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  • 1
    Electronic Resource
    Electronic Resource
    Solar gradual hard X-ray bursts: Observations and an interpretation
    Amsterdam : Elsevier
    Advances in Space Research 6 (1986), S. 249-252 
    Details
    ISSN: 0273-1177
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics , Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0273-1177(86)90154-7
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  • 2
    Electronic Resource
    Electronic Resource
    Simultaneous radio scattering and white light observations of a coronal transient (1982)
    [s.l.] : Nature Publishing Group
    Nature 300 (1982), S. 157-159 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Figure 1 shows four coronal images obtained with the Solwind instrument6 on 24 October, 1979. The upper images were taken at 0316 and 1258 UT while the lower ones are difference images formed by subtracting the images at 0536 and 0804 UT from that at 0316 UT to show the changes that had taken place ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/300157a0
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  • 3
    Electronic Resource
    Electronic Resource
    Coronagraphic observations of two new sungrazing comets (1982)
    [s.l.] : Nature Publishing Group
    Nature 300 (1982), S. 239-242 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Our observations were obtained with the Naval Research Laboratory's Earth-orbiting SOLWIND coronagraph. This instrument has been operating routinely on the US Air Force Space Test Program satellite, P78-1, since March 1979. Its broadband (4,100-6,350 A) images show a Sun-centred annular field of ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/300239a0
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  • 4
    Electronic Resource
    Electronic Resource
    Rocket Observations of the Corona on March 7, 1970 (1970)
    [s.l.] : Nature Publishing Group
    Nature 226 (1970), S. 1135-1138 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] ON several occasions we have made non-eclipse photographs of the outer corona between 3 and 9 solar radii, using a rocket-borne coronagraph1. The instrument consists of two small Lyot coronagraphs placed side by side. Solar occultation for each is by a circular disk placed 76 cm in front of the 25 ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/2261135a0
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  • 5
    Electronic Resource
    Electronic Resource
    Observations of coronal structure during sunspot maximum (1982)
    Springer
    Space science reviews 33 (1982), S. 219-231 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract This paper presents some of the results that have been obtained from the Kitt Peak observations of coronal holes and the NRL observations of coronal transients during the recent years near sunspot maximum (1979–1981). On the average, low-latitude coronal holes of comparable size contained 3 times more flux near sunspot maximum than near the previous minimum. In the outer corona, transients occurred at the observed rate of at least 2 per day, and quiet conditions persisted during less than 15 % of the observed days. We describe a sample of the more than 800 events that we have observed so far, including the observation of a comet apparently colliding with the Sun.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00213255
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  • 6
    Electronic Resource
    Electronic Resource
    Rocket-coronagraph photometry of the 7 March, 1970 corona from 3 to 8.5 R s (1971)
    Springer
    Solar physics 21 (1971), S. 408-417 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A rocket-borne coronagraph utilizing external occulting disks was used to photograph the solar corona from 3 to 9 R s at 1931 UT on 7 March, 1970. Comparison of the rocket and ground-based observations shows a one-to-one correspondence between major streamers from the inner to the outer corona. In particular streamers over the poles are clearly visible against the background corona from 3 to ≳ 8 R s. These rocket data had a scattered light level of ∼1.2 × 10−10 B s. The derived quiet equatorial and polar K + F corona was within 10% of the absolute brightness of standard coronal models and displayed identical radial gradients to those models. The photometric profiles of the NE limb streamer were analyzed assuming a model in which the core density follows a Gaussian distribution in directions perpendicular to the radius vector. This streamer was assumed to be rooted on the visible disk at 55 to 60° from the plane-of-the-sky as based on K-coronameter and XUV data. An uncertainty of as much as a factor of three still remains for the value of the axis density owing to uncertainty in the line-of-sight dimension of the streamer.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00154292
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  • 7
    Electronic Resource
    Electronic Resource
    Observations of coronal disturbances from 1 to 9 R ⊙ (1974)
    Springer
    Solar physics 36 (1974), S. 203-217 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Hα, white-light and radio observations of a coronal disturbance on 1973 January 11 commencing at about 00h36m UT show that a piston-driven shock wave propagated outwards through the corona to heights of at least 9 R ⊙. Probably most of the expelled coronal gas originated in a coronal enhancement in the lower corona. Our estimate of the kinetic energy and the mass of the expelled gas is compatible with observations of piston-driven shock waves near the Earth. Shock-wave parameters are evaluated and a model of the disturbance outlined.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151561
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  • 8
    Electronic Resource
    Electronic Resource
    Coronal transients near sunspot maximum (1981)
    Springer
    Solar physics 69 (1981), S. 169-175 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Naval Research Laboratory's most recent Earth-orbiting coronagraph, called Solwind, has been observing the Sun's outer corona (2.6–10.0 R ⊙) at 10-min intervals since March 28, 1979. These observations provide the first comprehensive view of coronal transients near the peak of a sunspot cycle. Six, well-defined transients in our quick-look data have masses ranging from 7 × 1014 g to 2 × 1016 g and outward speeds ranging from 150 km s−1 to 900 km s−1. These values are comparable to the ones that were obtained with the OSO-7 and Skylab observations during the declining phase of the last sunspot cycle. Although the amount of quick-look data is not sufficient to provide meaningful statistics, the coronal transients near sunspot maximum seem to occur with a greater frequency and a wider latitude range than the transients during the declining phase of the cycle. In both eras, there is a good, but imperfect, association between the occurrence of coronal transients and surface phenomena such as eruptive prominences and flares.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151264
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  • 9
    Electronic Resource
    Electronic Resource
    The Large Angle Spectroscopic Coronagraph (LASCO) (1995)
    Springer
    Solar physics 162 (1995), S. 357-402 
    Details
    ISSN: 1573-093X
    Keywords: Sun ; Corona ; Coronagraph
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Large Angle Spectroscopic Coronagraph (LASCO) is a three coronagraph package which has been jointly developed for the Solar and Heliospheric Observatory (SOHO) mission by the Naval Research Laboratory (USA), the Laboratoire d'Astronomie Spatiale (France), the Max-Planck-Institut für Aeronomie (Germany), and the University of Birmingham (UK). LASCO comprises three coronagraphs, C1, C2, and C3, that together image the solar corona from 1.1 to 30 R⊙ (C1: 1.1 – 3 R⊙, C2: 1.5 – 6 R⊙, and C3: 3.7 – 30 R⊙). The C1 coronagraph is a newly developed mirror version of the classic internally-occulted Lyot coronagraph, while the C2 and C3 coronagraphs are externally occulted instruments. High-resolution imaging spectroscopy of the corona from 1.1 to 3 R⊙ can be performed with the Fabry-Perot interferometer in C1. High-volume memories and a high-speed microprocessor enable extensive on-board image processing. Image compression by a factor of about 10 will result in the transmission of 10 full images per hour.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00733434
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  • 10
    Electronic Resource
    Electronic Resource
    The Shape of the Outer Corona during Cycle 21 (1998)
    Springer
    Solar physics 180 (1998), S. 247-263 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Naval Research Laboratory (NRL) Solwind coronagraph recorded the outer corona at elongations 2_5 R⊙ to 10 R⊙ during the 6 1/2-year interval from March 1979, before solar maximum, to the beginning of solar minimum in September 1985. During the minimum period, when the solar magnetic field was dipole-like, the observed corona consisted of the equatorial streamer belt that is characteristic of solar minimum, and that is interpreted as an edgewise view of a nearly flat current sheet or coronal disk lying near the plane of the heliographic equator. The observed disk was a radial projection from the magnetic neutral line that was computed for the 2.5 R⊙ source surface surrounding the Sun. At earlier times, shortly after solar maximum, the observed corona often consisted of a single coronal disk similar to that at solar minimum, but strongly tilted to the heliographic equator. Again this disk projected from a tilted magnetic neutral line that was computed for the 2.5 R⊙ source surface. Solar rotation allowed this coronal disk to be viewed in all aspects. In the edgewise view it appeared as a tilted streamer belt. In the broadside view the more flower-like pattern of solar maximum was observed. The latter view was interpreted as a non-uniform distribution of coronal material in the thin coronal disk. There were many intervals during the declining phase of the solar cycle when the computed magnetic neutral line at 2.5 R⊙ remained relatively simple but was not the source of an observable coronal disk. This latter result was probably because of the limitations of plane-of-sky observations, combined with short-term changes in the corona. Altogether, a single coronal disk, either flat or somewhat convoluted, was recognizable during only one third of the year lifetime of the coronagraph.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005039609265
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