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  • 1
    Electronic Resource
    Electronic Resource
    Solar Flares and Coronal Mass Ejections (1992)
    Palo Alto, Calif. : Annual Reviews
    Annual Review of Astronomy and Astrophysics 30 (1992), S. 113-141 
    Details
    ISSN: 0066-4146
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1146/annurev.aa.30.090192.000553
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  • 2
    Electronic Resource
    Electronic Resource
    Preflare X-ray morphology of active regions observed with the AS & E telescope on Skylab (1976)
    Springer
    Solar physics 47 (1976), S. 157-165 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Images from the AS & E X-ray telescope on Skylab were examined for evidence of a flare build-up during the 20 minute periods preceding eight small X-ray flares. In two cases no activity could be seen up to 2 min before the flare onset. In no case did a preflare brightening occur in and only in the region which flared.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152252
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  • 3
    Electronic Resource
    Electronic Resource
    The quantitative properties of three soft X-ray flare kernels observed with the AS&E X-ray telescope on Skylab (1976)
    Springer
    Solar physics 50 (1976), S. 179-196 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The physical parameters for the kernels of three solar X-ray flare events have been deduced using photographic data from the S-054 X-ray telescope on Skylab as the primary data source and 1–8 and 8–20 Å fluxes from Solrad 9 as the secondary data source. The kernels had diameters of ∼5–7″ and in two cases electron densities at least as high as 3 × 1011 cm−3. The lifetimes of the kernels were 5–10 min. The presence of thermal conduction during the decay phases is used to argue: (1) that kernels are entire, not small portions of, coronal loop structures, and (2) that flare heating must continue during the decay phase. We suggest a simple geometric model to explain the role of kernels in flares in which kernels are identified with emerging flux regions. The flare is triggered at the neutral sheet between the EFR and a larger loop structure. We associate the X-ray kernels with Hα kernels, which previously associated (incorrectly, we believe) with the nonthermal impulsive phases of flares.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00206200
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  • 4
    Electronic Resource
    Electronic Resource
    Preflare characteristics of active regions observed in soft X-rays (1979)
    Springer
    Solar physics 62 (1979), S. 347-357 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract X-ray images from the AS&E telescope on Skylab are used to investigate coronal conditions in solar active regions during the 20-min periods preceding the X-ray onsets of small flares. The preflare or precursor phase is defined as a phase with a characteristic length or time scale significantly different from that of the rise phase. We show that there is no observational evidence of a requirement for a coronal preflare heating phase with a time scale longer than 2 min for small flares characterized by one or two loops. In 18 out of 25 cases the flaring X-ray structure was not the brightest feature in the preflare active region. The electron densities are estimated for preflare loops.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155363
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  • 5
    Electronic Resource
    Electronic Resource
    The GLE-associated flare of 21 August, 1979 (1983)
    Springer
    Solar physics 89 (1983), S. 181-193 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We use a variety of ground-based and satellite measurements to identify the source of the ground level event (GLE) beginning near 06∶30 UT on 21 August, 1979 as the 2B flare with maximum at ∼06∶15 UT in McMath region 16218. This flare differed from previous GLE-associated flares in that it lacked a prominent impulsive phase, having a peak ∼9 GHz burst flux density of only 27 sfu and a ≳20 keV peak hard X-ray flux of ≲3 × 10-6 ergs cm-2s-1. Also, McMath 16218 was magnetically less complex than the active regions in which previous cosmic-ray flares have occurred, containing essentially only a single sunspot with a rudimentary penumbra. The flare was associated with a high speed (≳700 km s-1) mass ejection observed by the NRL white light coronagraph aboard P78-1 and a shock accelerated (SA) event observed by the low frequency radio astronomy experiment on ISEE-3.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00211961
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  • 6
    Electronic Resource
    Electronic Resource
    The spatial distribution of 6 centimeter gyroresonance emission from a flaring X-ray loop (1984)
    Springer
    Solar physics 92 (1984), S. 271-281 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We compare simultaneous high resolution soft X-ray and 6 cm images of the decay phase of an M3 X-ray flare in Hale Region 16413. The photographic X-ray images were obtained on an AS & E sounding rocket flown 7 November, 1979, and the 6 cm observations were made with the VLA. The X-ray images were converted to arrays of line-of-sight emission integrals and average temperature throughout the region. The X-ray flare structure consisted of a large loop system of length ∼ 1.3 arc min and average temperature ∼8 × 106 K. The peak 6 cm emission appeared to come from a region below the X-ray loop. The predicted 6 cm flux due to thermal bremsstrahlung calculated on the basis of the X-ray parameters along the loop was about an order of magnitude less than observed. We model the loop geometry to examine the expected gyroresonance absorption along the loop. We find that thermal gyroresonance emission requiring rather large azimuthal or radial field components, or nonthermal gyrosynchrotron emission involving continual acceleration of electrons can explain the observations. However, we cannot choose between these possibilities because of our poor knowledge of the loop magnetic field.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157251
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  • 7
    Electronic Resource
    Electronic Resource
    Discussion of paper ‘on the polarization and anisotropy of solar X-radiation during flares’, by G. Elwert and E. Haug (1971)
    Springer
    Solar physics 20 (1971), S. 422-424 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00159774
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  • 8
    Electronic Resource
    Electronic Resource
    Energetic protons from the solar flare of March 24, 1966 (1967)
    Springer
    Solar physics 2 (1967), S. 179-191 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Ten to 100 meV protons from the solar flare of March 24, 1966 were observed on the University of California scintillation counter on OGO-I. The short rise and decay times observed in the count rates of the 32 channels of pulse-height analysis show that scattering of the protons by the interplanetary field was much less important in this event than in previously observed proton flares. A diffusion theory in which D = M r β is found to be inadequate to account for the time behavior of the count rates of this event. Small fluctuations of the otherwise smooth decay phase may be due to flare protons reflected from the back of a shock front, which passed the earth on March 23.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155918
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  • 9
    Electronic Resource
    Electronic Resource
    The possible role of energetic electrons in the production of surges (1973)
    Springer
    Solar physics 32 (1973), S. 477-484 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Energetic electrons, which play a major role in the explosive phases of flares, are proposed as the energy source for the production of surges. Flare data from a two-year interval are analyzed to show that the probability of having surges associated with flares is greater when there are accompanying decimeter type III bursts or impulsive 8800 MHz bursts. The model of chromospheric heating by impulsive electrons proposed by Hudson is examined and shown to provide an adequate explanation for the origin of flare surges. The proposed surge model is consistent with the temporal evolution of the flare-surge event and the required surge energy. Surges not accompanied by flares can also probably be explained by the model.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00154960
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  • 10
    Electronic Resource
    Electronic Resource
    Reply to ‘shock wave effects in solar cosmic ray events’ by I. D. Palmer (1973)
    Springer
    Solar physics 33 (1973), S. 239-240 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152394
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