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  • 1
    Electronic Resource
    Electronic Resource
    Bolometric detection of the recoil spectrum in the alpha decay of ^2^1^0Po
    Amsterdam : Elsevier
    Nuclear Instruments and Methods in Physics Research Section A: 349 (1994), S. 225-230 
    Details
    ISSN: 0168-9002
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1016/0168-9002(94)90624-6
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  • 2
    Electronic Resource
    Electronic Resource
    Performance and applications of cooled composite bolometers in the field of ionizing radiation metrology
    Amsterdam : Elsevier
    Nuclear Instruments and Methods in Physics Research Section A: 312 (1992), S. 24-33 
    Details
    ISSN: 0168-9002
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0168-9002(92)90121-J
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    Paper (German National Licenses)
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  • 3
    Electronic Resource
    Electronic Resource
    High resolution spectroscopy of the disk chromosphere (1974)
    Springer
    Solar physics 37 (1974), S. 309-315 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We describe the properties of dark structures which are seen in the K-line wings and which seem to propagate inward into the K-line core, or upward in the solar atmosphere. These so-called dark whiskers appear to be related to the bright disturbances (bright whiskers) described by Liu (1974). Both may be related to the shocks that heat the chromosphere and corona.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152490
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    Paper (German National Licenses)
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  • 4
    Electronic Resource
    Electronic Resource
    O VI (λ = 1032 Å) profiles in and above an active region prominence, compared to quiet Sun center and limb profiles (1980)
    Springer
    Solar physics 68 (1980), S. 187-206 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract O vi (λ = 1032 Å) profiles have been measured in and above a filament at the limb, previously analyzed in H i, Mg ii, Ca ii resonance lines (Vial et al., 1979). They are compared to profiles measured at the quiet Sun center and at the quiet Sun limb. Absolute intensities are found to be about 1.55 times larger than above the quiet limb at the same height (3″); at the top of the prominence (15″ above the limb) one finds a maximum blue shift and a minimum line width. The inferred non-thermal velocity (29 km s−1) is about the same as in cooler lines while the approaching line-of-sight velocity (8 km s−1) is lower than in Ca ii lines. The O vi profile recorded 30″ above the limb outside the filament is wider (FWHM = 0.33 Å). It can be interpreted as a coronal emission of O vi ions with a temperature of about 106 K, and a non-thermal velocity (NTV) of 49 km s−1. This NTV is twice the NTV of quiet Sun center O vi profiles. Lower NTV require higher temperatures and densities (as suggested by K-coronameter measurements). Computed emission measures for this high temperature regime agree with determinations from disk intensities of euv lines.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153276
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  • 5
    Electronic Resource
    Electronic Resource
    EIT: Extreme-ultraviolet Imaging Telescope for the SOHO mission (1995)
    Springer
    Solar physics 162 (1995), S. 291-312 
    Details
    ISSN: 1573-093X
    Keywords: Solar X-rays ; Solar EUV ; Multilayer telescope
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Extreme-ultraviolet Imaging Telescope (EIT) will provide wide-field images of the corona and transition region on the solar disc and up to 1.5 R⊙ above the solar limb. Its normal incidence multilayer-coated optics will select spectral emission lines from Fe IX (171 Å), Fe XII (195 Å), Fe XV (284 Å), and He II (304 Å) to provide sensitive temperature diagnostics in the range from 6 × 104 K to 3 × 106 K. The telescope has a 45 x 45 arcmin field of view and 2.6 arcsec pixels which will provide approximately 5-arcsec spatial resolution. The EIT will probe the coronal plasma on a global scale, as well as the underlying cooler and turbulent atmosphere, providing the basis for comparative analyses with observations from both the ground and other SOHO instruments. This paper presents details of the EIT instrumentation, its performance and operating modes.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00733432
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  • 6
    Electronic Resource
    Electronic Resource
    Profiles of Hi (La), Mgii (h and k), Caii (H and K) Lines of an active filament at the limb, with the LPSP instrument aboard the OSO-8 Satellite (1979)
    Springer
    Solar physics 61 (1979), S. 39-59 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We scanned the H i Lα, Mg ii h and k, Ca ii K and H lines simultaneously with the LPSP instrument on OSO-8, to investigate the low and moderate temperature regions of an ‘active region filament’. The Lα line is not reversed except for the innermost position in the prominence. Intensity (k/h), (K/H) ratios are respectively 2 and 1.1, indicating that the Mg ii lines are optically thin, and that Ca ii K is saturated, although not clearly reversed. The results obtained during the second sequence of observations (K saturated before Lα for example) indicate that within the size of the slit (1″ × 10″) we are not observing the same emitting features in the different lines. We also observe an important line-of-sight velocity at the outer edge of the feature, increasing outwards from a few km s−1 to 20 km s−1 within 2″. Less than half an hour later, this velocity is reduced to 15 km s−1 while the intensities increase. Full width at half maximum intensities for this component indicate turbulence variations from 22 to 30 km s−1. The observed high velocities at the top of the prominence can be compared with radial velocities that Mein (1977) observed in Hα at the edges of an active filament and interpreted as velocity loops slightly inclined on the axis of the filament.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155445
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  • 7
    Electronic Resource
    Electronic Resource
    Solar astrometry by photolithography (1990)
    Springer
    Solar physics 128 (1990), S. 281-286 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Observed temporal variations of shape and size of the solar disk as viewed from Earth may act as constraints for theories of the interior of the Sun. In addition to existing programs of solar diameter measurements we investigate a ground-based photographic method. The solar limb profile is recorded on a photoresist-coated substrate over a 20″ radial length simultaneously all along the circonference as a three-dimensional 21 mm diameter, 0.0015mm thick permanent object available for inspection by interferometric methods. The exposure time is long enough for filtering much of the atmospheric turbulence, whereas the slope of the observed solar limb should help to locate a ‘standard’ solar limb. The first results of February 1989 at large zenith distance and low altitude are a set of differential measurements of the position of a solar limb around a circle with, after taking into account the 3″.7 atmospheric differential refraction, a 0″.34r.m.s. dispersion of the residuals for a fit to a circular solar disk. We estimate that this method of accuracy comparable to other ground-based methods, with potentially more than 600 independent simultaneous measurements along the circonference, could help to discriminate between terrestrial and solar causes for variations of shape and size of the solar disk. We note that operation outside the Earth's atmosphere would provide access not only to undisturbed images but also to UV wavelengths, i.e., to a better definition of the solar limb.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00154164
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  • 8
    Electronic Resource
    Electronic Resource
    Eit Observations of the Extreme Ultraviolet Sun (1997)
    Springer
    Solar physics 175 (1997), S. 571-599 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Extreme Ultraviolet Imaging Telescope (EIT) on board the SOHO spacecraft has been operational since 2 January 1996. EIT observes the Sun over a 45 x 45 arc min field of view in four emission line groups: Feix, x, Fexii, Fexv, and Heii. A post-launch determination of the instrument flatfield, the instrument scattering function, and the instrument aging were necessary for the reduction and analysis of the data. The observed structures and their evolution in each of the four EUV bandpasses are characteristic of the peak emission temperature of the line(s) chosen for that bandpass. Reports on the initial results of a variety of analysis projects demonstrate the range of investigations now underway: EIT provides new observations of the corona in the temperature range of 1 to 2 MK. Temperature studies of the large-scale coronal features extend previous coronagraph work with low-noise temperature maps. Temperatures of radial, extended, plume-like structures in both the polar coronal hole and in a low latitude decaying active region were found to be cooler than the surrounding material. Active region loops were investigated in detail and found to be isothermal for the low loops but hottest at the loop tops for the large loops. Variability of solar EUV structures, as observed in the EIT time sequences, is pervasive and leads to a re-evaluation of the meaning of the term ‘quiet Sun’. Intensity fluctuations in a high cadence sequence of coronal and chromospheric images correspond to a Kolmogorov turbulence spectrum. This can be interpreted in terms of a mixed stochastic or periodic driving of the transition region and the base of the corona. No signature of the photospheric and chromospheric waves is found in spatially averaged power spectra, indicating that these waves do not propagate to the upper atmosphere or are channeled through narrow local magnetic structures covering a small fraction of the solar surface. Polar coronal hole observing campaigns have identified an outflow process with the discovery of transient Fexii jets. Coronal mass ejection observing campaigns have identified the beginning of a CME in an Fexii sequence with a near simultaneous filament eruption (seen in absorption), formation of a coronal void and the initiation of a bright outward-moving shell as well as the coronal manifestation of a ‘Moreton wave’.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1004902913117
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  • 9
    Electronic Resource
    Electronic Resource
    Eit and LASCO Observations of the Initiation of a Coronal Mass Ejection (1997)
    Springer
    Solar physics 175 (1997), S. 601-612 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present the first observations of the initiation of a coronal mass ejection (CME) seen on the disk of the Sun. Observations with the EIT experiment on SOHO show that the CME began in a small volume and was initially associated with slow motions of prominence material and a small brightening at one end of the prominence. Shortly afterward, the prominence was accelerated to about 100 km s-1 and was preceded by a bright loop-like structure, which surrounded an emission void, that traveled out into the corona at a velocity of 200–400 km s-1. These three components, the prominence, the dark void, and the bright loops are typical of CMEs when seen at distance in the corona and here are shown to be present at the earliest stages of the CME. The event was later observed to traverse the LASCO coronagraphs fields of view from 1.1 to 30 R⊙. Of particular interest is the fact that this large-scale event, spanning as much as 70 deg in latitude, originated in a volume with dimensions of roughly 35" (2.5 x 104 km). Further, a disturbance that propagated across the disk and a chain of activity near the limb may also be associated with this event as well as a considerable degree of activity near the west limb.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1004907307376
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  • 10
    Electronic Resource
    Electronic Resource
    OSO-8 observations of CaII H and K, MgII h and k, Lα and Lβ above a sunspot (1981)
    Springer
    Solar physics 69 (1981), S. 289-300 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Observations with the French (L.P.S.P.) experiment on board OSO-8 of a sunspot and nearby plage region are described. The behaviour of the emission cores of the Ca II H and K and Mg II h and k resonance lines is very similar and the correspondence in intensity between the four lines persists in all observed features. In contrast, the Lyman lines show little correlation with the other lines. Their emission regions appear broader in the spectroheliograms than the underlying sunspot structure and must not necessarily possess a counterpart in lower layers. From the central intensity of Lα above the umbra an electron density of 4.3 × 1010 cm-3 ≲n e * ≲2.3 × 1011 cm-3 at 20 000 K is estimated.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149995
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