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  • 1
    Electronic Resource
    Electronic Resource
    The mean evershed flow
    Amsterdam : Elsevier
    Chinese Astronomy and Astrophysics 8 (1984), S. 194-200 
    Details
    ISSN: 0275-1062
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0275-1062(84)90022-5
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  • 2
    Electronic Resource
    Electronic Resource
    The Helmholtz instability of magnetic flux sheets - AApS 11/4 (1991) 378-382
    Amsterdam : Elsevier
    Chinese Astronomy and Astrophysics 16 (1992), S. 111 
    Details
    ISSN: 0275-1062
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0275-1062(92)90020-C
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  • 3
    Electronic Resource
    Electronic Resource
    The dynamical process of a coronal transient associated with an eruptive prominence (1983)
    Springer
    Astrophysics and space science 92 (1983), S. 395-415 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Based on the Paper I (Hu, 1983a), the piston model suggested for the coronal transient. The piston may consist of the eruptive prominence and the preceding compressed magnetic field region, and the moving piston is considered to be the driving source of the coronal transient. There is the compressed flow region ahead the piston and the rarefaction region behind the piston. In this paper, two analytical solutions are discussed in finite regions of piston model. A consistent solution of the ideal magnetohydrodynamical equations including the gravity is obtained for the two-dimensional unsteady configuration in which density and magnetic field are time dependent. Gravity, Lorentz and inertial forces are balanced by the pressure gradient. The analysis gives a consistent radial velocityu(t) which agrees with the typical velocity of eruptive prominence. The density profile is proportional to 1/r and propagates outward with the velocityu. This solution may be applied to the piston region of moving plasma and magnetic field. Furthermore, the compressed flow driven by the piston is discussed. The consistent solution of gasdynamical equations including solar gravity is obtained for the unsteady and two-dimensional configuration, which is applied to the region between the piston and shock wave. This solution may satisfy the jump conditions of shock wave, which separates the region of compressed flow and quiet corona.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651303
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  • 4
    Electronic Resource
    Electronic Resource
    The non-axisymmetrical configuration of a large-scale solar and stellar magnetic field (1983)
    Springer
    Astrophysics and space science 90 (1983), S. 391-403 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The non-axisymmetric and nonlinear solutions of the magnetostatic equations are given in three-dimensional space of spherical coordinates (r, θ, ϕ). These solutions are applied to the large-scale solar magnetic field. Their basic features are similar to a dipole field near the polar regions and the polarity reverses near the equator. These features agree with observations for the large-scale solar magnetic field. The solutions can also be applied to investigating the connection between the structure of the magnetic field and the density distribution of the corona. It is shown that the tops of the closed magnetic field associate with density enhancements. Similar results may apply to the large-scale configuration of the stellar field.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00650071
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  • 5
    Electronic Resource
    Electronic Resource
    The influence of fluctuation fields on the force-free field (1983)
    Springer
    Astrophysics and space science 97 (1983), S. 353-367 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In Paper I (Hu, 1982), we discussed the the influence of fluctuation fields on the force-free field for the case of conventional turbulence and demonstrated the general relationships. In the present paper, by using the approach of local expansion, the equation of average force-free field is obtained as (1+b)∇×B 0=(α#x002B;a)B 0#x002B;a (1)×B 0#x002B;K. The average coefficientsa,a (1),b, andK show the influence of the fluctuation fields in small scale on the configurations of magnetic field in large scale. As the average magnetic field is no longer parallel to the average electric current, the average configurations of force-free fields are more general and complex than the usual ones. From the view point of physics, the energy and momentum of the turbulent structures should have influence on the equilibrium of the average fields. Several examples are discussed, and they show the basic features of the fluctuation fields and the influence of fluctuation fields on the average configurations of magnetic fields. The astrophysical environments are often in the turbulent state, the results of the present paper may be applied to the turbulent plasma where the magnetic field is strong.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653491
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  • 6
    Electronic Resource
    Electronic Resource
    The influence of momentum addition on the acceleration of the solar and stellar winds (1984)
    Springer
    Astrophysics and space science 98 (1984), S. 171-189 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The influence of the momentum addition, which may be associated with the average or fluctuation transverse component of the magnetic field or others, on the acceleration the solar wind or stellar wind is studied in a local streamtube. The results show that the larger the momentum addition the stronger the acceleration of the wind. For example, if the typical transverse magnetic field is about 0.1 of the longitudinal field, the velocity of the solar wind at 1 AU may be increased by 40%. The coronal hole may be considered as a streamtube, the presence of a high stream from the coronal hole may be explained by the existence of an average or fluctuation transverse magnetic field in the streamtube. A similar conclusion may be applied to the polar region, where the velocity of the solar wind will be larger than elsewhere as if there is a transverse component of magnetic field, as well as to the stellar wind. The influence of other parameters on the acceleration of the solar wind is also discussed. From the viewpoint of the solar wind mechanism, the present paper shows that the momentum addition in the subsonic flow region can increase the velocity of the solar wind at 1 AU.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651957
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  • 7
    Electronic Resource
    Electronic Resource
    Influence of fluctuating field on the configuration of force-free field (1982)
    Springer
    Astrophysics and space science 85 (1982), S. 351-360 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The consistent equations for random force-free magnetic fields are obtained from the fluctuation and average equations of both momentum and induction ones based on the statistical approach. Some features of average force-free fields are discussed. This idea may be applied to explain many configurations of magnetic field in the astronomical environment.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653457
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  • 8
    Electronic Resource
    Electronic Resource
    Three-dimensional distribution of interstellar gas in disk-shaped galaxies
    Amsterdam : Elsevier
    Chinese Astronomy 1 (1977), S. 51-62 
    Details
    ISSN: 0146-6364
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0146-6364(77)90022-6
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  • 9
    Electronic Resource
    Electronic Resource
    Asymmetric structure of an isolated flux arch (1993)
    Springer
    Astrophysics and space science 208 (1993), S. 253-260 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract This paper extends two-dimensional model of symmetric magnetostatic flux arches confined in stratified atmospheres (Zhang and Hu, 1992, 1993) to asymmetric models. Numerical results show that the flux structure is influenced greatly by the boundary condition of magnetic field, the force-free factor, the atmospheric pressure distribution and the position of footpoints (especially the width ratio of outlet to entrance, which differs from symmetric case).
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00657940
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  • 10
    Electronic Resource
    Electronic Resource
    The piston model of coronal transients (1984)
    Springer
    Astrophysics and space science 100 (1984), S. 391-406 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In the present paper, the piston model of the coronal transient (see Hu. 1983a, b is discssed in detail, and the quantitative results of unsteady gasdynamics are applied to the coronal transient processes. The piston model explains the major features of the transient observations, such as the density profile, the geometric configuration, the kinetic process and the classifications of the coronal transient. Based on the idea of piston model, the bright feature and the dark feature of the transient are the gasdynamical response of the dense plasma ejecting into the corona, and associate with the compressed and rarefied flows, respectively. The quantitative results show that the density increment in the compressed region and the density decrement in the rarefied region are one order of magnitude larger and smaller, respectively, to the density in the quiet corona, it agrees quantitatively with the observations, and both the bright feature and dark feature are explained at the same time.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651614
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