Microwave emission from a sunspot     

Jeongwoo W. Lee  G. J. Hurford  Dale E. Gary 《Solar physics》1993,144(1):45-57

From the gyroresonance brightness temperature spectrum of a sunspot, one can determine the magnetic field strength by using the property that microwave brightness is limited above a frequency given by an integer-multiple of the gyrofrequency. In this paper, we use this idea to find the radial distribution of magnetic field at the coronal base of a sunspot in the active region, NOAA 4741. The gyroresonance brightness temperature spectra of this sunspot are obtained from multi-frequency interferometric observations made at the Owens Valley Radio Observatory at 24 frequencies in the range of 4.0–12.4 GHz with spatial resolution 2.2″–6.8″. The main results of present study are summarized as follows: first, by comparison of the coronal magnetic flux deduced from our microwave observation with the photospheric magnetic flux measured by KPNO magnetograms, we show that theo-mode emission must arise predominantly from the second harmonic of the gyrofrequency, while thex-mode arises from the third harmonic. Second, the radial distribution of magnetic fieldsB(r) at the coronal base of this spot (say, 2000–4000 km above the photosphere) can be adequately fitted by $$B(r) = 1420(1 \pm 0.080)\exp \left[ { - \left( {\frac{r}{{11.05''(1 \pm 0.014)}}} \right)^2 } \right]G,$$ wherer is the radial distance from the spot center at coronal base. Third, it is found that coronal magnetic fields originate mostly from the photospheric umbral region. Fourth, although the derived vertical variation of magnetic fields can be approximated roughly by a dipole model with dipole moment 1.6 × 10³⁰ erg G^?1 buried at 11000 km below the photosphere, the radial field distribution at coronal heights is found to be more confined than predicted by the dipole model.  相似文献   

Multi-method radiometric dating of volcano-sedimentary layers from northern Italy: Age and duration of the Priabonian stage     

G.S. Odin  V. Barbin  A.J. Hurford  H. Baadsgaard  B. Galbrun  P.-Y. Gillot 《Earth and Planetary Science Letters》1991,106(1-4)

A comparison between conventional KAr (biotite) ages and fission track (zircon and apatite) and UPb (zircon) ages obtained from stratigraphically well-constrained Priabonian (Late Eocene) volcano-sedimentary deposits of northern Italy is presented. Two sections at Priabona (one level) and Possagno (two levels) were dated. The application of fission track dating appears fruitful for obtaining reasonably precise (±4 to 5% 2σ errors) ages useful for time-scale calibration. The concordancy of apatite and zircon fission track ages, and the reproducibility of results provide the time of volcanic eruption and deposition. The UPb analysis of the zircons has not been unsuccessful, but discordancy does not permit accurate dating. Significant dates obtained from Possagno are: KAr method, 35.0 ± 0.5 Ma (duplicate analysis on K-rich biotite from the same level); fission track dating method, 35.8 ± 1.4 Ma (weighted mean age on 2 apatite and 3 zircon separates from the same level); UPb method, 36.7 ± 1.0 Ma (maximum age of discordant zircons from the same level). The comparison between the present results and recent multi-method and multi-laboratory results obtained from time equivalent Priabonian (Late Eocene) biotite-rich layers from the Apennines shows perfect agreement and supports the location of a Priabonian stage between about 37.5 Ma and about 33.7 (±0.5) Ma; the alternative ages preferred by the Decade of North American Geology convention should be abandoned and a large portion of this scale revised accordingly.  相似文献   

新一代天气雷达在泥石流灾害中的应用探讨     

陶云  唐川 《云南地理环境研究》2007,19(3):26-30,65

天气雷达的发展大致经历了4个阶段，其主要用于监测强对流天气、定量估计降水，是气象部门的重要探测和监测手段之一。新一代天气雷达观测的实时回波强度（Z）、径向风速（V）、速度谱宽（W）的回波图像中，提供了丰富的有关强对流天气的信息，综合使用Z、V、W的图像分析，有利于较准确和及时地监测灾害性天气。云南滑坡泥石流灾害高发区与云南暴雨中心有很好的对应关系，云南滑坡泥石流灾害空间分布与暴雨空间分布的空间相关系数为0．19，通过了0．05的显著性水平检验，也进一步说明云南暴雨在滑坡泥石流灾害发生中起着重要作用。以2004年7月5日德宏州特大山洪泥石流灾害为例子，探讨了新一代天气雷达在泥石流灾害的临阵预警中的应用。  相似文献   

Hard X-ray Microflares down to 3 keV     

Krucker  Säm  Christe  Steven  Lin  R.P.  Hurford  Gordon J.  Schwartz  Richard A. 《Solar physics》2002,210(1-2):445-456

The excellent sensitivity, spectral and spatial resolution, and energy coverage down to 3 keV provided by the Reuven Ramaty High-Energy Solar Spectroscopic Imager mission (RHESSI) allows for the first time the detailed study of the locations and the spectra of solar microflares down to 3 keV. During a one-hour quiet interval (GOES soft X-ray level around B6) on 2 May, 1:40–2:40 UT, at least 7 microflares occurred with the largest peaking at A6 GOES level. The microflares are found to come from 4 different active regions including one behind the west limb. At 7′′ resolution, some events show elongated sources, while others are unresolved point sources. In the impulsive phase of the microflares, the spectra can generally be fitted better with a thermal model plus power law above ∼ 6–7 keV than with a thermal only. The decay phase sometimes can be fitted with a thermal only, but in some events, power-law emission is detected late in the event indicating particle acceleration after the thermal peak of the event. The behind-the-limb microflare shows thermal emissions only, suggesting that the non-thermal power law emission originates lower, in footpoints that are occulted. The power-law fits extend to below 7 keV with exponents between −5 and −8, and imply a total non-thermal electron energy content between 10²⁶–10²⁷ erg. Except for the fact that the power-law indices are steeper than what is generally found in regular flares, the investigated microflares show characteristics similar to large flares. Since the total energy in non-thermal electrons is very sensitive to the value of the power law and the energy cutoff, these observations will give us better estimates of the total energy input into the corona. (Note that color versions of figures are on the accompanying CD-ROM.) Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1022404512780  相似文献   

The secondary spectral component of solar microwave bursts     

M. Stähli  D. E. Gary  G. J. Hurford 《Solar physics》1990,125(2):343-357

Microwave observations in the range 1 to 18 GHz with high spectral resolution (40 frequencies) have shown that many events display a complex microwave spectrum. From a set of 14 events with two or more spectral components, we find that two different classes of complex events can be distinguished. The first group (4 events) is characterized by a different temporal evolution of the spectral components, resulting in a change of the spectral shape. These events probably can be explained by gyrosynchrotron emission from two or more individual sources. The second class (10 events) has a constant spectral shape, so that the two spectral components vary together in intensity. For all ten events in this second class, the ratio of primary to secondary peak frequencies is remarkably similar, exhibiting an average value of 3.4, and both components show a common circular polarization. These properties suggest either a common source for the different spectral components or several sources which are closely coupled. An additional example of this class of burst was observed interferometrically to provide spatial resolution. This event suggests that the primary and secondary components have a similar location, but that the surface area of the secondary component is larger.Swiss National Science Foundation Fellow from the University of Bern.  相似文献   

戈壁风沙流结构特性及其意义     

屈建军  黄宁  拓万全  雷加强  董治宝  刘贤万  薛娴  俎瑞平  张克存 《地球科学进展》2005,20(1):19-023

通过砾质戈壁风沙流野外实测数据的分析以及风洞模拟实验研究发现：戈壁风沙流结构具有与沙漠风沙流完全不同的风沙流特征,戈壁风沙地表的粗糙度随风速的增大而增加,其表面风沙流输沙量高度分布表现出独特的"象鼻"效应,在一定高度处呈现最大值,并随风速的增加而增高。该"象鼻"效应导致戈壁风沙流结构特征值λ远大于 1,不论风速多大,风沙流都处于未饱和状态的非堆积搬运状态。这种特殊性质比较清楚地解释了敦煌莫高窟千年来不被沙山埋没的谜底。并且在风沙防治工程实践中,采用砾石压沙措施,构造类似与砾质戈壁的下垫面,人工促使风沙流结构呈现"象鼻"形状,可使防沙工程达到理想的输导作用。  相似文献   

The influence of obliquity on europan cycloid formation     

T.A. Hurford  A.R. Sarid  B.G. Bills 《Icarus》2009,202(1):197-215

Tectonic patterns on Europa are influenced by tidal stress. An important well-recognized component is associated with the orbital eccentricity, which produces a diurnally varying stress as Jupiter's apparent position in Europa's sky oscillates in longitude. Cycloidal lineaments seem to have formed as cracks propagated in this diurnally varying stress field. Maps of theoretical cycloid patterns capture many of the characteristics of the observed distribution on Europa. However, a few details of the observed cycloid distribution have not been reproduced by previous models. Recently, it has been shown that Europa has a finite forced obliquity, so Jupiter's apparent position in Europa's sky will also oscillate in latitude. We explore this new type of diurnal effect on cycloid formation. We find that stress from obliquity may be the key to explaining several characteristics of observed cycloids such as the shape of equator-crossing cycloids and the shift in the crack patterns in the Argadnel Regio region. All of these improvements of the fit between observation and theory seem to require Jupiter crossing Europa's equatorial plane 45° to 180° after perijove passage, suggestive of complex orbital dynamics that locks the direction of Europa's pericenter with the direction of the ascending node at the time these cycloids were formed.  相似文献   

Geological implications of a physical libration on Enceladus     

T.A. Hurford  B.G. Bills  P. Helfenstein  G.V. Hoppa 《Icarus》2009,203(2):541-552

  相似文献   

四川省盐源县盐泉的特征与形成     

李娜  周训  郭娟  拓明明  徐艳秋 《现代地质》2020,34(1):177-188

研究天然盐泉的形成有助于揭示陆地水文循环过程中的物质迁移。采用水文地球化学的方法,分析四川省盐源县的9个泉水和卤水水样的水化学特征和同位素特征,探讨盐泉的溶质来源,总结盐泉的成因模式。水样可以分为TDS为311.69 g/L的Cl-Na型卤水、TDS为55.77~89.43 g/L的Cl-Na型盐泉、TDS为1.17 g/L的Cl-Na型微咸泉和TDS为0.26~0.56 g/L的以HCO₃-Ca、HCO₃·SO₄-Ca·Mg型为主的淡水泉。泉水和卤水的氢氧同位素显示其来源于大气降水;水样的特征系数显示盐泉和卤水都属于溶滤型,且指示研究区基本不具有找钾前景。泉水的盐分主要来源于石盐、方解石、石膏和白云石等矿物的溶滤。盐泉的形成模式可以概括为:在山区获得大气降水入渗补给后,地下水经历较浅和较深的地下径流并且溶滤含盐地层或者盐矿,使其矿化度升高,在地形较低处汇集出露地表成泉。  相似文献   

Seasonal and sub-seasonal oxygen and nutrient fluctuations in an embayment of an eastern boundary upwelling system: St Helena Bay     

GC Pitcher  TA Probyn 《African Journal of Marine Science》2017,39(1):95-110

Seasonal, sub-seasonal and spatial fluctuations in bottom dissolved oxygen (DO) were examined in St Helena Bay, South Africa’s largest and most productive embayment, between November 2013 and November 2014. Alongshore bay characteristics were assessed through comparison of variables along the 50-m depth contour. A mean coefficient of variation of 0.35 provided a measure of the relative variability of near-bottom DO concentrations along this contour. Consistently lower DO concentrations in the southern region of the bay in summer and autumn are attributed to enhanced retention. Across-shelf transects captured the seasonal development of hypoxia in relation to the distribution of phytoplankton biomass. Exceptional dinoflagellate blooms form extensive subsurface thin layers preceding the autumn DO minima in the south of the bay, prior to winter ventilation of the bottom waters. The seasonal decline in DO concentrations in the bottom waters was marked by sub-seasonal events of hypoxia, and ultimately anoxia linked to episodic deposition of organic matter, as indicated by increases in bottom chlorophyll-a concentrations. Seasonal changes in bottom water macronutrient concentrations followed trends in apparent oxygen utilisation (AOU), both of which mirrored DO concentrations. In the south of the bay, nitrogen loss through denitrification/anammox in suboxic waters was indicated by a dissolved inorganic N deficit in the bottom waters, which was most pronounced in autumn.  相似文献