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The spatial and spectral behaviors of two solar flares observed by the Nobeyama Radioheliograph (NoRH) on 24 August 2002 and
22 August 2005 are explored. They were observed with a single loop-top source and double footpoint sources at the beginning,
then with looplike structures for the rest of the event. NoRH has high spatial and temporal resolution at the two frequencies
of 17 and 34 GHz where a nonthermal radio source is often optically thin. Such capabilities give us an opportunity to study
the spatial and spectral behaviors of different microwave sources. The 24 August 2002 flare displayed a soft – hard – soft
(SHS) spectral pattern in the rising – peak – decay phases at 34 GHz, which was also observed for the spectral behavior of
both loop-top and footpoint sources. In contrast, the 22 August 2005 flare showed a soft – hard – harder (SHH) spectral pattern
for its both loop-top and footpoint sources. It is interesting that this event showed a harder spectrum in the early rising
phase. We found a positive correlation between the spectral index and microwave flux in both the loop-top source and the footpoint
sources in both events. The conclusions drawn from the flux index could apply to the electron index as well, because of their
simple linear relationship under the assumption of nonthermal gyrosynchrotron mechanism. Such a property of spatial and spectral
behaviors of microwave sources gives an observational constraint on the electron acceleration mechanism and electron propagation. 相似文献
43.
2010-2011年深圳湾浮游植物季节变化及其与环境因子关系 总被引：3，自引：0，他引：3
2010-2011年对深圳湾水采浮游植物进行了4个航次的现场调查,共鉴定出浮游植物5门45属83种,硅藻门占总种数的83.1%,甲藻门占10.8%。种类组成以广温广盐种和暖水种为主,中肋骨条藻(skeletonema costatum)为该海域常年优势种。此次调查发现深圳湾海域浮游植物丰度年波动范围为9.63~19904.0×103/L,平均值为964.5×103/L表现为秋季最高,夏、冬季次之,春季最低。浮游植物多样性指数及均匀度指数偏低,群落结构单一,稳定性较差。春季由于受到深圳河与降水的影响,水采浮游植物丰度最低;秋季各个环境条件适宜,浮游植物丰度达到最大;冬季温度成为限制浮游植物生长的重要因子。 相似文献
44.
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We analyze a special kind of temporal fine structure in microwave radio emission for the 25 August 1999 solar flare observed
by the PMO spectrometer over the range of 4.5 – 7.5 GHz. This flare displays continuum emission after a group of reverse-slope
type III bursts around 6 GHz. High-resolution dynamic spectra reveal three evolving emission lines (EELs) following the type
III group. They are characterized by isolated, narrow, and continuous emission strips, which display frequency fluctuations
with time. Their frequency-drift rates are between −2 and 3 GHz s−1. Distinct from the EELs at lower frequencies, three EELs have a very short duration of a few seconds. They show an average
bandwidth of Δf≈330 MHz and a relative bandwidth of Δf/f≈0.057. This is the first time that this kind of fine structure has been observed around 6 GHz. 相似文献
46.
47.
The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) gives us a chance to investigate the theoretical Neupert effect using the correlation between the thermal-energy
derivative and the nonthermal energy, or the thermal energy and the integral nonthermal energy. Based on this concept, we
analyze four M-class RHESSI flares on 13 November 2003, 4 November 2004, 3 and 25 August 2005. According to the evolution
of the temperature [T], emission measure [EM], and thermal energy [E
th], each event is divided into three phases during the nonthermal-energy input [
\frac dEnthdt\frac {\mathrm{d}E_{\mathrm{nth}}}{\mathrm{d}t} in the units of erg s−1]. Phase 1 is identified as the interval before the temperature maximum, while after the thermal-energy maximum is phase 3,
between them is phase 2. We find that these four flares show the Neupert effect in phase 1, but not in phase 3. The Neupert
effect still works well in the second phase, although the cooling becomes slightly important. We define the parameter μ in the relation of
\fracdEthdt=m\fracdEnth(t)dt\frac{\mathrm {d}E_{\mathrm{th}}}{\mathrm{d}t}=\mu\frac{\mathrm{d}E_{\mathrm {nth}}(t)}{\mathrm{d}t} or
Eth(t0)=mò0t0\fracdEnth(t)dt dtE_{\mathrm{th}}(t_{0})=\mu\int_{0}^{t_{0}}\frac{\mathrm{d}E_{\mathrm{nth}}(t)}{\mathrm{d}t}\,\mathrm{d}t when the cooling is ignored in phase 1. Considering the uncertainties in estimating the energy from the observations, it
is not possible to precisely determine the fraction of the known energy in the nonthermal electrons transformed into the thermal
energy of the hottest plasma observed by RHESSI. After a rough estimate of the flare volume and the assumption of the filling
factor, we investigate the parameter μ in these four events. Its value ranges from 0.02 to 0.20, indicating that a small fraction (2% – 20%) of the nonthermal energy
can be efficiently transformed into thermal energy, which is traced by the soft X-ray emission, and the bulk of the energy
is lost possibly due to cooling. 相似文献
48.
Zongjun Ning 《Solar physics》2008,247(1):53-62
This paper explores the time evolution of microwave and hard X-ray spectral indexes in the solar flare observed by Nobeyama
Radio Polarimeters (NoRP) and the Ramaty High Energy Solar Spectroscopy Imager (RHESSI) on 13 December 2006. The microwave
spectral index, γ
MW, is derived from the emissions at two frequencies, 17 and 35 GHz, and hard X-ray spectral index, γ
HXR, is derived from RHESSI spectra. Fifteen subpeaks are detected at the microwave and hard X-ray emissions. The microwave spectral
indexes tend to be harder than hard X-ray spectral indexes during the flare, which is consistent with previous findings. All
detected subpeaks follow the soft-hard-soft spectral behaviours in the hard X-ray rise-peak-decay phases. However, the corresponding
microwave subpeaks display different spectral behaviour, such as soft-hard-soft, soft-hard-harder, soft-hard-soft + hard or
irregular patterns. These contradictions reveal the complicated acceleration mechanism for low- and high-energy electrons
during this event. It is also interesting that the microwave interpeak spectral indexes are much more consistent with one
another. 相似文献
49.
Zongjun Ning 《Astrophysics and Space Science》2008,314(1-3):137-143
We explore the correlations between the inferred reconnection rate and hard X-ray spectral hardness for two double-ribbon flares on 2003 November 1 and 2005 May 17 in this paper. The magnetic reconnection rate of φ rec is derived from the time rate of change of the product between the normal magnetic field and the newly brightened ribbon area of TRACE 1600 Å observations. And the spectral index of γ is derived from RHESSI hard X-ray data. Both events show a soft-hard-soft spectral behaviour in the rise-peak-decay phases. An anti-correlated behaviour is found between the time evolution of reconnection rate and spectral index. From the regression analysis, we obtain a negative power-law dependence and quantify the relationship between these two quantities. This is consistent with the simulation results before, and further confirms the importance of magnetic reconnection for the electron acceleration in solar flares. 相似文献
50.
胶州湾滨海湿地的景观格局变化及环境效应 总被引：3，自引：0，他引：3
在湿地景观类型分类基础上,利用RS及GIS技术提取了1986、1995和2010年胶州湾滨海湿地的Landsat卫星假彩色合成影像的空间属性数据,利用斑块动态度、斑块密度指数、景观多样性指数、斑块破碎化指数研究了胶州湾滨海湿地的景观格局变化及累积环境效应。结果表明,1986～2010年胶州湾滨海湿地总面积减少,河流与河口湿地面积稍有增大,潮间带滩涂和潮上带湿地面积和斑块数减小;养殖池面积增大、斑块数增多,盐田面积减小、斑块数基本未变,增加了湿地公园这种新的人工湿地景观类型。期间,湿地的景观斑块密度指数、多样性指数和景观斑块破碎化指数增大了。上述湿地面积和景观格局变化是由围垦、城市化、港口和道路建设、河流径流量和输沙量减少、海岸侵蚀、海水入侵、全球变暖、海面上升等因素引起的,并导致湿地生物多样化水平下降、有害植物入侵、环境净化功能降低、污染和赤潮灾害加重、植被退化演替、渔业资源衰退和湿地生态系统服务价值降低等累积环境效应。为减轻这些不利的累积环境效应,应采取建设湿地自然保护区、控制养殖池和盐田规模、发展工业循环经济和生态农业等措施保护胶州湾滨海湿地。 相似文献