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  • 1
    Electronic Resource
    Electronic Resource
    Investigation of two-wave mixing in arbitrary oriented sillenite crystals (1996)
    Springer
    Applied physics 64 (1996), S. 49-56 
    Details
    ISSN: 0340-3793
    Keywords: PACS: 42.40 ; 42.65 ; 42.70
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract.  A generalized systematic description of the Two-Wave Mixing (TWM) process in sillenite crystals allowing for arbitrary orientation of the grating vector is presented. An analytical expression for the TWM gain is obtained for the special case of plane waves in a thin crystal (∣g∣d≪1) with large optical activity (∣g∣/ϱ≪1, g is the coupling constant, ϱ the rotatory power, d the crystal thickness). Using a two-dimensional formulation the scope of the nonlinear equations describing TWM can be extended to finite beams in arbitrary geometries and to any crystal parameters. Two promising applications of this formulation are proposed. The polarization dependence of the TWM gain is used for the flattening of Gaussian beam profiles without expanding them. The dependence of the TWM gain on the interaction length is used for the determination of the crystal orientation. Experiments carried out on Bi12GeO20 crystals of a non-standard cut are in good agreement with the results of modelling.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/s003400050144
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    Paper (German National Licenses)
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  • 2
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    Comparison of CME masses and kinetic energies near the Sun and in the inner heliosphere (1995)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: Masses have now been determined for many of the CMEs observed in the inner heliosphere by the HELIOS 1 and 2 zodiacal light photometers. The speed of the brightest material of each CME has also been measured so that, for events having both mass and speed determinations, the kinetic energies of the CMEs are estimated. We compare the masses and kinetic energies of the individual CMEs measured in the inner heliosphere by HELIOS and near the Sun from observations by the SOLWIND (1979-1983) and SMM coronagraphs (1980). Where feasible we also compare the speeds of the same CMEs. We find that the HELIOS masses and energies tend to be somewhat larger by factors of 2-5 than those derived from the coronagraph data. We also compare the distribution of the masses and energies of the HELIOS and coronagraph CMEs over the solar cycle. These results provide an important baseline for observations of CMEs from coronagraphs, from the ISEE-3/ICE, WIND and Ulysses spacecraft and in the future from SOHO.
    Keywords: Solar Physics
    Type: International Solar Wind 8 Conference; 97; NASA-CR-199940
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  • 3
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    The Solar Mass Ejection Imager (1995)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: We are designing a Solar Mass Ejection Imager (SMEI) capable of observing the Thomson-scattered signal from transient density features in the heliosphere from a spacecraft situated near AU. The imager is designed to trace these features, which include coronal mass ejections. corotating structures and shock waves, to elongations greater than 90 deg from the Sun. The instrument may be regarded as a progeny of the heliospheric imaging capability shown possible by the zodiacal-light photometers of the HELIOS spacecraft. The instrument we are designing would make more effective use of in-situ solar wind data from spacecraft in the vicinity of the imager by extending these observations to the surrounding environment. The observations from the instrument should allow deconvolution of these structures from the perspective views obtained as they pass the spacecraft. An imager at Earth could allow up to three days warning of the arrival of a mass ejection from the Sun .
    Keywords: Solar Physics
    Type: International Solar Wind 8 Conference; 97; NASA-CR-199940
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  • 4
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    Correspondence between solar fine-scale structures in the corona, transition region, and lower atmosphere from collaborative observations (1989)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The Soft X-Ray Imaging Payload and the High Resolution Telescope and Spectrograph (HRTS) instrument were launched from White Sands on 11 December 1987 in coordinated sounding rocket flights to investigate the correspondence of coronal and transition region structures, especially the relationship between X-ray bright points (XBPs) and transition region small spatial scale energetic events. The coaligned data from X-ray images are presented along with maps of sites of transition region energetic events observed in C IV (100,000 K), HRTS 1600 A spectroheliograms of the T sub min region and ground based magnetogram and He I 10830 A images.
    Keywords: SOLAR PHYSICS
    Type: American Science and Engineering, Inc., Solar X-ray Astronomy Sounding Rocket Program; 26 p
    Format: application/pdf
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  • 5
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    Coronal manifestations of preflare activity (1986)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: A variety of coronal manifestations of precursors or preheating for flares are discussed. Researchers found that almost everyone with a telescope sees something before flares. Whether an all-encompassing scenario will ever be developed is not at all clear at present. The clearest example of preflare activity appears to be activated filaments and their manifestations, which presumably are signatures of a changing magnetic field. But researchers have seen two similar eruptions, one without any evidence of emerging flux (Kundu et al., 1985) and the other with colliding poles (Simon et al., 1984). While the reconnection of flux is generally agreed to be required to energize a flare, the emergence of flux from below (at least on short timescales and in compact regions) does not appear to be a necessary condition. In some cases the cancelling of magnetic flux (Martin, 1984) by horizontal motions instead may provide the trigger (Priest, 1985) Researchers found similarities and some differences between these and previous observations. The similarities, besides the frequent involvement of filaments, include compact, multiple precursors which can occur both at and near (not at) the flare site, and the association between coronal sources and activity lower in the atmosphere (i.e., transition zone and chromosphere).
    Keywords: SOLAR PHYSICS
    Type: Energetic Phenomena on the Sun: The Solar Maximum Mission Flare Workshop. Proceedings; 32 p
    Format: application/pdf
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  • 6
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    X-ray and microwave observations of active regions (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Coordinated high-resolution (1-3 arcsec) observations of two active solar regions (H 421 and H 419) on November 16, 1979, are reported: soft-X-ray filtergrams from a sounding rocket flight, VLA total-intensity and circular-polarization microwave (6-cm) radio maps, KPNO full-disk photospheric magnetograms, and BBSO H-alpha data. The images were converted to 4.8-arcsec/mm-scale transparencies and coaligned on the basis of sunspot positions for comparison. The two active regions are characterized in detail, and intensity, size, and polarization data for the brightest microwave components (BMC) are listed. It is found that 19 of the 32 BMC are farther than 5 arcsec from any sunspot, and that X-ray-emitting structures only rarely correspond to sunspots, or BMC. About one third of the BMC are located at the feet or legs of coronal loops smaller than about 50,000 km. The limitations implied by these obervations for proposed thermal-bremsstrahlung, thermal-gyro-resonance, and nonthermal microwave-emission mechanisms are discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 85; June 198
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  • 7
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    X-ray and H-alpha observations of a filament-disappearance flare - An empirical analysis of the magnetic field configuration (1981)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: On August, 29, 1973, a flare event occurred that involved the disappearance of a filament near central meridian. The event, well-observed in X-rays on Skylab and in H-alpha, was a four-ribbon flare involving both new and old magnetic inversion lines which were roughly parallel. The H-alpha, X-ray, and magnetic field data are used to deduce the magnetic polarities of the H-alpha brightening at the footpoints of the brightest X-ray loops. It is suggested that the event involved a reconnection of magnetic field lines rather than a brightening in place of preexisting loops. The simultaneity of the H-alpha brightening onsets in the four ribbons and the apparent lack of an eruption of the filament are consistent with this interpretation.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 70; Apr. 198
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  • 8
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    Kinematical analysis of flare spray ejecta observed in the corona (1981)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Observations in H-alpha, soft X-ray, white light and radio wavelengths are used to track cool and hot material from limb de-occultation to the extent of six solar radii. The kinematics and thermodynamics of the internal material are determined, along with the overall mass and energy budget of the event. It is found that the majority of the mass and energy is linked with the coronal material, but at least 20% of the ejected mass originated as near-surface prominence material, leading to the conclusions that the upper part of the prominence was being heated to coronal temperatures as it rose through the corona. Evidence was found that a moving type IV burst, indicative of strong magnetic fields, was associated with the upper part of the prominence, and the observations are judged to be most consistent with magnetic propulsion models of coronal transients.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 73; Oct. 198
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  • 9
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    Coronal loops and active region structure (1981)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Synoptic H-alpha Ca K, magnetograph and Skylab soft X-ray and EUV data were compared for the purpose of identifying the basic coronal magnetic structure of loops in a 'typical' active region and studying its evolution. A complex of activity in July 1973, especially McMath 12417, was emphasized. The principal results are: (1) most of the brightest loops connected the bright f plage to either the sunspot penumbra or to p satellite spots; no non-flaring X-ray loops end in umbrae; (2) short, bright loops had one or both ends in regions of emergent flux, strong field or high field gradients; (3) stable, strongly sheared loop arcades formed over filaments; (4) EFRs were always associated with compact X-ray arcades; and (5) loops connecting to other active regions had their bases in outlying plage of weak field strength in McM 417 where H-alpha fibrils marked the direction of the loops
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 69; Jan. 198
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  • 10
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    Mechanical energy output of the 5 September 1973 flare (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The mechanical energy flux of observed macroscopic mass plasma motions in the solar flare of Sept. 5, 1973, is estimated. Consideration is given to the cool eruptive material in the eruptive filament and large surge as revealed by H alpha observations, the moving emission front seen in Ca II as well as H alpha, the piston-driven shock and mass ejection coronal transient observed in radio spectra and flare core motions, and mechanical energy estimates of 5.6 x 10 to the 29th to 8.9 x 10 to the 30th, 9.0 x 10 to the 29th, 2 x 10 to the 30th (thermal) and 10 to the 31st (magnetic), and 9 x 10 to the 24th erg are obtained, respectively, in agreement with previous estimates. It is concluded that the mechanical energy of large-scale mass motions dominates the radiative output of the flare by more than two orders of magnitude, and that a significant portion of the mechanical energy is in the form of magnetic flux delivered to interplanetary space.
    Keywords: SOLAR PHYSICS
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