This study aims to validate the Multiple Sclerosis (MS) International Quality of Life (MusiQoL) questionnaire, a multi-dimensional, self-administered questionnaire, available in 14 languages, as a disease-specific quality of life scale that can be applied internationally. A total of 1992 patients with different types and severities of MS from 15 countries were recruited. At baseline and day 21 +/- 7, each patient completed the MusiQoL, a symptom checklist and the short-form (SF)-36 QoL questionnaire. Neurologists also collected socio-demographic, MS history and outcome data. The database was randomly divided into two subgroups and analysed according to different patient characteristics. For each model, psychometric properties were tested and the number of items was reduced by various statistical methods. Construct validity, internal consistency, reproducibility and external consistency were also tested. Nine dimensions, explaining 71% of the total variance, were isolated. Internal consistency and reproducibility were satisfactory for all the dimensions. External validity testing revealed that dimension scores correlated significantly with all SF-36 scores, but showed discriminant validity by gender, socio-economic and health status. Significant correlations were found between activity in daily life scores and clinical indices. These results demonstrate the validity and reliability of the MusiQoL as an international scale to evaluate QoL in patients with MS.

Regulation of the initial phase of embryo implantation may involve the recognition interplay of glycoconjugates and respective receptors such as endogenous lectins on both cellular surfaces. Whereas changes in glycoconjugate composition have been detected in preparation for embryo implantation and described in detail, knowledge on endogenous lectins has remained scant. Affinity probes (carrier-immobilized carbohydrate structures as ligand part on a histochemically inert backbone) are used in the present investigation in order to gain further insights in this area. Cryostat sections of rabbit Fallopian tubes and uteri in nonpregnant and early pregnant [tubes: 3 days post coitum (d p.c.); uteri: 3, 5, 7 and 9 d p.c.] states were studied for binding patterns of a series of biotinylated (neo)glycoproteins. A high density of binding sites was detected with beta-galactosides (with decreasing intensity: beta-D-galactose-BSA, asialofetuin with its triantennary glycan chains, lactose-BSA). Considerably less binding (but with the same pattern) was obtained with beta-N-acetyl-D-glucosaminide-BSA and is interpreted to originate from a cross-reactivity of such sites which may bind physiologically to Gal-beta1,3/4-GlcNAc sequences. In contrast, no evidence for the presence of binding molecules with specificities for a-D-mannose-BSA, maltose-BSA, N-acetyl-galactosaminide-BSA and N-acetyl-D-neuraminic acid-BSA was obtained in these tissues under the same conditions. The epithelium of the Fallopian tube showed a high density of beta-galactoside-binding sites at the apical cell poles (including the cytoplasm and membrane region) already in the nonpregnant state. At 3 d p.c., a strong reaction in all epithelial cells of the isthmus and a marked decrease in the ampulla were noted. The putative lectin(s) appear(s) to be synthesized and secreted by the tubal epithelium. A physiological role in forming the mucoprotein layer of the blastocyst coverings by precipitating the appropriate mucin-type molecules can be considered. Within the endometrium, the beta-galactoside-binding molecules were almost exclusively localized at the apical cell pole of epithelial cells, whereas there was hardly any binding in the epithelial cytoplasm or in the endometrial stroma. The reaction was very weak in the non-pregnant state but increased considerably until 5 d p.c., starting in the luminal-most parts of the epithelium. While the reaction was rather homogeneous at the surface of the luminal epithelium at 5 d p.c., the degree of heterogeneity increased stepwise from 7 to 9 d p.c. In the implantation chamber, the density of these beta-galactoside-specific 'receptors' was further enhanced in particular at the epithelial surface of the placental folds. In contrast, the reaction was less intense at the antimesometrial uterine epithelium and in interblastocyst segments of the uterus, and it remained weak in the middle and deep crypts. The trophoblast showed a high density of galactoside-binding sites at its surface, and less in the cytoplasm. Neoglycoprotein binding to the blastocyst coverings observed at 7 d p.c. was strong in particular at the outer and inner surfaces. Physical factors (e.g. differential texture at surfaces) are discussed to influence the staining patterns of these extracellular coverings. Nevertheless, the observations made on the tubal and the uterine mucosa suggest that the putative lectin(s) detected here is (are) secreted by these epithelia and could be involved in the structural organization of the various layers of the blastocyst coverings with their remarkable content of oligosaccharide chains. This effect on topological aspects of the zona pellucida equivalents may be important for the interplay between trophoblast and uterine epithelium and the cascade leading to implantation initiation.

An explanation is proposed for the observed and often discussed clustering of long-period comet aphelia on the sky. Poisson and several multinomial distributions are applied to the most conspicuous cluster, considering only the 80 "new" and 59 "intermediate" comets with the best-determined orbits. The observed number of aphelion points in adjacent areas in two tests with 24 and 36 equal sky areas, respectively, shows a large deviation from a random distribution. The expected probability frequency for this to happen by chance is <0.1% for the "new" comets alone; it is further reduced when "new" and "intermediate" comets are combined. When these comets are analyzed separately from others, it is found that the clustering is the result of perturbations of their original orbits by the passage of a star, or a stellar system, through Oort's cloud a few million years ago. Because the statistical effect on the change of a comet's angular momentum about the sun is proportional to the square of the ratio of the mass to the velocity of a star relative to the sun, it is a priori probable that passages by a few stars should produce clustering of the aphelia, as is discussed in detail.

The different methods of labeling blood cells, in particular erythrocytes and platelets, for survival studies are reviewed. Besides the technical information about these procedures, attention is also paid to the indications of blood cell survival studies, the effective dose equivalent involved and the interpretation of the resulting data. In the final section the possibilities created by dual-labeling procedures are discussed.

Before entering the subject of magnetohydrodynamic dissipation we comment briefly on the question of thesupplyof kinetic energy to the interstellar gas. This topic has been considered in the 1953 Symposium by Schlüter and myself, and also by Oort. As had been pointed out already by Spitzer in Paris, 1949, the visible HII regions, owing to their excess pressure as compared with the HI regions and the dilute HII regions, must be assumed to expand with a velocity of the order of 10 or 20 km/sec. By this expansion part of the radiation energy of the star is converted into kinetic energy. It was estimated (p. 153 of the proceedings) that a typical HII region around a BO star feeds 1035ergs/sec to the instellar gas, and that the number of these regions is such, that each region has to provide kinetic energy on the average to 1036−1037g of interstellar material. Thus a value of 10−2−10−1erg g−1sec−1was found (which corresponds to 10−26−10−25erg cm−3sec−1, assuming 10−24g/cm3for the mean density of the interstellar material in the disk).

AbstractEs wird im Gegensatz zu der Ansicht von F. Schmeidler hervorgehoben, daß Konvektion bei thermisch stabiler Schichtung (unteradiabatischem Temperaturgradienten) nur durch ständige zusätzliche Zufuhr mechanischer Energie stationär aufrecht erhalten werden kann, deren Betrag proportional ist der Energie, welche zur Aufrechterhaltung des thermischen Gleichgewichts (welches infolge der Vergrößerung des Temperaturgradienten durch die Konvektion sonst gestört würde) konvektiv nach innen transportiert werden muß; wenn die Konvektion einen stationären Temperaturgradienten nahe unterhalb des adiabatischen erzwingt, so wird dieser erzwungene Energiefluß nach innen hin vergleichbar dem Strahlungsenergiefluß nach außen (wenn er auch natürlich kleiner bleibt). Die genauere Diskussion ergibt, daß pro Schicht einer Mächtigkeit der sogenannten homogenen Dicke ein Betrag von der Ordnung von 2/5 des nach außen fließenden Nettoenergiestromes in mechanische Energie umgesetzt werden muß. Andererseits haben neuere Untersuchungen über die (akustische) Abstrahlung mechanischer Energie aus Konvektionszonen (von Lighthill u. a.) ergeben, daß die so abgestrahlte mechanische Energie proportional einer höheren Potenz der der Turbulenz zugeordneten Machzahl ist; die letztere ist aber im Sterninnern stets klein gegen 1. Daher kann die stationäre Turbulenz einer Instabilitätszone höchstens eine nur begrenzte Nachbarzone im stabilen Bereich in Mitleidenschaft ziehen; die Unschärfe der Begrenzung von Konvektionszonen im Sterninnern ist daher höchstens vergleichbar mit der homogenen Schichtdicke. Die dem normalen Spektralgesetz der Turbulenz zugrunde liegenden Voraussetzungen gelten (wie auch Schmeidler bemerkt) für gegen stabile Schichtung erzwungene Turbulenz insofern nicht, als die Bewegungsenergie zur Hauptsache in gegen die Stabilität der Schichtung zu leistende Arbeit übergeht.Im speziellen Fall der Sonne zeigt sich außerdem, daß bei vollständig konvektivem Aufbau sich die Mittelpunktsdichte zu 8.5 g/cm3 ergeben würde und die Mittelpunktstemperatur höchstens zu 8.7 Millionen Grad (dieser Wert entspricht einem Molekulargewicht von 0.7), also viel zu niedrig für die energieliefernden Kernreaktionen. Ein Vergleich mit dem an die Beobachtung angeschlossenen Druck‐Dichteverlauf der oberflächennahen Schichten zeigt außerdem, daß dieser an das vorerwähnte Modell nicht angeschlossen werden kann. Zu dem Schluß, daß die Wasserstoffkonvektionszone der Sonne nicht tiefer als bis zu T ≈ 3·106 Grad reichen kann, führen auch die Beobachtungen über die Häufigkeit der gegen Kernreaktionen empfindlichen Elemente Lithium und Beryllium.

Astronomische NachrichtenVolume 279, Issue 5-6 p. 237-237 Article Bemerkung zu vorstehender Arbeit L. Biermann, L. Biermann GöttingenSearch for more papers by this author L. Biermann, L. Biermann GöttingenSearch for more papers by this author First published: 1951 https://doi.org/10.1002/asna.19512790506AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinkedInRedditWechat No abstract is available for this article. Volume279, Issue5-61951Pages 237-237 RelatedInformation

Astronomische NachrichtenVolume 266, Issue 1 p. 1-6 Article Leuchtkraft und Konvektion bei Sternmodellen mit sehr starker Konzentration der Energiequellen L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author First published: 1938 https://doi.org/10.1002/asna.19382660102Citations: 1AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinkedInRedditWechat Citing Literature Volume266, Issue11938Pages 1-6 RelatedInformation

Astronomische NachrichtenVolume 267, Issue 8 p. 131-136 Article Über die Zahl der Freiheitsgrade von Sternmodellen L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author First published: 1938 https://doi.org/10.1002/asna.19382670804Citations: 1AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onEmailFacebookTwitterLinkedInRedditWechat References p131_1) AN 257. 269 (1935) und Google Scholar AN 264. 361 (1938), im folgenden zitiert als K I und K II. Google Scholar p131_2) AN 258. 133 (1936); Google Scholar MN 98. 528 (1938). Google Scholar p133_1) MN 98 l. c. Das in den einleitenden Bemerkungen dieser Arbeit von Cowling wiedergegebene Argument des Verfassers ist das in K I benutzte, nicht das von K II (vgl. K II p. 394 und die weiteren Ausführungen oben). – Zu der vorliegenden Arbeit schreibt mir Herr Dr. Cowling in einem Brief, den ich mit seiner freundlichen Erlaubnis hier zitiere, daß er sich in allgemeiner Übereinstimmung mit dem hier eingenommenen Standpunkt befindet, wobei er weitere Untersuchungen für notwendig hält, bevor wirklich eindeutige Schlußfolgerungen über dne Einfluß von Rotation und Deformation erreicht werden können. Google Scholar p133_2) Für die Behandlung des Randwertproblems läßt sich die Funktion p R (P) getrennt untersuchen. Vgl. hierzu Biermann, Z f Ap 3. 116 (1931). Google Scholar p133_3) Z f Ap 5. 117 (1932). Für neuere Mitteilungen hierzu bin ich Herrn Prof. E. Schmidt zu Dank verpflichtet. PubMedGoogle Scholar p133_4) Hierauf hat mich Herr Dr. Cowling freundlicherweise hingewiesen. Google Scholar p133_5) In K II war ihm vielleicht noch zuviel Gewicht beigemessen. Google Scholar p135_1) Ich glaube, daß ich diese Formulierung des Arguments Herrn Prof. Siedentopf verdanke. Google Scholar p135_2) Z f Ap 15. 315 (1938). Google Scholar p135_3) MN 91. 251, 501, 756 (1931). Google Scholar p135_4) Vgl. Kreiken, l. c. p. 757–758. Herrn. Dr. Klauder bin ich für Bemerkungen zu diesem Punkt dankbar. Google Scholar p135_5) Siehe etwa Klauder, AN 250. 89 (1933). Google Scholar p135_6) Biermann, AN 258. 257 (1936) und Google Scholar AN 266. 1 (1938). Google Scholar Citing Literature Volume267, Issue81938Pages 131-136 ReferencesRelatedInformation

Astronomische NachrichtenVolume 264, Issue 22-24 p. 395-398 Article Zur Theorie der Granulation und der Wasserstoffkonvektionszone der Sonne L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author L. Biermann, L. Biermann Sternwarte Berlin-BabelsbergSearch for more papers by this author First published: 1937 https://doi.org/10.1002/asna.19372642203Citations: 10AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinkedInRedditWechat No abstract is available for this article.Citing Literature Volume264, Issue22-241937Pages 395-398 RelatedInformation

Astronomische NachrichtenVolume 258, Issue 15 p. 257-264 Article Über Sternmodelle mit der Energieerzeugung ϵ ∼ T L. Biermann, L. Biermann Universitäts-Sternwarte, JenaSearch for more papers by this author L. Biermann, L. Biermann Universitäts-Sternwarte, JenaSearch for more papers by this author First published: 1936 https://doi.org/10.1002/asna.19362581502Citations: 1AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinked InRedditWechat Citing Literature Volume258, Issue151936Pages 257-264 RelatedInformation

Astronomische NachrichtenVolume 257, Issue 17-18 p. 269-294 Article Konvektion im Innern der Sterne L. Biermann, L. Biermann Universitäts Sternwarte, JenaSearch for more papers by this author L. Biermann, L. Biermann Universitäts Sternwarte, JenaSearch for more papers by this author First published: 1935 https://doi.org/10.1002/asna.19352571702Citations: 8AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinked InRedditWechat Citing Literature Volume257, Issue17-181935Pages 269-294 RelatedInformation

Before presenting a summary of the work on con- trolled thermonuclear fusion in the Federal Republic of Germany, I should like to make some general comments about the scope and background of this work Soon after the first Geneva Conference on the Peace- ful Uses of Atomic Energy, physicists m a number of scientific institutions m Western Germany began to give serious attention to the potential possibilities of controlled fusion The advantages of thermonuclear devices and of using magnetic fields for containing the hot charged particles were realized very early It was natural, therefore, that both experimental physicists with experience in the physics of gaseous discharges, plasmas and theoretical astrophysicists with their acquaintance with magnetohydrodynamics and with the propagation of cosmic rays m cosmic magnetic fields, started to think about how a plasma with the required high temperature could be controlled I may say that the closest connections to our work are to be found, perhaps, in the developments at Princeton and at Harwell Experiments on high current discharges at Gottingent and Aachen î are as yet on a fairly small scale as compared with some of the other experiments described at this conference, although experiments with toroidal discharges, suitable exterior magnetic fields, and large diameters ranging between 40 cm and 1 m, have also been considered at Aachen and Gottingen