Interpreting Helioseismic Structure Inversion Results of Solar Active Regions

Helioseismic techniques such as ring-diagram analysis have often been used to determine the subsurface structural differences between solar active and quiet regions. Results obtained by inverting the frequency differences between the regions are usually interpreted as the sound-speed differences between them. These in turn are used as a measure of temperature and magnetic-field strength differences between the two regions. In this paper we first show that the “sound-speed” difference obtained from inversions is actually a combination of sound-speed difference and a magnetic component. Hence, the inversion result is not directly related to the thermal structure. Next, using solar models that include magnetic fields, we develop a formulation to use the inversion results to infer the differences in the magnetic and thermal structures between active and quiet regions. We then apply our technique to existing structure inversion results for different pairs of active and quiet regions. We find that the effect of magnetic fields is strongest in a shallow region above 0.985R _⊙ and that the strengths of magnetic-field effects at the surface and in the deeper (r<0.98R _⊙) layers are inversely related (i.e., the stronger the surface magnetic field the smaller the magnetic effects in the deeper layers, and vice versa). We also find that the magnetic effects in the deeper layers are the strongest in the quiet regions, consistent with the fact that these are basically regions with weakest magnetic fields at the surface. Because the quiet regions were selected to precede or follow their companion active regions, the results could have implications about the evolution of magnetic fields under active regions.     

Stochastic heating of cooling flows

It is generally accepted that the heating of gas in clusters of galaxies by active galactic nuclei is a form of feedback. Feedback is required to ensure a long-term, sustainable balance between heating and cooling. This work investigates the impact of proportional stochastic feedback on the energy balance in the intracluster medium. Using a generalized analytical model for a cluster atmosphere, it is shown that an energy equilibrium can be reached exponentially quickly. Applying the tools of stochastic calculus, it is demonstrated that the result is robust with regard to the model parameters, even though they affect the amount of variability in the system.     

The INTEGRAL complete sample of type 1 AGN

In this paper we discuss the broad-band X-ray characteristics of a complete sample of 36 type 1 active galactic nuclei (AGN), detected by INTEGRAL in the 20–40 keV band above the 5.5σ level. We present, for all the objects in the sample, the broad-band (1–110 keV) spectral analysis obtained by using INTEGRAL / Swift /Burst Alert Telescope observations together with XMM–Newton , Chandra , ASCA and Swift /X-Ray Telescope data. We also present the general average properties of the sample, i.e. the distribution of photon indices, high-energy cut-offs, reflection fractions and absorption properties, together with an in-depth analysis of their parameter space. We find that the average Seyfert 1 power law has an index of 1.7 with a dispersion of 0.2. The mean cut-off energy is at around 100 keV, with most objects displaying E _c in the range 50–150 keV; the average amount of Compton reflection is 1.5 with a typical dispersion of 0.7. We do not find any convincing correlation between the various parameters, an indication that our analysis is not strongly dependent by the interplay between them. Finally, we investigate how the results presented in this work fit into current frameworks for AGN spectral modelling and cosmic diffuse X-ray background synthesis models.     

Brightness temperature for 166 radio sources

Using the database of the University of Michigan Radio Astronomy Observatory （UMRAO） at three radio frequencies （4.8, 8 and 14.5 GHz）, we determined the short-term variability timescales for 166 radio sources. The timescales are 0.15d （2007＋777） to 176.17 d （0528-250） with an average timescale of Atobs = 17.1 4- 16.5 d for the whole sample. The timescales are used to calculate the brightness temperatures, TB. The value of log TB is in the range of log TB = 10.47 to 19.06 K. In addition, we also estimated the boosting factor for the sources. The correlation between the polarization and the Doppler factor is also discussed.     

The X-ray jets of active galaxies

Jet physics is again flourishing as a result of Chandra’s ability to resolve high-energy emission from the radio-emitting structures of active galaxies and separate it from the X-ray-emitting thermal environments of the jets. These enhanced capabilities have coincided with an increasing interest in the link between the growth of super-massive black holes and galaxies, and an appreciation of the likely importance of jets in feedback processes. I review the progress that has been made using Chandra and XMM-Newton observations of jets and the medium in which they propagate, addressing several important questions, including: Are the radio structures in a state of minimum energy? Do powerful large-scale jets have fast spinal speeds? What keeps jets collimated? Where and how does particle acceleration occur? What is jet plasma made of? What does X-ray emission tell us about the dynamics and energetics of radio plasma/gas interactions? Is a jet’s fate determined by the central engine?     

The accuracy of supermassive black hole masses determined by the single-epoch spectrum (Dibai) method

The first set of supermassive black hole mass estimates, published from 1977 to 1984 by E.A. Dibai, are shown to be in excellent agreement with recent reverberation-mapping estimates. Comparison of the masses of 17 AGNs covering a mass range from about 10⁶ to 10⁹ M _⊙ shows that the Dibai mass estimates agree with reverberation-mapping mass estimates to significantly better than ±0.3 dex and were, on average, only 0.14 dex (∼40%) systematically lower than masses obtained from reverberation mapping. This surprising agreement with the results of over a quarter of a century ago has important implication for the structure and kinematics of AGNs and implies that type-1 AGNs are very similar. Our results give strong support to the use of the single-epoch-spectrum (Dibai) method for investigating the co-evolution of supermassive black holes and their host galaxies. The article was translated by the authors.     

Dew and rain water collection in the Dalmatian Coast, Croatia

Passive dew harvesting and rainwater collection requires a very small financial investment but can exploit a free, clean (outside urban/industrial zones) and inexhaustible source of water. This study investigates the relative contributions of dew and rain water in the Mediterranean Dalmatian coast and islands of Croatia, with emphasis on the dry summer season. In addition, we evaluate the utility of transforming abandoned roof rain collectors (“impluviums”) to collect dew water too. Two sites were chosen, an exposed open site on the coast favourable to dew formation (Zadar) and a less favourable site in a cirque of mountains in Komiža (Vis Island). Between July 1, 2003 and October 31, 2006, dew was collected two or three times per day on a 1 m² inclined (30°) test dew condenser, together with standard meteorological data (air temperature and relative humidity, cloud cover, windspeed and direction). Maximum yields were 0.41 mm in Zadar and 0.6 mm in Komiža. The mean yearly cumulative dew yields were found to be 20 mm (Zadar) and 9.3 mm (Komiža). Because of its physical setting, Komiža represents a poor location for dew collection. However, during the dry season (May to October), monthly cumulative dew water yield can represent up to 38% of water collected by rainfall. In both July 2003 and 2006, dew water represented about 120% of the monthly cumulative rain water. Refurbishing the abandoned impluviums to permit dew collection could then provide useful supplementary water, especially during the dry season. As an example, the 1300 m² impluvium at Podšpilje near Komiža could provide, in addition to rain water, 14,000 L dew water per year.     

中国东南部4～5月年代际干旱的南移特征及潜热影响的数值模拟

利用1958～2000年旬平均中国560站地面观测资料和ERA－40再分析资料, 分析了东亚气候在4～5月的年代际变化特征。发现发生在1970年代末的中国东南部干旱出现于4月中旬至5月中旬, 干旱带随季节推进逐渐向南移动。这种南移特征与对流层中上层年代际变冷中心的移动是一致的, 上层变冷中心所伴随的局地风场异常, 即异常下沉运动和对流层低层北风异常, 均显著存在于4月中旬至5月中旬, 且逐渐南移。中国东南部年代际干旱带在4~5月的南移从一定程度上意味着 4月黄淮流域降水异常对5月江南地区的降水多少具有一定的指示意义。由于干旱区位于上层变冷区的南侧, 意味着该地区向上输送的潜热通量减少能够使对流层大气进一步冷却, 这在一个变网格全球模式的敏感性试验中得到了验证, 能够部分地解释大气中的冷信号为何持续存在和南移。     

利用一个海气耦合模式对台风Krovanh的模拟

采用中尺度大气模式MM5和区域海洋模式POM构造了中尺度海气耦合模式, 模拟了Krovanh (0312) 台风过程中台风－海洋相互作用, 分析了台风引起的海面降温影响台风强度的机制和海洋对台风响应的特征。试验结果显示: 考虑台风引起的海面降温使台风强度模拟有了较大改进, 模拟的台风中心气压和近中心最大风速均与实况较符合。POM模拟的海表面温度与TRMM/TMI观测的海表面温度也较为一致, 台风Krovanh在其路径右侧95 km处引起较大的海面降温, 最大降温幅度达5.8℃。与海表面温度降低相对应的是混合层深度的增加, 较大的海面降温对应较大的混合层加深, 表明大风夹卷在海表面温度的降低中起主要作用。分析表明, 台风引起的海面降温降低海洋向大气输送的潜热通量和感热通量, 特别是在台风内核区, 平均总热通量减少了32.1%。热通量的减少使得湿静力能及湿静力能径向梯度减小, 削弱了台风强度。     

U型块石路基结构对多年冻土的降温作用

通过对比北麓河试验段U型块石路基结构和普通路基下部土体温度监测研究,U型块石路基显著地抬升路基下部多年冻土上限,具有较强的降低多年冻土温度的作用.2005—2007年间,U型块石路基下多年冻土上限平均抬升幅度达0.9~1.4 m.路基中心下部0.5 m深土体温度降温幅度达1.13℃,原天然上限附近土体温度降温达1.28℃,5 m深的多年冻土降温幅度达0.77℃,且U型块石路基下部土体温度呈现逐年降低的趋势.然而,普通路基下部土体温度远比U型块石路基下部要高,2005年普通路基下部0.5 m深土体年平均温度比U型块石路基高1~3℃,1.5 m处高0.8~1.9℃,5 m处高1.2~1.5℃.同时,U型块石路基下部多年冻土上限抬升比普通路基大,2004—2006年间U型块石路基左路肩下多年冻土上限抬升比普通路基大0.86 m,路基中心大0.5 m.