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Gegenstand und Ziel: Ziel dieser Arbeit ist die Darstellung der aktuellen Versorgungsstrukturen fur Krebs-Patienten mit psychosozialen Belastungen. Methoden: Literaturrecherche fur die Versorgungssektoren (stationar, ambulant, sektorenubergreifend) und Einholung von Expertenwissen Ergebnisse: Psychoonkologische Versorgung steht in allen Versorgungsbereichen fur die Patienten, ihre Angehorigen und Hinterbliebenen zur Verfugung, jedoch nicht immer flachendeckend. Vor allem im ambulanten Bereich und im landlichen Raum gibt es noch erhebliche Versorgungslucken. Die Arbeit der Krebsberatungsstellen ist durch mangelnde Regelfinanzierung nicht sichergestellt. Im stationaren Bereich konnen Leistungen zwar dokumentiert werden, sind jedoch auch nicht erlosrelevant, sodass die Versorgung nur uber das freiwillige Zertifizierungssystem gesichert ist. Eine wichtige Hurde zur Inanspruchnahme besteht darin, dass Patienten nicht uber die vorhandenen Angebote informiert sind. Sie wunschen sich haufig, dass ihr Arzt ihnen empfiehlt, dass sie Unterstutzung in Anspruch nehmen sollten und ihnen sagt, wohin sie sich wenden konnen. Schlussfolgerungen: Die Versorgungssituation konnte noch weiter verbessert warden durch die Sicherstellung der Finanzierung und durch bessere Informierung der Patienten. Arzte konnen ihren Patienten helfen, indem sie konkrete Empfehlungen zur Inanspruchnahme von psychoonkologischen Angeboten aussprechen. Objectives: This work aims to describe the current care structures for cancer patients with psycho-social stress. Methods: Literature search for the different care sectors (inpatient, outpatient, cross-sector) and procuring expert knowledge. Results: Psycho-oncological care is available in all areas of care for patients, their relatives and the bereaved, but not always comprehensively. In particular, there are still considerable gaps in care in the outpatient setting and in rural areas. Due to a lack of regular funding, the continued existence of the Cancer Counselling Centres is not yet assured. Although services in the inpatient setting can indeed be documented, they are not relevant from a revenue prospective, with the result that this type of care is only safeguarded via a voluntary certification system. An important hurdle to using this type of care is that patients are not informed about the available options. They often wish that their doctor would recommend that they obtain support and tell them where they can turn to. Conclusion: The care situation could be further improved by securing funding and better informing patients. Physicians can help their patients by expressing concrete recommendations that they use psycho-oncological care options.

Die psychoonkologische Versorgung in Deutschland wird stationar, ambulant und sektorenubergreifend angeboten. In den Akutkrankenhausern hat sich die Versorgungssituation durch die Einfuhrung der Zertifizierungen in den letzten Jahren erheblich verbessert. In zertifizierten Zentren mussen alle Patienten die Gelegenheit erhalten, bei Bedarf mit einem qualifizierten Psychoonkologen zu sprechen. Onkologische Spitzenzentren mussen daruber hinaus uber eine psychoonkologische Ambulanz verfugen. In Rehabilitationskliniken werden supportive psychoonkologischen Behandlungen, kunstlerische und Bewegungstherapien angeboten, die die Patienten gewinnbringend fur ihre Bewaltigung der Tumorerkrankung nutzen konnen. Im ambulanten Bereich erfolgt psychoonkologische Versorgung vorrangig durch multiprofessionelle Teams in Krebsberatungsstellen und durch niedergelassene Psychotherapeuten mit Zusatzqualifikation. Die Finanzierung der Leistungen von Krebsberatungsstellen ist noch nicht ausreichend gesichert. Sektorenubergreifende psychoonkologische Versorgung ist im Rahmen der ambulanten spezialarztlichen Versorgung moglich, allerdings bisher nur im Rahmen der Psychotherapie-Richtlinien.

Precise starlight positions near the sun were measured during the 21 August 2017 total solar eclipse in order to measure their gravitational deflections. The equipment, procedures, and analysis are described in detail. A portable refractor, a CCD camera, and a computerized mount were set up in Wyoming. Detailed calibrations were necessary to improve accuracy and precision. Nighttime measurements taken just before the eclipse provided cubic optical distortion corrections. Calibrations based on star field images 7.4 deg on both sides of the sun taken during totality gave linear and quadratic plate constants. A total of 45 images of the sky surrounding the Sun were acquired during the middle part of totality, with an integrated exposure of 22 seconds. The deflection analysis depended on accurate star positions from the USNO's UCAC5 star catalog. The final result was a deflection coefficient L = 1.752 arcsec, compared to the theoretical value of L = 1.751 arcsec, with an uncertainty of only 3%., Comment: 21 pages, 11 figures, 6 tables. Submitted to Classical and Quantum Gravity

A compact refractor simplifies imaging stars during a total solar eclipse from remote, temporary locations. To achieve astrometric accuracy, cubic distortion terms were measured using hundreds of nighttime images. A detailed procedure is presented here, along with an example from a portable telescope. The results show that precisions down to the 20 mas level are possible with commercial equipment.

The aim of this study was to identify the causative factors of porcine ear necrosis syndrome (PENS) in 72 pigs, 5.5-10 weeks in age housed on nine farms. Biopsy samples of ear pinnae were collected from all piglets for bacteriology, histopathology and in situ hybridization for porcine circovirus type 2 (PCV2). At the same time, serum samples were taken for serological analysis and viral PCR, and feed was sampled for mycotoxin analysis. The initial lesion of PENS seemed to be a focal epidermal necrosis. Streptococci were isolated from 44 and staphylococci from 36 pinnae. PCV2 could not be detected by in situ hybridization or qPCR. Seven piglets were positive for porcine reproductive and respiratory syndrome virus, and one for Mycoplasma suis. One piglet had antibodies against Sarcoptes scabiei var. suis. No infectious agents were found in 15 samples. Positive virology and parasitology were often found alongside positive bacteriology. Deoxynivalenol, zearalenone and ergot alkaloids were detected in feed. The findings suggest that PENS is multifactorial in origin and that although infectious agents can be involved in the development of the syndrome they are not the exclusive triggering factor.

The aim of the study was to investigate the whole-body protein turnover, either before or after continuous, moderate ethanol-induced oxidative stress by red wine consumption over a relatively short period in healthy volunteers. Ten healthy adults received an individual regular diet over 20 days. After 10 days, the subjects consumed 0.4 ml ethanol kg(-1) day(-1) as red wine together with dinner over a 10-day period. After 8 and 18 days, respectively, a (15)N-labelled yeast protein was administered in a dosage of 4.2 mg kg(-1) body weight. Urine and faeces were collected over 48 h, respectively. The (15)N-enrichment was measured by isotope ratio mass spectrometry, whereas the protein flux rates were calculated by a three-compartment model. The whole-body protein turnover without/with red wine consumption amounted to 3.73±0.6 and 3.49±0.6 g kg(-1) day(-1) (not significant), respectively. Moderate alcohol consumption does not induce significant short-term changes in the whole-body protein turnover of healthy adults.

The sky brightness was measured during the partial phases and during totality of the 21 August 2017 total solar eclipse. A tracking CCD camera with color filters and a wide-angle lens allowed measurements across a wide field of view, recording images every 10 s. The partially and totally eclipsed Sun was kept behind an occulting disk attached to the camera, allowing direct brightness measurements from 1.5° to 38° from the Sun. During the partial phases, the sky brightness as a function of time closely followed the integrated intensity of the unobscured fraction of the solar disk. A redder sky was measured close to the Sun just before totality, caused by the redder color of the exposed solar limb. During totality, a bluer sky was measured, dimmer than the normal sky by a factor of 10,000. Suggestions for enhanced measurements at future eclipses are offered.

A pendulum inclinometer has been built and tested, suitable for measuring the deflection of the gravitational vertical to an accuracy of 1 μrad. The design is based on measuring the differential capacitance between a pendulum bob and two closely spaced parallel electrodes. Two independent pendulums are oriented orthogonally to measure both coordinates. A collimated optical beam is stably attached to the inclinometer pair and provides a means for making stellar measurements relative to the gravitational vertical. For optimum performance, the inclinometer is operated at its null position by supporting the entire assembly on a rigid tilting plate. Good repeatability is a key feature of this inclinometer.

Measuring the change in the optical alignment of a camera attached to a telescope is necessary to perform astrometric measurements. Camera movement when the telescope is refocused changes the plate constants, invalidating the calibration. Monitoring the shift in the optical axis requires a stable internal reference source. This is easily implemented in a Petzval refractor by adding an illuminated pinhole and a small obscuration that creates a spot of Arago on the camera. Measurements of the optical axis shift for a commercial telescope are given as an example.

A low‐voltage demonstration Tesla coil using a solid‐state photovoltaic relay to replace the conventional spark gap has been analyzed and then built. This relay incorporates an isolated LED to illuminate a silicon photovoltaic stack which drives a bidirectional FET. Component values for the inductances and capacitances have been determined theoretically from measured parameters. Computer simulation by integrating the coupled circuit equations shows excellent agreement with oscilloscope traces. Energy transfer between the primary and secondary circuits is demonstrated, along with continuous secondary oscillations after the primary circuit is interrupted. This low‐voltage design is easier to build and diagnose than high‐voltage Tesla coils.

Recombinant phages that carry the human smooth muscle (enteric type) gamma-actin gene were isolated from human genomic DNA libraries. The amino acid sequence deduced from the nucleotide sequence matches those of cDNAs but differs from the protein sequence previously reported at one amino acid position, codon 359. The gene containing one 5' untranslated exon and eight coding exons extends for 27 kb on human chromosome 2. The intron between codons 84 and 85 (site 3) is unique to the two smooth muscle actin genes. In the 5' flanking region, there are several CArG boxes and E boxes, which are regulatory elements in some muscle-specific genes. Hybridization with the 3' untranslated region, which is specific for the human smooth muscle gamma-actin gene, suggests the single gene in the human genome and specific expressions in enteric and aortic tissues. From characterized molecular structures of the six human actin isoform genes, we propose a hypothesis of evolutionary pathway of the actin gene family. A presumed ancestral actin gene had introns at least sites 1, 2, and 4 through 8. Cytoplasmic actin genes may have directly evolved from it through loss of introns at sites 5 and 6. However, through duplication of the ancestral actin gene with substitutions of many amino acids, a prototype of muscle actin genes had been created. Subsequently, striated muscle actin and smooth muscle actin genes may have evolved from this prototype by loss of an intron at site 4 and acquisition of a new intron at site 3, respectively.

The elimination of a hydrogen bond in imidazolium based ionic liquids which results in an increased melting point is investigated by means of static quantum chemical and molecular dynamics simulations.

Dependable systems must often detect, recover from, and tolerate faults. A common problem in the behavioural specification of such systems is that one cannot specify a response to faults without also specifying that faults must be able to occur, even though non-faulty systems are acceptable. Our solution is to adopt modal process logic, which allows one to distinguish between events of a specification that must be implemented and those that may be implemented. We describe the problem and illustrate the application of modal process logic to the verification of an industrial failure-recovery protocol.

GLINT (Geo Light Imaging National Testbed) is a program to image geo-synchronous satellites using Fourier telescopy. The design of the GLINT system requires knowledge of the reflectance properties of the satellites in certain specific wavelength ranges. Calibrated measurements of satellite brightness due to solar illumination can be made with a telescope. This report details such measurements and the data processing necessary to yield curves of normalized satellite return versus phase angle in given wavelength ranges. These measurements can be used to check the accuracy of satellite reflectivity models.

A wavefront control system will be employed on NIF to correct beam aberrations that otherwise would limit the minimum target focal spot size. For most applications, NIF requires a focal spot that is a few times the diffraction limit. Sources of aberrations that must be corrected include prompt pump-induced distortions in the laser slabs, thermal distortions in the laser slabs from previous shots, manufacturing figure errors in the optics, beam off-axis effects, gas density variations, and gravity, mounting, and coating-induced optic distortions.

We report the latest progress on the design, fabrication and testing of the adaptive secondary mirror to be used in the adaptive optics system to for the 6.5m upgrade to the Steward Observatory's MMT. The adaptive secondary will use electromagnetic force actuators in conjunction with a rigid reference structure to deformed a thin and flexible glass facesheet. The facesheet is fabricate with figure accuracy comparable to the surface of a traditional static secondary mirror. The flexible facesheet can however, be deformed by the actuators to conjugate the changing atmospheric aberration. Capacitive position sensors are placed at each actuator and are used to rapidly measure the position of the glass facesheet relative to the rigid reference structure. These measurements are used as feedback in a servo control- loop which maintains the desired figure of the adaptive secondary facesheet. In the proposed design the mechanical interface between the facesheet and the reference structure is limited to a small hub in the center of the facesheet. Due to heat dissipation in the electromagnetic voice-coils a temperature control system is required to maintain the facesheet of the adaptive secondary near the ambient temperature of the atmosphere. We report on laboratory test of a nearly full size 60 actuator adaptive secondary prototype. We include test of actuator stroke and position accuracy, control-loop stability, and closed-loop bandwidth.

The Multiple Mirror Telescope on Mt. Hopkins will soon be upgraded to a single 6.5 m primary mirror.An adaptive- optical system, featuring a thin-shell, adaptive-secondary mirror with 330 voice-coil actuators is being developed for this new telescope. The thin-shell mirror is supported by a thick, concave aluminum substrate which also holds the actuator control and monitoring electronics and serves as the reference surface. With the actuator electronics dissipating heat into the substrate, the thermal behavior of the aluminum reference plate becomes as important issue. This paper presents results form tow experiments designed to determine the thermal behavior of the reference plate.

The Multiple Mirror Telescope (MMT) is now being replaced by a single 6.5m telescope which will have an integral adaptive optics system optimized for near IR operation. We illustrate key results obtained with low-order adaptive optics at the MMT and report on progress on the major components of the system for the new telescope. We also give a brief update on the status of the telescope itself. First light for the adaptive system is expected in mid 1999.

The upgraded 6.5 m MMT in Arizona will use an adaptive secondary to optimize performance in the near infrared spectral region. The secondary mirror is a 2 mm thick, 640 mm diameter Zerodur shell suspended only by a flexible center hub. Three hundred voice coil actuators installed in an aluminum reference surface deform the shell according to commands from a wavefront sensor. Capacitor position sensors surrounding each actuator provide feedback in an inner servo loop, much faster than the exterior wavefront sensor control bandwidth. A 60 actuator prototype, nearly identical to the final adaptive secondary size, has been built and is currently being tested.

The new 6.5 m single mirror multiple mirror telescope (MMT) will be equipped with adaptive optics capabilities to enhance high resolution infrared astronomy. Before we build the 64 cm diameter adaptive secondary, we fabricated a smaller prototype mirror. The adaptive secondary uses voice coil force actuators with an average spacing of 30 mm. Surrounding each actuator is an analog capacitor position sensor operating in a digital closed loop at 10 kHz. This allows the force actuators to be controlled as if they were position actuators. The adaptive secondary configuration and performance test results are presented, followed by the changes to be incorporated into the next curved shell prototype.

ThermoTrex Corporation has designed and built a prototype of the fast steering mirror to be used for image motion control in the TNG adaptive optics system. The principal characteristic of this mirror is the use of voice coil actuators whose positions are controlled with closed loops based on capacitive sensors. Here we report the main features of the mirror assembly and laboratory measurements done to characterize the mirror behavior. The Bode diagram of the mirror is reported and discussed.© (1997) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

An unusual dual-aperture 28.5-inch, f/21 Ritchey-Chretien telescope has been completed and will be installed in the recently upgraded University of Denver extreme high altitude observatory facility, atop 14,268 ft. Mount Evans in Colorado. Designed to optimize high spatial resolution imaging, the Meyer binocular telescope incorporates active thermal management of the telescope structure. The secondary mirror support elements are fabricated from INVAR and permit active tip-tilt and focusing capability. The optics were fabricated from Zerodur by Contraves USA, and each system has a measured total wavefront error less than 0.050 lambda at 633 nm. All optical surfaces are coated with a multi- layer dielectric enhanced silver, providing high reflectance from below 350 nm to beyond 26 micrometer. The telescope control system has been designed to allow initial operation from an insulated control room. Long-term plans call for totally remote operation from the University of Denver campus via direct microwave radio link. Instrumentation planned for the telescope at first light includes: (1) a low order 400 nm to 1,000 nm band adaptive optics system (AO5: adaptive optics, 5 mode) equipped with a large format CCD camera; (2) a mid-infrared array camera (TNTCAM: ten and twenty micron camera); and (3) a mid-IR moderate dispersion spectrometer (TGIRS: two grating IR spectrometer). Some of the science problems the dual aperture telescope is uniquely situated to tackle include the study of planetary atmosphere, detection of planetary systems around nearby stars and the analysis of evolutionary changes in stars. The Mount Evans site (at 4,303 meters elevation, the highest operating astronomical facility in the world) is located 70 km west of Denver and can be reached via a paved state highway which extends all the way to the summit. The observatory is currently under construction with installation of the telescope planned for late summer 1996.

The Center for Astronomical Adaptive Optics (CAAO) at the University of Arizona is developing a diffraction-limited adaptive optics (AO) system at infrared wavelengths utilizing a sodium laser guide star. This system (Lloyd-Hart et al., this conference), based on an adaptive secondary mirror with 300 actuators, will be placed in operation following the installation of the 6.5 m mirror upgrade at the Multiple Mirror Telescope (MMT) mount. As an interim step, we have built an adaptive optics system which provides tip-tilt correction for each of the 6 individual beams of the current MMT. This instrument, called FASTTRAC II, will produce a combined image at the diffraction limit of the 1.8 m primary mirrors (≲0.3″ at 2.2 μm) yielding moderately high resolution images in the near infrared. The current system incorporates the design philosophy of the 6.5 m system and provides a testbed for development of the system components in addition to serving as a significant scientific instrument in its own right.

A low order adaptive optics system for astronomical telescopes based on simple optics and commercially available key components can serve as more than an introduction to adaptive optics hardware and testing. For a one meter telescope, in the case of (D/r0) between about five and eight, only five correction orders are required to produce significantly improved images. Such a low order system has been designed and built, using translating lenses to produce smooth aberration corrections. The system, called the AO-5, is meant to correct atmospheric turbulence in the visible and near infrared spectral regions. This paper reports on measurements of the corrections applied to synthesized atmospheric aberrations created by a turbulence generator. The AO-5 will installed in the summer of 1996 on one of the Meyer Foundation's dual 0.72 m Ritchey-Cretién telescopes on the 4300 meter level of Mount Evans, Colorado.

We present a novel, high performance, and economical design for tip-tilt mirrors. The two- dimensional tilt of each mirror is sensed through capacitive displacement sensors sensitive to approximately 1 nm rms out to 10 KHz. An analogue PID circuit utilizes this positional feedback to lock the mirrors to the commanded tilt via voice coil drivers. These mirrors achieve a 10 - 90% risetime of 3.0 ms and have a critically damped response at 100 - 150 Hz update rates. We have incorporated six of these tip-tilt mirrors to adaptively combine all six beams from the MMT. During first light of the instrument in April 1995, individual beams improved from 1.1 inch to 0.6 inch FWHM in 60 s exposures corrected with 60 Hz update rates.

A new adaptive optics system has been constructed for moderately high resolution in the near infrared at the Multiple Mirror Telescope (MMT). The system, called FASTTRAC II, has been designed to combine the highest throughput with the lowest possible background emission by making the adaptive optical element be an existing and necessary part of the telescope, and by eliminating all warm surfaces between the telescope and the science camera's dewar. At present, only natural guide stars are supported, but by the end of 1995, we will add the capability to use a single sodium resonance beacon derived from a laser beam projected nearly coaxially with the telescope. In this paper, we present a description of FASTTRAC II, and show results from its first test run at the telescope in April 1995.© (1995) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

We present an overview of the new adaptive system under development for the conversion of the Multiple Mirror Telescope (MMT) to a 6.5 m continuous primary mirror. The system is optimized for diffraction-limited imaging from 1.6 to 2.2 micrometer wavelength, using an adaptive secondary mirror which directly feeds an infrared science detector at f/15 Cassegrain focus. Nearly full sky coverage will be obtained using a low-power, continuous wave (cw) sodium laser beacon to sense high-order wavefront errors, with image motion sensing using a quadrant detector sensitive to infrared field star photons in the 1.2 - 1.6 micrometer band. Components are currently under development, so that the adaptive instrument can be integrated with the new 6.5 m telescope soon after first light.

In 1996, the Multiple Mirror Telescope will be replaced with a 6.5 m single primary mirror. Development is currently underway on a sodium laser guide star adaptive optical system for the new telescope. One unique feature will be an adaptive secondary mirror, consisting of 320 individually controlled voice coil actuators on the back side of a thin, 64 cm diameter mirror. This paper describes initial tests on a 15 cm diameter, thin, flat prototype mirror with a single actuator. The thin mirror is held near a thick substrate which also serves as an immovable reference surface. A novel voice coil actuator connects the two glass parts. A custom capacitance sensor surrounding the voice coil actuator measures the absolute distance between the mirror back side and the reference surface. This prototype provides detailed performance measurements, including temporal and spatial actuator response functions. Assembly, alignment, and calibration techniques for the 64 cm mirror will be debugged. The data will help optimize the design and performance of the adaptive secondary.

The new 6.5 m single mirror Multiple Mirror Telescope (MMT) will be equipped with adaptive optics capabilities. In particular, high resolution infrared astronomy will use a new adaptive secondary on a regular basis. Before we design the adaptive secondary in detail, we fabricated a smaller prototype mirror using similar actuators and actuator geometry. The prototype's purpose is to debug the components and allow comparisons with theoretical predictions. We are studying system interactions and looking for unexpected performance characteristics. Manufacturing techniques and reliability are also being tested, to reduce risks when building the adaptive secondary.

An adaptive optics system for small to medium astronomical telescopes has been designed and is under construction. This adaptive optics system corrects the five lowest order Zernike wavefront aberrations, providing near diffraction-limited performance for telescope diameters smaller than about 5*ro, and useful correction up to about 10*ro. This adaptive optics system design consists of a lens-based wavefront aberrator, a CCD-based Shack-Hartmann wavefront sensor, and a personal computer-based feedback loop.© (1994) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Wilms' tumor is a childhood nephroblastoma that is postulated to arise through the inactivation of a tumor suppressor gene by a two-hit mechanism. A candidate 11p13 Wilms' tumor gene, WT1, has been cloned and shown to encode a zinc finger protein. Patients with the WAGR syndrome (Wilm's tumor, aniridia, genitourinary abnormalities, and mental retardation) have a high risk of developing Wilms' tumor and they carry constitutional deletions of one chromosome 11 allele encompassing the WT1 gene. Analysis of the remaining WT1 allele in a Wilms' tumor from a WAGR patient revealed the deletion of a single nucleotide in exon 7. This mutation likely played a key role in tumor formation, as it prevents translation of the DNA-binding zinc finger domain that is essential for the function of the WT1 polypeptide as a transcriptional regulator.

Using somatic cell genetics and Southern blot hybridization, we have mapped five structural genes in the owl monkey, coding for catalase (CAT), the β-globin gene cluster (HBBC), c-Ha-ras 1 (HRAS1), insulin (INS), and parathyroid hormone (PTH). All five loci are mapped to chromosome 19 of karyotype VI (2n = 49,50) of the owl monkey; CAT, HBBC, INS, and PTH can be assigned to chromosome 4 of karyotype V (2n = 46), while CAT and HBBC can be assigned to chromosome 2 of karyotype III (2n = 53). Using in situ hybridization, the CAT gene was precisely mapped on the mid-region and the β-globin gene cluster on the telomeric end of chromosome 2q(K-ΠI). Our results provide significant insight into the evolutionary history of these gene loci. While these loci are separated into at least two major segments in rodents such as the mouse, our results suggest conservation of a single chromosome arm among higher primates.

Two-phonon Raman spectra have been measured for solid-argon samples at two densities at low temperature. These results are compared with published calculations based on a point-dipole model, and some shortcomings of this model are indicated. The development of the Raman spectra with increasing temperature in the solid at constant density has been studied, and the results discussed in the context of this model. Finally, spectra were measured for solid and fluid argon at a number of points along the melting curve at pressures up to 4 kbar, in order to explore the changes which occur upon melting. These results are compared with previously published data for fluid argon at other temperatures and pressures. Some comparisons with molecular-dynamics calculations are also made.

Mit Hilfe der kinetischen Methode der Auflosungsge schwindigkeiten nach Karsten wurden die Losungsgleichgewichte im Sylvin/Steinsalz- und Carnallit/Steinsalz-Feld des quinaren Systems der ozeanischen Salzablagerungen bei Magnesiumchlorid-Konzentrationen von 0 bis 100 Mol und Magnesiumsulfat-Konzentrationen von 0 bis 10 Mol auf 1000 Mol Wasser bei 20°C genauer als mit der bisher ublichen stationaren Ruhrmethode nach J. H. van't Hoff ermittelt und in Rasterdiagrammen dargestellt. Im Carnallit-Feld wurden auch metastabile Losungszustande erfast.

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