week-to-week, and year-to-year. We find that although there are changes in the flows on all these time scales, there are also basic patterns that persist. On a daily time scale we observe that the flow is reduced in those areas which are occupied by large active regions. On somewhat longer time-scales we see bands of persistent fast and slow zonal flow that are identifiable as torsional oscillations. As we examine these bands during a series of years, we find that these bands migrate toward the equator as solar activity increases. Similarly, the latitudes at which the meridional flow reaches maximum follow these regions of fast zonal flow as they migrate equatorwards. These Dense-Pack samplings also reveal substantial differences in the zonal and meridional flow patterns in the northern and southern hemispheres. 相似文献
3.
H. Moradi C. Baldner A. C. Birch D. C. Braun R. H. Cameron T. L. Duvall Jr. L. Gizon D. Haber S. M. Hanasoge B. W. Hindman J. Jackiewicz E. Khomenko R. Komm P. Rajaguru M. Rempel M. Roth R. Schlichenmaier H. Schunker H. C. Spruit K. G. Strassmeier M. J. Thompson S. Zharkov 《Solar physics》2010,267(1):1-62
While sunspots are easily observed at the solar surface, determining their subsurface structure is not trivial. There are two main hypotheses for the subsurface structure of sunspots: the monolithic model and the cluster model. Local helioseismology is the only means by which we can investigate subphotospheric structure. However, as current linear inversion techniques do not yet allow helioseismology to probe the internal structure with sufficient confidence to distinguish between the monolith and cluster models, the development of physically realistic sunspot models are a priority for helioseismologists. This is because they are not only important indicators of the variety of physical effects that may influence helioseismic inferences in active regions, but they also enable detailed assessments of the validity of helioseismic interpretations through numerical forward modeling. In this article, we provide a critical review of the existing sunspot models and an overview of numerical methods employed to model wave propagation through model sunspots. We then carry out a helioseismic analysis of the sunspot in Active Region 9787 and address the serious inconsistencies uncovered by Gizon et al. (2009a, 2009b). We find that this sunspot is most probably associated with a shallow, positive wave-speed perturbation (unlike the traditional two-layer model) and that travel-time measurements are consistent with a horizontal outflow in the surrounding moat. 相似文献
4.
R. Howe R. Komm F. Hill R. Ulrich D. A. Haber B. W. Hindman J. Schou M. J. Thompson 《Solar physics》2006,235(1-2):1-15
Migrating bands of weak, zonal flow, associated with the activity bands in the solar cycle, have been observed at the solar
surface for some time. More recently, these flows have been probed deep within the convection zone using global helioseismology
and examined in more detail close to the surface with the techniques of local helioseismology. We compare the near-surface
results from global and local helioseismology using data from the Michelson Doppler Imager and the Global Oscillation Network
Group with surface Doppler velocity measurements from the Mount Wilson 150-foot tower and find that the results are in reasonable
agreement, with some explicable differences in detail. All of the data sets show zones of faster rotation approaching the
equator from mid-latitudes during the solar cycle, with a variation at any given location that can be approximately, but not
completely, described by a single sinusoid and an amplitude that does not drop off steeply below the surface. 相似文献
5.
Randolph D. Borys Edward E. Hindman Paul J. DeMott 《Journal of Atmospheric Chemistry》1988,7(3):213-239
The relationships between the physical and chemical properties of mixed-phase clouds were investigated at Storm Peak Laboratory (3220m MSL) located near the continental divide in northwestern Colorado. Interstitial aerosol particles, cloud droplets and snow crystals were concurrently collected when the laboratory was enveloped by a precipitating cloud. All samples were analyzed for trace elements, soluble anions, electrical conductivity and acidity.The results show average trace constituent concentration ratios of cloud water to snow water range from 0.4 to 26. All but six of the 32 elements and ions measured had ratios greater than one. This result suggests a chemical species dependency of in-cloud aerosol particle scavenging processes. Evidence of a decrease of in-cloud aerosol particle scavenging efficiency by snow due to increases in aerosol concentration is also presented.Differences between the chemical composition of cloud water and snow water are manifested most strongly when snow crystals grow by vapor deposition. In-cloud scavenging efficiencies by snow crystals for most aerosol particle chemical species are dependent on the growth of the snow crystals by accretion of cloud droplets. This chemical fractionation of the atmospheric aerosol by snow crystal formation and growth should be most active where narrow, continental cloud droplet size distributions and low liquid water contents are prevalent, enhancing the probability of snow crystal growth by diffusion. 相似文献
6.
Using data from SOI-MDI (Haber et al., 2000), we compute the local frequencies of high-degree p modes and f modes. The frequencies are obtained through ring-diagram mode fitting. The Dense-Pack data set consists of a mosaic of 189 overlapping tiles, each tracked separately at the surface rotation rate over 1664-min time intervals during the Dynamics Programs. Each tile is 16° square and the tile centers are separated by 7.5° in latitude and longitude. For each sampling day and for each tile, we have computed the frequency shift measured relative to the temporal and spatial average of the entire set of frequencies. The motion of active regions as they rotate across the solar disk is vividly traced by these measurements. Active regions appear as locations of large positive frequency shifts. If the shifts are averaged over the solar disk and are scaled down to the appropriate wave number regime, the magnitude and frequency dependence of the shifts are consistent with the measured changes in global oscillation frequencies that occur over the solar cycle. As with the frequency shifts of low-degree global oscillations, the frequency dependence of the shifts indicates that the physical phenomena inducing the shifts is confined to the surface layers of the Sun. 相似文献
7.
Inferences of subsurface flow velocities using local domain ring-diagram helioseismology depend on measuring the frequency shifts of oscillation modes seen in acoustic power spectra. Current methods for making these measurements use maximum-likelihood fitting techniques to match a model of modal power to the spectra. The model typically describes a single oscillation mode, and each mode in a given power spectrum is fit independently. We present a new method that produces measurements with higher reliability and accuracy by fitting multiple modes simultaneously. We demonstrate that this method permits measuring sub-surface flows deeper into the Sun while providing higher uniformity in data coverage and velocity response closer to the limb of the solar disk. While the previous fitting method performs better for some measurements of low phase-speed modes, we find this new method to be particularly useful for high phase-speed modes and small spatial areas. 相似文献
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