On the Nature of Rheumatoid Rice Bodies

The nature of rice bodies was studied, utilizing histochemistry, immunofluorescence, and scanning and transmission electron microscopy. Rice bodies were found to consist primarily of fibrous material, most of which was fibrin with small amounts of collagen. Channels containing a variety of viable cells permeated the rice bodies. Blood vessels occurred in a few rice bodies indicating a former connection with the synovial membrane. Nonvascularized rice bodies might represent a further degeneration of the vascular type. Rice bodies seem to be a nonspecific response to inflammation.     

Trachyandesitic volcanism in the early Solar System

Volcanism is a substantial process during crustal growth on planetary bodies and well documented to have occurred in the early Solar System from the recognition of numerous basaltic meteorites. Considering the ureilite parent body (UPB), the compositions of magmas that formed a potential UPB crust and were complementary to the ultramafic ureilite mantle rocks are poorly constrained. Among the Almahata Sitta meteorites, a unique trachyandesite lava (with an oxygen isotope composition identical to that of common ureilites) documents the presence of volatile- and SiO₂-rich magmas on the UPB. The magma was extracted at low degrees of disequilibrium partial melting of the UPB mantle. This trachyandesite extends the range of known ancient volcanic, crust-forming rocks and documents that volcanic rocks, similar in composition to trachyandesites on Earth, also formed on small planetary bodies ∼4.56 billion years ago. It also extends the volcanic activity on the UPB by ∼1 million years (Ma) and thus constrains the time of disruption of the body to later than 6.5 Ma after the formation of Ca–Al-rich inclusions.A large number of planetary embryos, tens to hundreds of kilometers in size, accreted within the early Solar System. In some of these embryos, internal heating triggered melting and differentiation, giving rise to a varied suite of lithologies as documented by the achondritic meteorites. Planetary crustal growth occurs via both volcanic eruptions and plutonic intrusions. Constraining these processes and the diversity of crustal materials that formed the outermost solid shell of planetary bodies is crucial for understanding Solar System planetary processes and evolution.Ureilites are among the most common achondrites and represent remnants of the mantle from a planetary body from which magmas have been extensively extracted (1–4). Several details of ureilite petrogenesis (e.g., the mode of melt extraction) remain controversial (e.g., refs. 1 and 2) because crustal rocks from the ureilite parent body (UPB) have not yet been discovered. Although tiny remnants of feldspathic and felsic melts from ureilitic breccias have been interpreted as UPB basalts or products of partial melting of plagioclase-bearing cumulates (e.g., refs. 5 and 6), it is generally assumed that the complementary melts were lost to space during explosive eruptions (e.g., refs. 7–9).A unique opportunity to gain new insights into ureilite petrogenesis was provided by the polymict asteroid 2008 TC₃ that impacted our planet October 7, 2008, in the Nubian Desert, Sudan, containing various ureilitic and ureilite-related fragments (10, 11). Among its remnant fragments collected in the strewn field, collectively named the “Almahata Sitta” meteorites, the sample ALM-A (Almahata Sitta trachyandesitic meteorite) was recovered (12). ALM-A weights 24.2 g and is covered with a greenish and shiny fusion crust (Fig. 1).Open in a separate windowFig. 1.(A) Greenish ALM-A hand specimen, (B) overview of the ALM-A thin section (polarized light, crossed nicols) showing high abundances of feldspar (mainly gray) and displaying a subdoleritic texture. Anhedral anorthoclase and subhedral, zoned plagioclase laths occur. Low-Ca and Ca pyroxene (both colored) are frequently encountered. (C) Close-up backscattered electron image illustrating the textural relation of feldspar (Fsp) and pyroxenes (Cpx, Ca rich; Px, low Ca). Ca pyroxene bears abundant inclusions of, e.g., feldspar and SiO₂-rich glass. Cl apatite (Ap) is developed as laths. (D) Quartz-normative, alkali-rich glass inclusions occur within large Ca pyroxene crystals (arrows; polarized light).The ALM-A sample described here is the only SiO₂-rich, rapidly cooled volcanic rock among the meteorites in our collections. This rock is texturally completely different from the felsic achondrite Graves Nunatak (GRA) 06128/9 (13) and granitic lithologies that occur as fragments in meteorite breccias (14). GRA 06128/9 shows a plutonic, granoblastic texture, 120° triple junctions between coexisting phases, and chemically equilibrated silicates (13). ALM-A clearly demonstrates that SiO₂-rich lavas were formed on the UPB and sets new important constraints on ureilite petrogenesis.     

Secondary Central Nervous System Lymphoma

This review summarizes current knowledge of secondary central nervous system lymphoma (SCNSL) in adults. We define SCNSL as CNS involvement not obvious at the initiation of treatment for systemic lymphoma. Recently, polymerase chain reaction and flow cytometry assays of cerebrospinal fluid have become available for the correct diagnosis of SCNSL. We reviewed reports of patients treated without CNS prophylaxis to evaluate the incidence of SCNSL. Elevated serum lactate dehydrogenase levels, the involvement of more than one extranodal site, an advanced stage, a high age-adjusted International Prognostic Index score at presentation, and special anatomic sites of involvement such as the testis are important risk factors for SCNSL. Histologic evidence of aggressiveness is generally an indicator of risk for SCNSL. In addition to conventional treatment, stem cell transplantation, intrathecal administration of rituximab, and liposomal cytarabine have come into clinical use for the treatment of established SCNSL. Prevention of isolated CNS recurrence is thought to be the main target of CNS prophylaxis. The value of CNS prophylaxis according to histologic subtype, status of systemic lymphoma, and other risk factors is summarized. Although prophylaxis is fundamental for treating highly aggressive non-Hodgkin's lymphoma (NHL), it is beginning to be appreciated for the treatment of aggressive NHL. CNS involvement is almost always fatal; however, a CNS-active strategy could complement other approaches that have led to recent improvements in the prognosis for lymphoma.     

On the Distribution of Red Cell Volumes

A large number of red cell volume distribution curves can be generated onthe same sample of blood by manipulating the length of the Coulter Counteraperture and the shape of the red cell. Curves derived from sphered red cellsflowing through an aperture 70 x 98µ long, or longer appear to be relativelyfree from artefacts and therefore the most likely to be "real."

The use of long apertures to size sphered red cells will give a volume distribution curve that is approximately Gaussian and with a mean that is largerelative to the variance. Whether red cells are Gaussian or log normal in theirvolume distribution is very difficult to determine. On a particle populationwhere volumes are controlled as closely as on red cells (i.e. with such a lowvariance), the normal and the log normal distributions become practicallyindistinguishable. If in the future this decision can be reached by some independent means, then the volume distributions using the Coulter volume transducer can be easily and simply fitted to the shape desired by appropriatemanipulation of aperture length. These ideal volume distribution curves arenot likely to differ markedly from those obtained under the conditions suggested in this paper. For the present, use of a 70 x 98µ aperture to size redcells sphered by suspension in isotonic Sodium Potassium Tartrate will contribute to considerably greater accuracy in identification of red cell subpopulations in abnormal blood.

Submitted on July 28, 1967 Accepted on October 7, 1967     

Cosmochemistry: Understanding the Solar System through analysis of extraterrestrial materials

Cosmochemistry is the chemical analysis of extraterrestrial materials. This term generally is taken to mean laboratory analysis, which is the cosmochemistry gold standard because of the ability for repeated analysis under highly controlled conditions using the most advanced instrumentation unhindered by limitations in power, space, or environment. Over the past 40 y, advances in technology have enabled telescopic and spacecraft instruments to provide important data that significantly complement the laboratory data. In this special edition, recent advances in the state of the art of cosmochemistry are presented, which range from instrumental analysis of meteorites to theoretical-computational and astronomical observations.     

Exoplanet orbital eccentricity: Multiplicity relation and the Solar System

The known population of exoplanets exhibits a much wider range of orbital eccentricities than Solar System planets and has a much higher average eccentricity. These facts have been widely interpreted to indicate that the Solar System is an atypical member of the overall population of planetary systems. We report here on a strong anticorrelation of orbital eccentricity with multiplicity (number of planets in the system) among cataloged radial velocity (RV) systems. The mean, median, and rough distribution of eccentricities of Solar System planets fits an extrapolation of this anticorrelation to the eight-planet case rather precisely despite the fact that no more than two Solar System planets would be detectable with RV data comparable to that in the exoplanet sample. Moreover, even if regarded as a single or double planetary system, the Solar System lies in a reasonably heavily populated region of eccentricity−multiplicity space. Thus, the Solar System is not anomalous among known exoplanetary systems with respect to eccentricities when its multiplicity is taken into account. Specifically, as the multiplicity of a system increases, the eccentricity decreases roughly as a power law of index –1.20. A simple and plausible but ad hoc and model-dependent interpretation of this relationship implies that ∼80% of the one-planet and 25% of the two-planet systems in our sample have additional, as yet undiscovered, members but that systems of higher observed multiplicity are largely complete (i.e., relatively rarely contain additional undiscovered planets). If low eccentricities indeed favor high multiplicities, habitability may be more common in systems with a larger number of planets.Solar System orbital eccentricities are unusually low compared with those of exoplanets. This fact is one of the most frequently noted major surprises revealed by the discovery and early explorations of the exoplanet population orbiting Sun-like stars and has been widely interpreted to indicate that the Solar System is not a representative example of a planetary system (reviews by refs. 1–3 and references therein). Many planetary formation theories developed before the discovery of exoplanets suggested planets would have eccentricities similar to the Solar System planets (4, 5). Several attempts have been made to accurately model the dynamical evolution of planetary systems since then, with the goal of explaining the observed eccentricity distribution (6–10). These papers invoke planet−planet interactions as the primary mechanism determining the distribution of orbital eccentricities. The most recent of these papers (10) concludes that there would be a dependence of eccentricity on multiplicity (the number of planets in the system) in this scenario. We use existing radial velocity (RV) exoplanet data to test that prediction.Our dataset consists of 403 of the 441 cataloged RV exoplanets obtained since the 1990s (exoplanet.org). Of these, 127 are members of known multiple-planet systems with multiplicities of up to six. The data are sufficient to allow an estimate of the relationship of eccentricity to multiplicity. It has been noted that eccentricity in two-planet systems tends to be lower than in single-planet systems (11). This paper explores the relation at higher multiplicities and notes its unexpected and surprising consistency with the Solar System case.The dataset is discussed in the next section. We then show the trend in eccentricity with multiplicity and comment on possible sources of error and bias. Next we measure the mean, median, and probability density distribution of eccentricities for various multiplicities and fit them to a simple power-law model for multiplicities greater than two. This fit is used to make a rough estimate of the number of higher-multiplicity systems likely to be contaminating the one- and two-planet system samples due to as yet undiscovered members under plausible, but far from certain, assumptions. Finally, we conclude with some discussion of the implications of this result.     

肾上腺髓质素在中枢神经系统内的分布

目的研究肾上腺髓质素（ＡｄＭ）在中枢神经系统内的分布。方法应用免疫组织化学（ＡＢＣ法）和反转录－聚合酶链式反应（ＲＴ－ＰＣＲ）方法，观察免疫活性的ＡｄＭ及其ＡｄＭｍＲＮＡ在大鼠和人脑内的分布。结果在所检查的大鼠每一个脑区，包括大脑皮层、室旁组织、下丘脑、中脑、延髓和小脑均发现有免疫活性的ＡｄＭ及ＡｄＭｍＲＮＡ存在，应用半定量ＲＴ－ＰＣＲ分析方法发现，在大鼠的室旁组织和延髓中，ＡｄＭｍＲＮＡ表达水平较高。在人脑也发现有ＡｄＭｍＲＮＡ表达。结论在大鼠和人的中枢神经系统中存在肾上腺髓质素，它可能作为一种神经递质、神经调质或神经激素发挥生物学作用。     

Origin of Auer Bodies

Evidence accrued by electron microscopic study of in vitro tissue-culturedleukemic cells supports Ackerman’s histochemical evidence that Auer bodiesare formed from azurophilic granules, a circumstance first postulated by Nakashima in 1924. The enzymatic content and structure of these granules conformsto that of lysosomes, according to deDuve’s concept. Therefore the Auer bodyactually represents an unusual form, or abnormal development, of lysosomes.

Submitted on May 24, 1965 Accepted on July 19, 1965