Magnetic field, helicity and the 2000 July 14 flare in solar active region 9077

In this paper we analyse the non-potential magnetic field and the relationship with current (helicity) in the active region NOAA 9077 in 2000 July, using photospheric vector magnetograms obtained at different solar observatories and also coronal extreme-ultraviolet 171-Å images from the TRACE satellite.
We note that the shear and squeeze of magnetic field are two important indices for some flare-producing regions and can be confirmed by a sequence of photospheric vector magnetograms and EUV 171-Å features in the solar active region NOAA 9077. Evidence on the release of magnetic field near the photospheric magnetic neutral line is provided by the change of magnetic shear, electric current and current helicity in the lower solar atmosphere. It is found that the 'Bastille Day' 3B/5.7X flare on 2000 July 14 was triggered by the interaction of the different magnetic loop systems, which is relevant to the ejection of helical magnetic field from the lower solar atmosphere. The eruption of the large-scale coronal magnetic field occurs later than the decay of the highly sheared photospheric magnetic field and also current in the active region.     

The evolution and efficiency of energy release of magnetized black-hole accretion disks

On the basis of the equivalent circuit model, we investigate two different mechanisms of extracting energy of rotation and angular momentum from a black hole by magnetic field, namely, the Blandford-Znajek (BZ) process and the magnetic coupling (MC) process. The contributions to the efficiency of energy release via pure accretion process, BZ process and MC process are compared in detail by studying the evolutionary characteristics of the spin parameter of the black hole at the center of the magnetized accretion disk. It is shown that the MC process is an important new mechanism of extracting energy from the rotating black hole and its efficiency of energy release is almost as high as that of the BZ process. The efficiency of energy release via pure accretion process is higher than those of BZ process and magnetic coupling process. However, when the rotation of a black hole approaches that of an extreme Kerr black hole,the efficiency of energy release is mainly due to the contributions of BZ process and MC process.     

山东省区域地球物理场

山东省各岩石磁性及密度参数基本可分为高、中、低3类.山东省磁性结晶基底为泰山岩群、荆山群、胶东岩群、胶南岩群.以沂沭断裂带为界,山东省区域地球物理场分为鲁东区和鲁西区.鲁东区进一步划分为3个次级区,即北部区、中部区和南部区.鲁西区进一步划分为5个次级区,即鲁北重磁缓变区、鲁西南重高磁高区、中部弧形重磁场区、鲁西中部重低磁高区、鲁中南条带状重磁场区.各区地球物理场由于地质原因各具特点.山东省莫氏面总体呈东浅西深的缓变带,在该缓变带的背景上,呈周边地区条带状幔隆、中部幔坳的特征.山东省居里面呈近南北向带状分布,有德州聊城菏泽隆起带、滨州淄博滕州深坳带、蓬莱海阳千里岩响水隆起带.鲁中隆起北部碰撞带为山东省特殊的构造地带,其特征为侵入岩体沿该带断续出现、岩体围岩或岩体内铜及多金属矿化较为普遍、地热田沿该带时有分布、地形上为南部山区和北部平原的分界地带.胶莱盆地内,蓼兰-高密缺失莱阳群层位;中生代早期,盆地东北部与西南部是盆地的沉积中心,至晚期盆地中心北移,第三纪沉积中心则为平度蓼兰附近;盆地较深部位位于诸城凹陷、平度凹陷.胶莱盆地的次级构造单元可划分为11个,七级镇构造带控制了胶莱盆地的成生和发展.山东省岩浆岩通常表现为强磁性、低密度,但基性程度高的岩体磁性高、密度亦高,酸性程度高的岩体磁性低、密度低.     

Basal heating in the atmospheres of cool stars

Summary This paper reviews observational evidence concerning the existence of so-calledbasal heating that occurs in the outer atmospheres of all stars with convective envelopes. Effects of basal heating depend primarily on the effective temperature, with little sensitivity to surface gravity or elemental abundances. Basal heating occurs predominantly in the chromosphere, possibly in the (lower) transition region, but not at an observable level in coronae (except perhaps in early F-type and in M-type dwarf stars). Basal fluxes are observed in the slowest rotators where it shows no significant modulation. The basal flux level is observed directly on the Sun only over regions void of intrinsically strong photospheric fields. There is substantial quantitative observational and theoretical evidence that the basal emission from stellar outer atmospheres is caused by the dissipation of acoustic waves generated by turbulent convection. The magnetic canopy turns out to be of little consequence, but effects of intrinsically weak fields on the basal mechanism cannot be entirely ruled out. Solar observations constrain the spatio-temporal character of the basal atmosphere and the acoustic flux levels as a function of height, resulting in a model in which intermittent wave dissipation causes emission characteristic of both cool and warm atmospheric areas, in which — at least in the solar case — a time-averaged chromospheric temperature rise may not even exist.     

The polarization-free approximation

The development of effective iterative methods capable of accurately solving NLTE Stokes transfer problems is of considerable importance for the investigation of solar and stellar magnetic fields. After briefly indicating the iterative approach which is being presently pursued for the exact solution of such problems, the particular regime where polarization signals can only be due to the Zeeman effect is considered in some detail. By means of NLTE Stokes transfer calculations for a two-level atomic model it is first shown that the currently-used field-free approximation (Rees, 1969) cannot be safely applied in the presence of magnetic field gradients. Such gradients lead to changes in the shape and width of the line profiles and they can produce non-negligible effects on the atomic level populations and line source functions. A new approximate method is then proposed, which does not require the actual solution of the Stokes vector transfer equation and is practically as fast as the field-free one. This polarization-free approximation provides a fairly good account of the effects of homogeneous and inhomogeneous magnetic fields on the statistical equilibrium and is very easy to implement in any existing non-magnetic, multi-level transfer code.On leave from the Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Largo E. Fermi 5, I-50125 Firenze, Italia     

The evolution of the core and surface magnetic fields in isolated neutron stars

We apply the model of flux expulsion from the superfluid and superconductive core of a neutron star, developed by Konenkov & Geppert, both to neutron star models based on different equations of state and to different initial magnetic field structures. Initially, when the core and the surface magnetic field are of the same order of magnitude, the rate of flux expulsion from the core is almost independent of the equation of state, and the evolution of the surface field decouples from the core field evolution with increasing stiffness. When the surface field is initially much stronger than the core field, the magnetic and rotational evolution resembles that of a neutron star with a purely crustal field configuration; the only difference is the occurrence of a residual field. In the case of an initially submerged field, significant differences from the standard evolution only occur during the early period of the life of a neutron star, until the field has been re-diffused to the surface. The reminder of the episode of submergence is a correlation of the residual field strength with the submergence depth of the initial field. We discuss the effect of the re-diffusion of the magnetic field on the difference between the real and the active age of young pulsars and on their braking indices. Finally, we estimate the shear stresses built up by the moving fluxoids at the crust–core interface and show that these stresses may cause crust cracking, preferentially in neutron stars with a soft equation of state.     

Accretion disc coronae as magnetic reservoirs

Most astrophysical sources powered by accretion on to a black hole, either of stellar mass or supermassive, when observed with hard X-rays show signs of a hot Comptonizing component in the flow, the so-called corona , with observed temperatures and optical depths lying in a narrow range (0.1≲ τ ≲1 and 1×10⁹ K≲ T ≲3×10⁹ K). Here we argue that these facts constitute strong supporting evidence for a magnetically dominated corona. We show that the inferred thermal energy content of the corona, in all black hole systems, is far too low to explain their observed hard X-ray luminosities, unless either the size of the corona is at least of the order of 10³ Schwarzschild radii, or the corona itself is in fact a reservoir , where the energy is mainly stored in the form of a magnetic field generated by a sheared rotator (probably the accretion disc). We briefly outline the main reasons why the former possibility is to be discarded, and the latter preferred.     

南海北部渔场表层沉积物中的硫化物

为了给南海北部渔场的资源和环境保护提供基础数据,用碘量法测定了南海北部陆架区表层沉积物中硫化物含量.结果表明,全部28份样品中硫化物含量为3.3～42.2mg/kg(干重,下同),平均为12.1mg/kg,符合外海含量低的一般规律,明显低于沿岸海湾的含量,远低于日本渔业环境质量标准(200mg/kg)和安全下限值(400mg/kg).硫化物含量在测站间和不同区域间存在一定差异,南北方向呈近岸(13.1mg/kg)略高于离岸(12.1mg/kg)、离岸略高于远岸(11.1mg/kg)的梯度分布,但梯度差异不显著(p＞0.10);东西方向的分布特点是粤西海域(23.7mg/kg)＞海南岛以东(15.3mg/kg)＞台湾浅滩(9.4mg/kg)≈粤东海域(8.7mg/kg)≈珠江口外海域(8.6mg/kg).空间分布不太均匀主要是受沉积物类型的影响,与陆源硫化物输入的关系不大.