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  • 1
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    Climate and weather of the Sun-Earth system (CAWSES) : selected papers from the 2007 Kyoto Symposium (2009)
    Tokyo : TERRAPUB
    Details
    Keywords: Sun-Earth system ; space weather ; solar cycles ; solar wind ; solar activity ; sunspot ; ozone ; troposphere ; stratosphere ; Quasi-Biennial Oscillation (QBO)
    Description / Table of Contents: Early Japanese contributions to space weather research—1945-1960— / A. Nishida / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 1-22 --- Hydrodynamics, magnetohydrodynamics, and astrophysical plasmas / E. N. Parker / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 23-40 --- The 1960s—A decade of remarkable advances in middle atmosphere research / M. A. Geller / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 41-62 --- Hinode "a new solar observatory in space" / S. Tsuneta, L. K. Harra, and S. Masuda / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 63-75 --- Coronal mass ejections and space weather / N. Gopalswamy / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 77-120 / © TERRAPUB, Tokyo, 2009. No claim is made to original U.S. Government works. / [Full text] (PDF 3.9 MB) --- Magnetotail after Geotail, Interball and Cluster: Thin current sheets, fine structure, force balance and stability / L. Zelenyi, H. Malova, A. Artemyev, V. Popov, A. Petrukovich, D. Delcourt, and A. Bykov / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 121-170 --- Simulating solar 'climate' / M. Dikpati / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 171-199 --- Evidence for solar forcing: Some selected aspects / J. Beer and K. McCracken / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 201-216 --- Total solar irradiance variability: What have we learned about its variability from the record of the last three solar cycles? / C. Fröhlich / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 217-230 --- Mechanisms for solar influence on the Earth's climate / J. D. Haigh / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 231-256 --- Variability in the stratosphere: The sun and the QBO / K. Labitzke and M. Kunze / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 257-278 --- Gravity wave coupling from below: A review / R. A. Vincent / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 279-293 --- What we have learnt from CPEA (Coupling Processes in the Equatorial Atmosphere): A review / S. Fukao / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 295-336 --- Vertical coupling by the semidiurnal tide in Earth's atmosphere / J. M. Forbes / Climate and Weather of the Sun-Earth System (CAWSES): Selected Papers from the 2007 Kyoto Symposium, / pp. 337-348
    Pages: Online-Ressource (VII, 351 Seiten)
    ISBN: 9784887041479
    URL: http://www.terrapub.co.jp/onlineproceedings/ste/CAWSES2007/
    Language: English
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  • 2
    Electronic Resource
    Electronic Resource
    Magnetic reconnection as the origin of X-ray jets and Hα surges on the Sun (1995)
    [s.l.] : Nature Publishing Group
    Nature 375 (1995), S. 42-44 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Many solar X-ray jets are known to be ejected from emerging flux regions1 3. This suggests that the magnetic energy of the emerging flux10 is converted to the bulk kinetic and internal energy of the jets. How can this conversion take place? The model of Shibata et al.n is ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/375042a0
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  • 3
    Electronic Resource
    Electronic Resource
    Formation of astrophysical jets by a contracting magnetic accretion disk (1986)
    Springer
    Astrophysics and space science 118 (1986), S. 443-447 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In the present paper, we discuss an MHD model for the formation of astrophysical jets, in which the directed flows are ejected along the rotation axis of an accretion disk formed from a cloud having a large scale magnetic field parallel to the angular momentum axis of the disk. The acceleration of jets is due to thej×B force in the relaxing magnetic twist which is produced by the rotation of the disk. The characteristic features of the jets, predicted by our mechanism and hopefully to be proven by observations, are the helical velocity and the hollow cylindrical shape of the jet, with a diameter of roughly the size of the region from which the acceretion disk collected its mass. Justification for the assumption of the perpendicular orientation of the disk, or the parallelism of the jets, to the external magnetic field may be provided by the fact that the component of rotation whose axis is perpendicular to the field may have been damped in the earlier phase of the cloud contraction.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651165
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  • 4
    Electronic Resource
    Electronic Resource
    Evidence of Magnetic Reconnection in Solar Flares and a Unified Model of Flares (1998)
    Springer
    Astrophysics and space science 264 (1998), S. 129-144 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The solar X-ray observing satellite Yohkoh has discovered various new dynamic features in solar flares and corona, e.g., cusp-shaped flare loops, above-the-loop-top hard X-ray sources, X-ray plasmoid ejections from impulsive flares, transient brightenings (spatially resolved microflares), X-ray jets, large scale arcade formation associated with filament eruption or coronal mass ejections, and so on. It has soon become clear that many of these features are closely related to magnetic reconnection. We can now say that Yohkoh established (at least phenomenologically) the magnetic reconnection model of flares. In this paper, we review various evidence of magnetic reconnection in solar flares and corona, and present unified model of flares on the basis of these new Yohkoh observations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1002413214356
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  • 5
    Electronic Resource
    Electronic Resource
    Rotating eruption of an untwisting filament triggered by the 3B flare of 25 April, 1984 (1987)
    Springer
    Solar physics 108 (1987), S. 251-264 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A great 3B flare, whose X-ray class was X13, occurred over a delta-sunspot at 00: 01 UT on April 25, 1984. Before the flare, a strong magnetic shear was found to be formed along the neutral line in the delta-sunspot with shear motions of umbrae. The shear motions of the umbrae were caused by the successive emergence of a magnetic flux rope. Before the flare, several groups of sheared Hα threads and filaments were found to merge into an elongated filament along the neutral line through the delta-sunspot. In the merging process the helical twists were formed in the filament by the reconnection as in the Pneuman's (1983) model. At the post-maximum phase of the flare, the helically twisted filament spouted out with an untwisting rotation. Examining the morphological and dynamical features of the filament eruption, we concluded that it has some typical features of the flare spray and that it seems to be accelerated by the sweeping-magnetictwist mechanism proposed by Shibata and Uchida (1986).
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00214165
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  • 6
    Electronic Resource
    Electronic Resource
    A magnetodynamic mechanism for the heating of emerging magnetic flux tubes and loop flares (1988)
    Springer
    Solar physics 116 (1988), S. 291-307 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A new magnetodynamic model for loop flares is proposed to explain the following observational facts obtained from space during the last solar activity maximum: (i) Blueshifted lines of Ca xix and Fe xxv appear in some cases a minute or so before the initiation of impulsive bursts and relax into the unshifted lines with large width by the time of the onset of impulsive bursts, (ii) the hot source is formed by that time at the top of a loop-like structure, and confined there for a considerable time, and (iii) γ-ray line enhancement occurs at about the same time as hard X-ray spikes. In our model, the supply of energy to the loop top comes from below the chromosphere immediately before the flare (30 s-1 min before the hard X-ray impulsive bursts) in the form of the relaxing fronts of magnetic twist of opposite sign. These packets are thought to be built up in the process of loop emergence, stored at the footpoints of the loop below the photosphere, and released when the part of the feet floats up further. These released packets of magnetic twist drive the mass in the high chromosphere and transition zone into helical flows with pinch heating, and when these collide at the top of the loop, a very hot region appears there with a violent unwinding of the twists, resulting in the rapid dynamical annihilation of the magnetic energy, $$B_\varphi ^2 /8\pi$$ . Electrons and ions, raised to medium energies in the pinch at the incidence of the packets to the loop, are accelerated further by the Fermi-I mechanism between the approaching fronts of magnetic twist, and when B ϕ is weakened by unwinding they are released towards the chromosphere, and cause simultaneous γ-ray and hard X-ray bursts.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157480
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  • 7
    Electronic Resource
    Electronic Resource
    On the origin of strong downdrafts associated with the birth of sunspots (1980)
    Springer
    Solar physics 66 (1980), S. 61-70 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract During the emerging phase of sunspot pores strong downdrafts are observed in photospheric lines, whereas the upward flow is not detected within the observational accuracy. For the study of the origin of these downdrafts, we present the numerical solutions of non-steady hydrodynamic equations in one dimension along the rising magnetic flux tubes. In these solutions, it is assumed that the solar gas inside the tube is initially in the hydrostatic HSRA and then the tube rises with a given velocity and configuration. The results reproduce well the observed radial velocity distributions, hence it is concluded that the observed strong downdrafts originate from the sliding matter along the rising magnetic flux tubes.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00150518
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  • 8
    Electronic Resource
    Electronic Resource
    Numerical hydrodynamics of the jet phenomena in the solar atmosphere (1982)
    Springer
    Solar physics 75 (1982), S. 99-118 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present a spicule model whose eruption occurs as a result of the sudden pressure enhancement at the bright point located at the root of the spicule. To show this, one dimensional (constant cross sectional) and time dependent hydrodynamic equations are solved numerically in the realistic solar atmosphere extending from the photosphere to the corona. Adiabatic motion is assumed. The pressure enhancement by a bright point at the base of the model atmosphere generates a shock wave. The shock gets stronger as it passes upward through the chromosphere and eventually collides with the chromosphere-corona interface which is a kind of a contact discontinuity. As the result, the interface begins to move upward. We identify the matter following behind this interface as the solar spicule. The model explains many observed features, such as the height and the density of the spicules, although such features have been hitherto considered not to be explained easily by shock theories.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153464
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  • 9
    Electronic Resource
    Electronic Resource
    Numerical hydrodynamics of the jet phenomena in the solar atmosphere (1982)
    Springer
    Solar physics 77 (1982), S. 121-151 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract One-dimensional hydrodynamic simulations of surges are performed in order to make clear their origin and structure. Surges are regarded as the jets resulting from a sudden pressure increase at the base of the model atmosphere. The height of the explosion (h 0), which is measured from the level of τ5000 = 1, is regarded as a free parameter. Another free parameter is the strength of the sudden pressure increase (p/p 0) at h 0. Simulations are performed for values in the ranges of 540 km ≤ h 0 ≤ 1920 km and 3 ≤ p/p 0 ≤ 30. It was found that for a fixed p/p 0 there exists a critical height (h c ) in h 0, which separates the jet (surge) models into two types. For h 0 〉 h c , jets are produced directly by the pressure gradient force near h 0, and made of the matter ejected from the explosion itself. The essential hydrodynamic structure of this type is the same as that in a shock tube (this type is called ‘shock tube’ type). For h 0 〈 h c , jets are not the direct results of the pressure enhancement, but are produced by the shock wave which are generated by the pressure enhancement and which has propagated through the chromosphere (this type is called the ‘crest shock’ type). It is shown that the critical height (h c ) ranges from 1000 km to 1500 km for 3 ≤ p/p 0 ≤ 30. General properties of both types are investigated in detail. The results are compared with observations and it is concluded that small surges associated with Ellerman bombsbelong to the ‘crest shock’ type, i.e. they are produced by the shock wave.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00156100
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  • 10
    Electronic Resource
    Electronic Resource
    Why are spicules absent over plages and long under coronal holes? (1982)
    Springer
    Solar physics 78 (1982), S. 333-345 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract One-dimensional hydrodynamic simulations are performed in order to examine the influence of initial atmospheric structures on the dynamics of spicules. This is an extended version of our previous spicule theory: spicules are produced by the shock wave (MHD slow mode shock) which originates from a bright point appearance (sudden pressure increase) at the network in the photosphere or in the low chromosphere. Simulation results well reproduce the observational facts that spicules are absent over plages and long under coronal holes. The physical reason is that the growth of a shock wave during its propagation through the chromosphere is small in plage regions and large in coronal hole regions, since the growth of a shock is determined by the density ratio (ϱ h 0/ϱ c ) between the bright point and the corona. An empirical formula ΔH max ∼ (ϱ h 0/ϱ c )0.46 is obtained, where ΔH max is the maximum height of spicules above the transition region. The cross-section of the vertical magnetic flux tube is assumed to be constant in the numerical simulations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151612
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