Regulation mechanisms of pheromone release in males of the desert locust, Schistocerca gregaria

Die Wüstenheuschrecke, Schistocerca gregaria, kommt in zwei Phasen vor, die sich morphologisch, physiologisch und ethologisch unterscheiden (UVAROV 1966, PENER & YERUSHALMI 1998). Während in der solitären Phase die Individuendichte sehr gering ist, bilden die Tiere in der gregären Phase riesige Schwärme mit mehreren Millionen Individuen. Unter den Bedingungen der stark erhöhten sexuellen Konkurrenz in der gregären Phase nutzen die Männchen zur chemischen Unterstützung der postkopulatorischen Partnerbewachung Phenylacetonitril (PAN, syn. Benzylcyanid) als Courtship Inhibiting Pheromone und zur Eigenmarkierung als Abstinon (SEIDELMANN & FERENZ 2002). PAN wird von Epidermis-Drüsenzellen hauptsächlich der Flügel und Sprungbeine produziert und nicht gespeichert (SEIDELMANN et al. 2003). Das Pheromon wird nur von geschlechtsreifen, gregären Männchen proportional zur Abundanz sexueller Konkurrenten abgegeben (DENG et al. 1996, SEIDELMANN et al. 2000). Als sensorische Eingänge zur Detektion einer Konkurrenz-Situation könnten neben optischen und olfaktorischen Kanälen auch die Chemorezeptoren der basiconischen Sensillen an den Sprungbein-Femoris dienen. Diese sind mit Mechanorezeptoren kombiniert (CHAPMAN 1982), welche den Wechsel von solitärem zu gregärem Verhalten induzieren (SIMPSON et al. 2001) und zur Wahrnehmung der Populationsdichte dienen. Die Bindung des Pheromons an die Geschlechtsreife (ca. 2 Wochen nach Adultschlupf) und die Anwesenheit von Paarungs-Konkurrenten deuten in Verbindung mit der fehlenden Speicherung des Pheromons auf eine Regulation der Biosynthese hin. In ersten Versuchen konnte gezeigt werden, dass die Synthese von PAN einer neurohormonalen Kontrolle durch ein PAN-Biosynthese-Aktivierendes-Neuropeptid (PAN-BAN) unterliegt (SEIDELMANN & FERENZ 2003). Die Struktur des Neuropeptids konnte bislang noch nicht aufgeklärt werden. Daher sollte durch die Verwendung von Rohextrakten folgenden Fragestellungen nachgegangen werden: (a) Welche sensorischen Eingänge induzieren eine PAN-BAN-Abgabe? (b) Wo wird PAN-BAN gebildet? (c) Wird die Kompetenz zur PAN-Abgabe durch die Reifung der Geschlechtsorgane oder durch den Titer des Reifungshormons der Insekten, Juvenilhormon (JH), gesteuert?Male desert locusts in the gregarious phase release phenylacetonitrile (PAN) when becoming sexually mature and turning yellow. The pheromone has repellent characteristics toward conspecifics. PAN is used by males in dense populations as a courtship inhibiting pheromone to chemically enhance mate guarding. Desert locust males produce PAN only when being grouped with other mature males. After physical isolation from sexual competitors PAN release drops to zero within a few days. Synthesis and release of PAN are under neurohormonal control by a PAN Biosynthesis Activating Neuropeptide (PAN-BAN). Here we report that PAN-BAN is produced in the oesophageal and suboesophageal ganglia and transported via the haemolymph to the epidermal pheromone gland cells. The release of PAN-BAN requires the perception of visual (complex eyes) or olfactory (antenna) stimuli from other mature males. Synchronism of sexual maturation and gland cell competence to produce PAN does not depend on a factor released by the testis or accessory glands. Instead Juvenile Hormone (JH) was found to be directly or indirectly involved in the regulation of PAN biosynthesis. Increasing the JH titre by transplanting corpora allata into juvenile gregarious males triggered the pheromone release within a couple of days. Whether JH stimulates directly the PAN-BAN receptor presence or the pheromone biosynthesis enzyme apparatus of the gland cells or indirectly by a still unknown factor remains to be investigated

Modeling population dynamics of solitary bees in relation to habitat quality

To understand associations between habitat, individual behaviour, and population development of solitary bees we developed an individual-based model. This model is based on field observations of <i>Osmia rufa</i> (L) (Apoideae: Megachilidae) and describes population dynamics of solitary bees. Model rules are focused on maternal investment, in particular on the female’s individual decisions about sex and size of progeny. In the present paper, we address the effect of habitat quality on population size and sex ratio. We examine how food availability and the risk of parasitism influence long-term population development. It can be shown how population properties result from individual maternal investment which is described as a functional response to fluctuations of environmental conditions. We found that habitat quality can be expressed in terms of cell construction time. This interface factor influences the rate of open cell parasitism as the risk for a brood cell to be parasitized is positively correlated with the time of its construction. Under conditions of scarce food and under resulting long provision times even low parasitism rates lead to a high extinction risk of the population, whereas in rich habitats probabilities of extinction are low even for high rates of parasitism. For a given level of food and parasitism there is an optimum time for cell construction which minimizes the extinction risk of the population. Model results demonstrate that under fluctuating environmental conditions, decreasing habitat quality leads to a decrease in population size but also to rapid shifts in sex ratio

Improved accuracies for satellite tracking

A charge coupled device (CCD) camera on an optical telescope which follows the stars can be used to provide high accuracy comparisons between the line of sight to a satellite, over a large range of satellite altitudes, and lines of sight to nearby stars. The CCD camera can be rotated so the motion of the satellite is down columns of the CCD chip, and charge can be moved from row to row of the chip at a rate which matches the motion of the optical image of the satellite across the chip. Measurement of satellite and star images, together with accurate timing of charge motion, provides accurate comparisons of lines of sight. Given lines of sight to stars near the satellite, the satellite line of sight may be determined. Initial experiments with this technique, using an 18 cm telescope, have produced TDRS-4 observations which have an rms error of 0.5 arc second, 100 m at synchronous altitude. Use of a mosaic of CCD chips, each having its own rate of charge motion, in the focal place of a telescope would allow point images of a geosynchronous satellite and of stars to be formed simultaneously in the same telescope. The line of sight of such a satellite could be measured relative to nearby star lines of sight with an accuracy of approximately 0.03 arc second. Development of a star catalog with 0.04 arc second rms accuracy and perhaps ten stars per square degree would allow determination of satellite lines of sight with 0.05 arc second rms absolute accuracy, corresponding to 10 m at synchronous altitude. Multiple station time transfers through a communications satellite can provide accurate distances from the satellite to the ground stations. Such observations can, if calibrated for delays, determine satellite orbits to an accuracy approaching 10 m rms

The Future of Time: UTC and the Leap Second

Before atomic timekeeping, clocks were set to the skies. But starting in 1972, radio signals began broadcasting atomic seconds and leap seconds have occasionally been added to that stream of atomic seconds to keep the signals synchronized with the actual rotation of Earth. Such adjustments were considered necessary because Earth's rotation is less regular than atomic timekeeping. In January 2012, a United Nations-affiliated organization could permanently break this link by redefining Coordinated Universal Time. To understand the importance of this potential change, it's important to understand the history of human timekeeping

How Well Do We Know the Orbits of the Outer Planets?

This paper deals with the problem of astrometric determination of the orbital elements of the outer planets, in particular by assessing the ability of astrometric observations to detect perturbations of the sort expected from the Pioneer effect or other small perturbations to gravity. We also show that while using simplified models of the dynamics can lead to some insights, one must be careful to not over-simplify the issues involved lest one be misled by the analysis onto false paths. Specifically, we show that the current ephemeris of Pluto does not preclude the existence of the Pioneer effect. We show that the orbit of Pluto is simply not well enough characterized at present to make such an assertion. A number of misunderstandings related to these topics have now propagated through the literature and have been used as a basis for drawing conclusions about the dynamics of the solar system. Thus, the objective of this paper is to address these issues. Finally, we offer some comments dealing with the complex topic of model selection and comparison.Comment: Accepted for publication in the Ap

Units of relativistic time scales and associated quantities

This note suggests nomenclature for dealing with the units of various astronomical quantities that are used with the relativistic time scales TT, TDB, TCB and TCG. It is suggested to avoid wordings like "TDB units" and "TT units" and avoid contrasting them to "SI units". The quantities intended for use with TCG, TCB, TT or TDB should be called "TCG-compatible", "TCB-compatible", "TT-compatible" or "TDB-compatible", respectively. The names of the units second and meter for numerical values of all these quantities should be used with out any adjectives. This suggestion comes from a special discussion forum created within IAU Commission 52 "Relativity in Fundamental Astronomy"