A New Method of Identifying 3D Null Points in Solar Vector Magnetic Fields   总被引：7，自引：0，他引：7  

Hui Zhao  Jing-Xiu Wang  Jun Zhang  Chi-Jie Xiao National Astronomical Observatories  Chinese Academy of Sciences  Beijing 《中国天文和天体物理学报》2005,5(5):443-447

Employing the Poincare index of isolated null-points in a vector field, we worked out a mathematical method of searching for 3D null-points in coronal magnetic fields. After introducing the relevant differential topology, we test the method by using the analytical model of Brown & Priest. The location of null-point identified by our method coincides precisely with the analytical solution. Finally we apply the method to the 3D coronal magnetic fields reconstructed from an observed MDI magnetogram of a super-active region (NOAA 10488). We find that the 3D null-point seems to be a key element in the magnetic topology associated with flare occurrence.  相似文献   

A possible origin of magnetic fields in galaxies and clusters: strong magnetic fields at  z∼ 10 ?     

Yutaka Fujita †  Tsunehiko N. Kato 《Monthly notices of the Royal Astronomical Society》2005,364(1):247-252

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A rigidly rotating magnetosphere model for circumstellar emission from magnetic OB stars     

R. H. D. Townsend  S. P. Owocki 《Monthly notices of the Royal Astronomical Society》2005,357(1):251-264

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A non-adiabatic analysis for axisymmetric pulsations of magnetic stars     

Hideyuki Saio 《Monthly notices of the Royal Astronomical Society》2005,360(3):1022-1032

This paper presents the results of a non-adiabatic analysis for axisymmetric non-radial pulsations including the effect of a dipole magnetic field. Convection is assumed to be suppressed in the stellar envelope, and the diffusion approximation is used to radiative transport. As in a previous adiabatic analysis, the eigenfunctions are expanded in a series of spherical harmonics. The analysis is applied to a  1.9-M_⊙  , main-sequence model  (log  T _eff= 3.913)  . The presence of a magnetic field always stabilizes low-order acoustic modes. All the low-order modes of the model that are excited by the κ-mechanism in the He  ii ionization zone in the absence of a magnetic field are found to be stabilized if the polar strength of the dipole magnetic field is larger than about 1 kG. For high-order p modes, on the other hand, distorted dipole and quadrupole modes excited by the κ-mechanism in the H ionization zone remain overstable, even in the presence of a strong magnetic field. It is found, however, that all the distorted radial high-order modes are stabilized by the effect of the magnetic field. Thus, our non-adiabatic analysis suggests that distorted dipole modes and distorted quadrupole modes are most likely excited in rapidly oscillating Ap stars. The latitudinal amplitude dependence is found to be in reasonable agreement with the observationally determined one for HR 3831. Finally, the expected amplitude of magnetic perturbations at the surface is found to be very small.  相似文献   

中尺度磁绳结构的行星际观测     

宋其武  吴德金 《天文学报》2004,45(4):381-388

由磁绳结构主导、平均尺度约二、三十个小时的行星际磁云是日冕物质抛射在行星际膨胀、传播的体现。最近，Moldwin等人报道在太阳风中还观测到一些尺度在几十分钟的小尺度磁绳结构，并认为太阳风中的磁绳结构在尺度分布上可能具有双峰特征，在全面检视了WIND卫星(1995年-2000年)和ACE卫星(1998年-2000年)的观测资料后，发现了在行星际太阳风中一些尺度为几个小时的中尺度磁绳结构，利用初步整理的其中28个中尺度磁绳结构事件，认为太阳风中的磁绳结构在尺度分布上可能是连续的，这对行星际太阳风中磁绳结构物理起源的研究可能提出重要的物理限制。  相似文献   

Can late-type active stars be explained by a dipole magnetic trap?     

B.J. Kellett  R. Bingham  R.A. Cairns  V. Tsikoudi 《Monthly notices of the Royal Astronomical Society》2002,329(1):102-108

In this paper we review four different types of X-ray and/or radio observations of active late-type stars. We then consider if a single magnetic source configuration – a toroidal dipole magnetic trap – can possibly explain these various different observations. We conclude that, indeed, dipole magnetic confinement (similar to the magnetic configurations of the Earth's radiation belts and the case of Jupiter and the Io torus) can explain all the diverse observational data. We take this to be very strong observational support for this type of magnetic confinement scheme. We also consider that this magnetic configuration is only likely to be established and maintained in the most active stars.  相似文献   

Milestones in the Observations of Cosmic Magnetic Fields     

Jin－LinHan RichardWielebinski 《中国天文和天体物理学报》2002,2(4):293-294

Magnetic fields are observed everywhere in the universe. In this review, we concentrate on the observational aspects of the magnetic fields of Galactic and extragalactic objects. Readers can follow the milestones in the observations of cosmic magnetic fields obtained from the most important tracers of magnetic fields, namely, the star-light polarization, the Zeeman effect, the rotation measures (RMs, hereafter) of extragalactic radio sources, the pulsar RMs, radio polarization observations, as well as the newly implemented sub-mm and mm polarization capabilities. The magnetic field of the Galaxy was first discovered in 1949 by optical polarization observations. The local magnetic fields within one or two kpc have been well delineated by starlight polarization data. The polarization observations of diffuse Galactic radio background emission in 1962 confirmed unequivocally the existence of a Galactic magnetic field. The bulk of the present information about the magnetic fields in the Galaxy comes from anal  相似文献   

太阳光球磁通量南北不对称性研究     

宋文彬  汪景琇  马霞 《天文学报》2005,46(1):19-26

运用统计方法系统研究了1978-2002年太阳光球磁通量南北不对称性变化特征，发现其与太阳活动周有关．不对称值在太阳活动极小年要明显高于太阳活动极大年，并且磁通量变化总是由上升段的北半球占优逐渐过渡到下降段的南半球占优．另外运用小波变换方法详细讨论了这种不对称性变化可能存在的周期信息．  相似文献   

冕洞观测研究的近期进展     

堵锦生 《天文学进展》1997,15(2):112-119

简要介绍了在１９８８－１９９５年期间冕洞观测研究的主要进展。文中共分五个方面：１．冕洞磁场观测研究的新进展；２．冕洞在太阳活动周不同位相时的规律性；３．冕洞区高速太阳风观测的新结果；４．冕洞加热问题；５．存在问题。  相似文献   

ON THE ORIGIN AGE OF THE SOUTHWEST BASIN IN THE SOUTH CHINA SEA     

刘昭蜀  闫贫  刘海龄 《中国海洋湖沼学报》1997,15(3):285-288

TheSouthChinaSea(SCS)islocatalinthejunCti0noftheEurasian,PacificandIndodeustralianPlates,andisoneofthebiggestrnarginalseasinthewesternPadfic~n.Uyeda(l977)regardedtheSCS'soriginasoneofthebasicprobboincompletelyre-solvedbytheTheoryofPlateTeCtoniesrv).Heaskedfl.Whydoesanarcriseup(theoriginofarcmountains)?2.Whyisthestressinthebackurcbasinregionextensional(theoriginofbackurcbasin)?3.Whyisthernantleintheinnerurcbelthot(theoriginofvohanismandhighgcothermalflow)?Therewermanyviewnointsontheori…  相似文献