bluuebunny/crossref_metadata_2025 huggingface dataset:
Conditional Sojourn times and the volatility of payment schemes for bandwidth sharing in packet networks
Authors: Guillemin Fabrice M. , Mazumdar Ravi R.
Published: March 2016

Predictability of revenue and costs to both operators and users is critical for payment schemes. We study the issue of the design of payment schemes in networks with bandwidth sharing. The model we consider is a processor sharing system that is accessed by various classes of users with different processing requirements or file sizes. The users are charged according to a Vickrey–Clarke–Groves mechanism because of its efficiency and fairness when logarithmic utility functions are involved. Subject to a given mean revenue for the operator, we study whether it is preferable for a user to pay upon arrival, depending on the congestion level, or whether the user should opt to pay at the end. This leads to a study of the volatility of payment schemes and we show that opting for prepayment is preferable from a user point of view. The analysis yields new results on the asymptotic behavior of conditional response times for processor sharing systems and connections to associated orthogonal polynomials.
Counting processes with Bernštein intertimes and random jumps
Authors: Orsingher Enzo , Toaldo Bruno
Published: March 2016

In this paper we consider point processes Nf
(t), t > 0, with independent increments and integer-valued jumps whose distribution is expressed in terms of Bernštein functions f with Lévy measure v. We obtain the general expression of the probability generating functions Gf
of Nf
, the equations governing the state probabilities pk
f
of Nf
, and their corresponding explicit forms. We also give the distribution of the first-passage times Tk
f
of Nf
, and the related governing equation. We study in detail the cases of the fractional Poisson process, the relativistic Poisson process, and the gamma-Poisson process whose state probabilities have the form of a negative binomial. The distribution of the times of jumps with height lj
() under the condition N(t) = k for all these special processes is investigated in detail.
Correlated fractional counting processes on a finite-time interval
Authors: Beghin Luisa , Garra Roberto , Macci Claudio
Published: March 2016

We present some correlated fractional counting processes on a finite-time interval. This will be done by considering a slight generalization of the processes in Borges et al. (2012). The main case concerns a class of space-time fractional Poisson processes and, when the correlation parameter is equal to 0, the univariate distributions coincide with those of the space-time fractional Poisson process in Orsingher and Polito (2012). On the one hand, when we consider the time fractional Poisson process, the multivariate finite-dimensional distributions are different from those presented for the renewal process in Politi et al. (2011). We also consider a case concerning a class of fractional negative binomial processes.
The extinction time of a subcritical branching process related to the SIR epidemic on a random graph
Authors: Windridge Peter
Published: March 2016

We give an exponential tail approximation for the extinction time of a subcritical multitype branching process arising from the SIR epidemic model on a random graph with given degrees, where the type corresponds to the vertex degree. As a corollary we obtain a Gumbel limit law for the extinction time, when beginning with a large population. Our contribution is to allow countably many types (this corresponds to unbounded degrees in the random graph epidemic model, as the number of vertices tends to∞). We only require a second moment for the offspring-type distribution featuring in our model.
On the role of Föllmer-Schweizer minimal martingale measure in risk-sensitive control asset management
Authors: Deshpande Amogh
Published: March 2016

Kuroda and Nagai (2002) stated that the factor process in risk-sensitive control asset management is stable under the Föllmer-Schweizer minimal martingale measure. Fleming and Sheu (2002) and, more recently, Föllmer and Schweizer (2010) observed that the role of the minimal martingale measure in this portfolio optimization is yet to be established. In this paper we aim to address this question by explicitly connecting the optimal wealth allocation to the minimal martingale measure. We achieve this by using a ‘trick’ of observing this problem in the context of model uncertainty via a two person zero sum stochastic differential game between the investor and an antagonistic market that provides a probability measure. We obtain some startling insights. Firstly, if short selling is not permitted and the factor process evolves under the minimal martingale measure, then the investor's optimal strategy can only be to invest in the riskless asset (i.e. the no-regret strategy). Secondly, if the factor process and the stock price process have independent noise, then, even if the market allows short-selling, the optimal strategy for the investor must be the no-regret strategy while the factor process will evolve under the minimal martingale measure.
On generalized max-linear models and their statistical interpolation
Authors: Falk Michael , Hofmann Martin , Zott Maximilian
Published: March 2016

We propose a method to generate a max-stable process in C[0, 1] from a max-stable random vector in R

d
by generalizing the max-linear model established by Wang and Stoev (2011). For this purpose, an interpolation technique that preserves max-stability is proposed. It turns out that if the random vector follows some finite-dimensional distribution of some initial max-stable process, the approximating processes converge uniformly to the original process and the pointwise mean-squared error can be represented in a closed form. The obtained results carry over to the case of generalized Pareto processes. The introduced method enables the reconstruction of the initial process only from a finite set of observation points and, thus, a reasonable prediction of max-stable processes in space becomes possible. A possible extension to arbitrary dimensions is outlined.
A multitype infinite-allele branching process with applications to cancer evolution
Authors: McDonald Thomas O. , Kimmel Marek
Published: March 2016

We extend the infinite-allele simple branching process of Griffiths and Pakes (1988) allowing the offspring to change types and labels. The model is developed and limit theorems are given for the growth of the number of labels of a specific type. We also discuss the asymptotics of the frequency spectrum. Finally, we present an application of the model's use in tumorigenesis.
A note on the virtual waiting time in the stationary PH/M/c+D queue
Authors: Kawanishi Ken'ichi , Takine Tetsuya
Published: March 2016

In this paper we consider the stationary PH/M/c queue with deterministic impatience times (PH/M/c+D). We show that the probability density function of the virtual waiting time takes the form of a matrix exponential whose exponent is given explicitly by system parameters.
Current Uses for Task-Based Language Assessment
Authors: Norris John M.
Published: March 2016

Task-based language assessment (TBLA) has generated interest since the early 1990s, primarily in conjunction with the ongoing development of task-based language teaching (TBLT) and the pursuit of developing appropriate testing models for this approach to pedagogy (Norris, 2002, 2009). However, tasks also offer considerable advantages for language assessment, beyond their obvious relevance within TBLT classes and programs. In fact, major innovations in the general domain of language assessment over the past two decades have occurred in conjunction with the introduction of tasks into assessment design, largely in response to the need for tests that better represent examinees’ abilities to use the language (Mislevy, Steinberg, & Almond, 2002), but also because tasks offer a meaningful space for language teachers, testers, learners, and others to examine, understand, and improve language learning endeavors (Van Gorp & Deygers, 2013). This article reviews the considerable range of current uses for TBLA, illustrating different types of assessment with concrete examples and highlighting distinct roles for tasks as a basic unit of analysis in test design, interpretation, and intended consequence. Ultimately, it argues that tasks offer a fundamental, though not exclusive, foundation for useful language assessment, and that task-based assessment, though challenging, is probably worth the effort.
Grape-6
Authors: Makino J.
Published: March 2016

We overview the GRAPE-6 project, a follow-up of the teraflops GRAPE-4 project. GRAPE-6 will be completed by 1999-2000 and its planned peak speed is 200 Tflops. Its architecture will be largely similar to that of GRAPE-4, which is a specialized hardware to calculate the gravitational interaction between particles. The improvement of the speed will mainly come from the advance in the silicon semiconductor technology. GRAPE-6 will enable us to directly simulate the evolution of star clusters with up to 1 million stars.
Grape-4: A Teraflops Machine for N-Body Simulations
Authors: Taiji Makoto
Published: March 2016

We have developed a massively parallel special-purpose computer system for N-body simulations, GRAPE-4 (GRAvity-PipE 4). The GRAPE-4 system is designed for high-accuracy simulations of dense stellar systems. The GRAPE-4 calculates gravitational forces, their derivatives in time and potential energies. It has a hardware for prediction of positions and velocities, which is used for the individual timestep scheme. We integrated 1692 chips of 640 megaflops performance to achieve the peak speed of 1.08 teraflops.
Numerical Simulations of Galaxies with the Marseille Grape-3 Systems
Authors: Athanassoula E. , Bosma A. , Lambert J.-C. , Makino J.
Published: March 2016

We briefly describe the performance and accuracy of the Marseille GRAPE-3 systems. We first give the description of the configurations. We then outline the modifications necessary to optimize the tree code for use on a GRAPE system, and discuss performance and accuracy issues. We summarize the results of several science projects executed with our hardware and software.
Pulsation Modes of Spherical Stellar Systems
Authors: Sellwood J. A. , Pryor C.
Published: March 2016

Kuhn & Miller (1989, KM hereafter) proposed that a small stellar system in orbit around a large galaxy could be heated through resonant coupling between the orbital motion and internal modes of oscillation of the satellite. They further argued that the apparently large mass-to-light (M/L) ratios of dwarf spheroidal (dSph) galaxies around the Milky Way (e.g., Armandroff, Olszewski & Pryor 1995) could be illusory because the satellites are far from virial equilibrium as a consequence of such resonant heating. We note that if the true M/Ls are small, some dSphs have much more kinetic energy than is required to unbind them; a resonant pumping mechanism which adds a modest amount of energy each cycle could not achieve this (Pryor 1996).
JD 16 – Spectroscopy With Large Telescopes of Chemically Peculiar Stars: Preface
Authors: Takada-Hidai M. , Zverko J.
Published: March 2016

The Keck 10-m telescope has begun to produce many new findings in a field of stellar spectroscopy with the help of the High Resolution Spectrograph (HIRES). The other large telescopes such as the Subaru, VLT, and Gemini are now being constructed and expected to perform high-resolution spectroscopy in a near future within several years or so. These highresolution spectroscopic studies will be carried out based on studies which have been made mainly with existing telescopes with aperture smaller than 4 m.
Diffusion in Stellar Envelopes
Authors: Seaton M.J.
Published: March 2016

In an attempt to make the present summary comprehensible yet sufficiently concise I will risk some over-simplification: further details are given in Seaton (1997, 1998 — Papers I and II).

In a star let Fv dv be the outward flux of radiant and let an atom of element k present an effective area of σv(k) for absorption of radiation. Then the momentum absorbed per atom and per-unit area and unit time is G(k) = (1/c) ∫ Fvσv(k) dv which is just the force acting on the atom. The radiative acceleration is grad(k) = G(k)/M(k) where M(k) is the atom’s mass.
Stellar Evolution, Particle Transport, and the CP Phenomenon
Authors: Michaud G. , Richer J.
Published: March 2016

In the light of recent results from helioseismology, the abundance anomalies seen at the surface of Bp, Ap, Am and Fm stars appear as the measurable superficial effect of a process that has much more general impact.
On the Earliest Stage of Chinese Astronomy: 3 Hypotheses
Authors: Maeyama Y.
Published: March 2016

With the achievements obtained in the last few years, in particular most recently, I arrived at the following three hypotheses which seem to combine some major problems of ancient Chinese astronomy on a common historical basis.
An Arabic Commentary on Al-Tūsū’S Al-Tadhkira and its Sanskrit Translation
Authors: Kusuba Takanori
Published: March 2016

Na๣īr al-Dīn al-Ṭūsī (1201-1274) composed his Tadhkira at Marāgha in 1261 and altered it with his students and produced his “final version” at Baghdad in 1274. The Baghdad version with all its differences from the Marāgha version was published by Ragep [1993]. That the Tadhkira was considered important by astronomers writing in Arabic is amply attested to by the fact that Ragep [1993] can list fourteen commentaries and supercommentaries as well as refer to numerous other derivative texts.
Indian Astronomy in Ancient China
Authors: Xiao-Yuan Jiang
Published: March 2016

Indian astronomy was introduced into China along with the intrusion of Buddhism. This process lasted about one thousand years in the Mediaeval age. For the study of this process, there are a lot of materials in ancient Chinese historic texts, while the Buddhist scriptures in Chinese translation are very important first-hand materials.
Projection Methods in Chinese, Korean and Japanese Star Maps
Authors: Miyajima Kazuhiko
Published: March 2016

The celestial map of the Chunyou stone inscription in Suzhou and that contained in the Xin yixiang fayao (), both belonging to the Song () Dynasty, are among the oldest of the extant celestial maps in China. The former has a circular form, and the latter is in two forms, circular and rectangular. I have been wondering which projection methods were used in these star maps, or rather, whether they were ever drawn accurately enough for us to be able to discuss their projection methods. While the stone inscription in Suzhou remains original without any change, we are not sure to which extent the star map in the Xin yixiang fayao maintains its original form, because the text underwent frequent reimpressions.
Contemporary Astronomy in Iran – A Status Report
Authors: Sobouti Y.
Published: March 2016

There are of the order of 30 astronomers with research records and another 40-50 with substantial education in astronomy and astrophysics. Geographically, astronomical and astrophysical research is concentrated mainly at Shiraz University (cosmology and photometric observations), Sharif University of Theran (cosmology and gamma-ray astronomy), Tabriz University (binaries and solar physics), Meshad University (binaries and interstellar matter), Zanjan University (stellar dynamics, radio astronomy) and the Institute for Advanced Studies in Basic Sciences, Zanjan (stellar and stellar systems studies).
Jets and Transients
Authors: Blandford R. D.
Published: March 2016

I have been asked to provide some general introduction to the topic of jets and high energy transients. I have chosen to do this by asking seven questions that seem to be timely following recent observational and theoretical developments, the most important of which may be the growing realization that the extragalactic- massive black hole and Galactic-stellar mass black hole manifestations of these phenomena provide two complementary ways of viewing a common physical mechanism. I have also chosen to illustrate these questions using one specific source in each case. The page limits prevent me from giving the answers. They also prohibit my even attempting to give a skeletal bibliography over so large a field. Fortunately almost all of these topics will be covered in greater depth during this meeting.
High-Energy Solar Gamma-Ray Observations
Authors: Yoshimori M. , Saita N. , Shiozawa A.
Published: March 2016

In the last solar maximum, gamma-rays associated with solar flares were observed with GRANAT, GAMMA-1, CGRO and YOHKOH. The gamma-ray energies ranged from 100 keV to a few GeV. We obtained several new findings of gamma-ray emission on the Sun: (1) Gamma-ray production in the corona, (2) GeV gamma-ray production in very long duration flares, (3) Electron-rich flares, (4) Gamma-ray lines and solar atmospheric abundances and (5) Possible location of gamma-ray emission. We present the observations of these new findings and discuss high energy phenomena relating to particle acceleration and gamma-ray production during solar flares.
X-Ray Transients — Results of Rosat Observations
Authors: Trümper J. , Dennerl K. , Englhauser J.
Published: March 2016

The main strengths of ROSAT [1] are its high quality imaging of extended sources and its large sensitivity for the detection of point sources. In the all-sky survey the diffuse X-ray emission was mapped with a resolution of 12 arcmin [2]. The number of point sources detected in the survey is ≈ 80 000 [3]. In addition more than 80 000 sources have been found in the ≈ 6 500 fields observed with the PSPC and HRI until now in the course of the pointed programme. A wealth of information about source variabilities has been extracted both from the all-sky survey and from the pointed observations, as well as from a combination of both.
Formation of Low-Mass Black Hole X-Ray Transients
Authors: Zwart Simon Portegies , Verbunt Frank , Ergma Ene
Published: March 2016

We study the formation of low-mass X-ray binaries with a black hole as accreting object. The performed semi-analytic analysis reveals that the formation rate of black holes in low-mass X-ray binaries is about two orders of magnitude smaller than that of systems with a neutron star as accretor. This is contradicted by the six observed systems, which are all transients, which suggest that the majority of these systems has not been seen jet. The birthrate for both type of objects are expected to be similar (for reviews see Cowley 1992, Tanaka & Lewin 1995).
Population Synthesis of High Energy Transients: Relativistic Binary Merging Rates
Authors: Lipunov V.M.
Published: March 2016

Binary relativistic stars merging — the most powerful high energy transient in the Universe:Lmerging˜ Mc2/Rg/c = c5/G ˜ 1058erg/s. That is equal to Planckian luminosity (Lipunov 1992)Lplanck= EPlanck/tplanck= C5/G.
Timing of Gamma-Ray Pulsars
Authors: Bisnovatyi-Kogan G.S.
Published: March 2016

Exept Geminga there could be other gamma ray pulsars with no radioemission, which are exhibited in EGRET observations as ordinary point-like sources [6]. Determination of pulsations in a hard gamma ray source is complicated by rareness of arriving quanta δt ≫ P, and their small total number. When the value of the period is known from other observations (radio or X-ray), timing analysis gives the possibility to find this periodicity also in a gamma region [1].
Gamma-Ray Bursts: Theoretical Considerations
Authors: Mészáros P.
Published: March 2016

The discovery of the afterglows of gamma-ray bursts (GRB) at X-ray, optical and radio wavelengths heralds a new era in the investigation of these objects. This provides a quantum jump in the type of observational information available, providing much more severe constraints on models, and probably represents the light at the end of the tunnel for this long-standing puzzle of astrophysics.
Particle Acceleration by Waves and Fields
Authors: Dröge Wolfgang
Published: March 2016

The acceleration of electrons and charged nuclei to high energies is a phenomenon occuring at many sites throughout the universe, including the galaxy, pulsars, quasars, and around black holes. In the heliosphere, large solar flares and the often associated coronal mass ejections (CMEs) are the most energetic natural particle accelerators, occasionally accelerating protons to GeV and electrons to tens of MeV energies. The observation of these particles offers the unique opportunity to study fundamental processes in astrophysics. Particles that escape into interplanetary space can be observed in situ with particle detectors on spacecraft. In particular, particle spectra can be diagnostic of flare acceleration processes. On the other hand, energetic processes on the sun can be studied indirectly, via observations of the electromagnetic emissions (radio, X-ray, gamma-ray) produced by the particles in their interactions with the solar atmosphere. The purpose of this article is to give a brief overview on current models on particle acceleration and the present status of observations of solar energetic particles.
Summary of Session A: Coronal Heating and Solar Wind Acceleration
Authors: Sakurai Takashi
Published: March 2016

The solar corona is not easily observable from the ground; only with the coronagraphs located in high mountains or at infrequent and short occasions of total eclipses. And in any case these observations are limited to the corona beyond the solar limb. Therefore, it is natural that our understanding of the physics of the solar corona has advanced dramatically by sustained observations from space-based platforms, like Skylab in the 1970’s. These several years are particularly notable in this respect, because of a wide variety of data from Yohkoh, Ulysses, and SOHO.
Education and Research in Astronomy in Central America
Authors: Carias M. C. Pineda De
Published: March 2016

Recently, important efforts have been made to organize and consolidate the Assembly of Central American Astronomers (AAAC), an organization created to contribute to the development of astronomy and astrophysics in Central America, with the help of international cooperation; the Central American Courses in Astronomy and Astrophysics, have been hosted each year by a different national university in Central America (1995: Universidad Nacional Autonoma de Honduras, 1996: Universidad de El Salvador, 1997: Universidad de San Carlos de Guatemala, and 1998: Universidad de Panama). These courses aimed to provide an exchange of knowledge and experience among university staff and students interested in continuing studies in Astronomy and Astrophysics. Regional Observational Campaigns have been organized to train young astronomers in the use of astronomical equipment and observational techniques. It seems that the broad development of astronomy and astrophysics in Central American as a whole, will be possible only when nuclei of astronomers in each of the countries concerned begin to develop many more activities, countries As part of the III Central American Course on Astronomy and Astrophysics (III-CURCAA, April 1997, Guatemala), in a forum about Education and Research in Astronomy in Central America, several important conclusions were stated. In this paper we present the six most relevant conclusions discussed there.
Strategies for Establishing Astronomy in Developing Countries
Authors: Othman Mazlan
Published: March 2016

Developing countries have their own particular political, economic and cultural circumstances. There are, therefore, no unique solutions. However there are some factors which are common to all or most of them, namely the lack of human and financial resources and in most cases an absence of a political commitment to the advancement of science. Such situations are in a sense not peculiar to developing nations because in some developed countries astronomy has a ‘developing’ status. Even in countries where astronomy is well established, the commitment and allocations required to maintain the status quo need to be continuously addressed. Hence strategies for fighting this “constant battle” are relevant to all astronomers of the world, while being especially vital to those in the developing world.
Training of Astronomers in Central Asia and Some Comparisons
Authors: Nuritdinov S. N.
Published: March 2016

In the Soviet Union (SU) professional curricula were the same in each republic. After the dissolution of the SU the various states in the Commonwealth of Independent States gradually adopted quite different curricula. Some professions were narrowed in scope or were no longer provided for. Until recently there were, in Central Asia, three types of curricula for taining astronomers.
Networking of Astronomy Institutions in the Third World Countries
Authors: Narlikar Jayant V.
Published: March 2016

There are several international organizations currently working towards raising the standard of science and technology in the third world countries (TWCs). It is being appreciated that instead of dealing with the issue on a country by country basis, it helps to view and solve the problem in a network mode. It is sometimes the case that one TWC may have resource persons, or facilities which can benefit by sharing with the other TWCs. Or, a group of workers from different TWCs can be brought together for a school or workshop in which experts drawn from different parts of the world participate as lecturers or guides.
Megamasers in Active Galactic Nuclei
Authors: Cohen R. J.
Published: March 2016

Extragalactic masers were discovered more than 20 years ago (Whiteoak & Gardner 1973). It soon became apparent that those extragalactic masers we can detect are intrinsically very powerful and are located in galactic nuclei. The term Megamaser was coined to describe the most luminous OH masers, which are a million times more powerful than any OH masers within our own Galaxy (Baan & Haschick 1984). The same word is nowadays applied to any powerful maser associated with an active galactic nucleus (AGN). Whereas normal Galactic masers would be barely detectable outside the Local Group, megamasers are detectable in principle out to redshifts of z ~ 2 (Baan 1997). The galaxies hosting megamasers in their nuclei are invariably active in some degree: they include ultraluminous infrared galaxies, starbursts and Seyfert galaxies.
Exploring OH Megamasers
Authors: Baan W.A.
Published: March 2016

The OH megamasers have a distinct parent population of dusty and FIR luminous merger galaxies. Optical, radio and molecular characteristics may be used to further identify the nature of the nuclear activity in the OH megamaser host galaxies. Recent interferometric data on OH megamasers Arp 220 and III Zw35 will be used to discuss the spatial distribution of the OH emission.
AGN Disk Diagnostics
Authors: Blandford R. D.
Published: March 2016

The discovery of megamasers in nearby active galactic nuclei (AGN) is an unexpected boon for AGN researchers. The most immediate benefit, brought out in observations of NGC4258 (Miyoshi et al 1995, Moran, these proceedings) is that it allows an accurate mass measurement for the central black hole, in this case of 3.6 x 107 M⊙, with unprecedented accuracy. (I shall not belabor the point that we have not proven rigorously that it is a black hole because this is surely on much firmer footing than what follows!) Masers also allow us to discover second order features of the kinematics, specifically that the disk is warped. Thirdly, and this is what I have been asked to review here, it should enable us to choose between several possible accretion modes by treating masers as diagnostic probes of physical conditions in the disk.
The Role of Lunar Astronomy in the Exploration and Development of the Moon
Authors: McLaughlin W. I.
Published: March 2016

Lunar astronomical facilities can be robotically emplaced or form an adjunct to a human base. Connected facilities are a means to increase science-per-dollar. Near-Earth and Centaur asteroids may also serve as venues for astronomy.
Examples of Possible Astronomical Research from the Moon
Authors: Swings Jean-Pierre
Published: March 2016

As stressed at the second International Lunar Exploration Working Group meeting (Kyoto, October 1996), the Moon, if kept free from pollution, contains a series of remarkable astronomical sites. In particular the following fields of instrumentation and research emerge :

(1) very low frequency radio-astronomical arrays to be located on the lunar far side for surveying an entirely new spectrum, albeit at fairly low angular resolution;

(2) interferometers in several wavebands to search for extrasolar planets as well as to perform other observations (morphological studies e.g.);

(3) transit optical telescopes for the detailed observation of dark matter and other targets;

(4) millimeter-wave telescopes for high sensitivity cosmic background mapping;

(5) infrared telescopes in permanently cryogenic environment (e.g. the lunar South pole);

(6) gravitational wave detectors;

(7) cosmic-ray and high energy detectors;
Low Frequency Radio Astronomy from the Moon
Authors: Jones D.L. , Weiler K.W.
Published: March 2016

The radio sky at frequencies of several MHz and below is essentially unexplored with high angular resolution due to refraction and opacity in the Earth’s ionosphere. An interferometer array in space providing arcminute resolution images would allow a wide range of problems in solar, planetary, galactic, and extragalactic astronomy to be attacked. These include the evolution of solar and planetary radio bursts, interplanetary and interstellar scintillation, the distribution of low energy cosmic rays and diffuse ionized hydrogen in our galaxy, the determination of spectral turnover frequencies and magnetic field strengths in galactic and extragalactic radio sources, searches for “fossil” radio galaxies which are no longer detectable by high frequency surveys, and searches for new sources of coherent radio emission. In addition, it is likely that unexpected objects and emission processes will be discovered by such an instrument, as has often happened when high resolution observations first become possible in a new spectral region. The Moon can provide shielding from terrestrial interference (and from the Sun half of the time) and consequently the lunar farside surface offers an ideal site of a low frequency radio array.
The Future Japanese CBR Anisotropy Observatory at the Moon
Authors: Tsuboi M. , Kaifu N. , Karoji H. , Takeuchi S. , Iwata T. , Itoh N. , Miyahara N.
Published: March 2016

We have a plan to a radioastronomy mission at the Moon. This is dedicated to the mapping of the CBR anisotropy in order to study the properties of the early Universe, especially galaxy formation. This is a candidate for the Moon mission of NASDA, launched by an HIIA Rocket. The mission carries an 1.5 m (min.) offset parabola antenna with radiation shield to the north polar region of the Moon. This will observe CBR anisotropy at three (min.) frequencies between 30 to 90 GHz. The angular resolution is 9’ at 90 GHz. The telescope will observe the donut-shaped sky between 5 to 30 degree (not fixed) from the Moon celestial north pole. The resultant sensitivity will reach ΔT/T ⋍ 106K in 30’x30’ pixel and ΔT/T ⋍ 105K in 9’x9’ pixel.
Early Observations of the Leonids in East Asia
Authors: Hasegawa I.
Published: March 2016

The parent comet of the Leonids, 55P/Tempel-Tuttle, was recovered in 1997. An improved orbit for the interval 1366 to 1997 together with predictions before 1366 were calculated by Nakano (1997). These orbital elements are used to determine the longitude of the descending node of the cometary orbit so that this can be compared with the solar longitude of meteors found in historic records. A number of catalogues listing the appearances of meteors showers have already been published. Most notable of these are Imoto and Hasegawa (1958), Zhuang (1977), Mason (1995), Rada and Stephenson (1992), Kidger (1993) and Hasegawa (1996). Nearly fifty records of the Leonids from AD855 to the end of the 19th century are found in these catalogues.
Observations of the Leonids over the Last Millenium
Authors: Dick Steven J.
Published: March 2016

The recognition of the astronomical origin of meteors is intimately connected to the Leonid meteors, and their tendency to “storm” with a period of 33 years. It was the Leonid storm of 1799, observed by Alexander von Humboldt among others, that first established the geographical extent of the phenomenon, with observations reported over 90 degrees of longitude and 60 degrees of latitude. During the 1833 storm, Olmsted (1834) at Yale and Twining (1834) at West Point established the radiant point in Leo, and the cosmic origin was clinched when H. A. Newton (1863), also at Yale, determined that the cycle repeated in intervals of sidereal years, not tropical years. Inspired by the 1866 storm, Adams (1866), Schiaparelli (1867), and Le Verrier (1867) determined a 33.25 year period and other orbital elements for the meteor stream; two years after the discovery of Comet Tempel-Tuttle in 1865, that comet was recognized as the parent body of the Leonid stream after von Oppolzer (1867) calculated a period of 33.17 years for the comet. Astronomers confidently predicted another storm in 1899, but none appeared, though there were good showers in 1901-1903. The years 1930-32 also brought fairly good showers, but 1966 brought the strongest storm witnessed in modern times, with an estimated 100,000 meteors per hour. Steady progress was made in meteor studies in the 20th century, especially with new photographic and radar techniques. The current question is what will happen in the 1997-1999 period; the only certainty is that the event will be studied with an even wider array of techniques.
RADAR Observations
Authors: Baggaley W.J.
Published: March 2016

Radar techniques can be a powerful adjunct for studying meteor storms in general because of their sensitivity, capacity for continuous observations and their use of current techniques facilitating the handling of data. While some radars are limited to only a range-time presentation (and so adequate for a time-profile description of a storm event), some facilities have the additional capacity to determine directional information or orbital elements which are valuable in delineating the dynamics and spatial structure of stream meteoroids. The following outlines the application of radar techniques to meteor storm recording and summarizes current and planned facilities.
Near-IR Spectroscopy of the Atmosphere of Jupiter
Authors: Carlson R.W. , Baines K.H. , Encrenaz T. , Drossart P. , Roos-Serote M. , Taylor F.W. , Irwin P. , Weir A. , Smith P. , Calcutt S.
Published: March 2016

The Galileo Near Infrared Mapping Spectrometer (NIMS) obtains spectral images in the wavelength range 0.7 to 5.2 μm with a spectral resolving power of approximately 200. This spectral range allows NIMS to sense cloud-reflected solar radiation, thermal emission produced in the deep atmosphere, and auroral emission from the thermosphere of Jupiter. Using 5 μm thermal emission spectroscopy, the amount of water vapor in the deep atmosphere, at approximately the (i to 8 bar level, is found to vary by a factor > 100. Deep atmosphere ammonia was also found to vary, with a spatial behavior different from that of water vapor. No evidence is found for a massive water cloud. Using reflected solar radiation in conjunction with thermal emission, two cloud layers are found, the upper at 0.5 bars and a lower one at 1-1.3 bars. The inferred absorption properties of these clouds are consistent with ammonia crystals (the upper cloud) and ammonium hydrosulfide particles (the lower cloud).
Galileo UVS Results and Cassini Preview
Authors: Esposito L.W. , Barth C.A. , Hendrix A.R. , Hord C.W. , Stewart A.I.F. , Ajello J.M. , West R.A.
Published: March 2016

UVS results from Jupiter show the Io torus colder and brighter than the Voyager observations. Aurora near Jupiter’s poles emit 1-4 MR from altitudes of 300 – 400 km. Ganymede and Callisto have extended hydrogen exospheres. The near-UV reflectance of the Galilean satellites shows SO2, magnetospheric alteration, and O3. Remote sensing of Jupiter’s stratospheric haze determines that it thickens and darkens towards higher latitudes.
ISO Observations of AGN and Ultraluminous IR Galaxies
Authors: Moorwood Alan F. M.
Published: March 2016

All the ISO instruments are contributing to the study of activity in galaxies of essentially all types. Although AGN's as such are pointlike, the beautiful CAM image of CenA shown by Catherine Cesarsky has given us the clearest view so far of its visually obscured nucleus and surrounding spiral disc embedded in an elliptical galaxy. The CAM CVF is also providing spectral images of the PAH features and important diagnostic ionic lines (e.g [NeII] and [NeIII]) in the circumnuclar regions of AGN and merging starburst systems (Vigroux et al., 1996). PHT is providing detailed spectral energy distributions over the complete 2.5-240µm range and PHTS is proving invaluable for assembling a catalogue of low resolution (R ⋍ 90) galaxy spectra covering the 6-12µm PAH features. SWS and LWS are generating higher resolution (R ⋍ 2000-200) spectra over the range 2.5-200µm such as that shown in Fig. 1. of the Circinus galaxy which exhibits both AGN and starburst activity and well illustrates the wide range of diagnostic features, many seen for the first time, accessible to ISO studies of galaxies. It shows the overall continuum with a peak around 100µm; PAH features and Si absorption which dominate the spectrum around 10µm; H recombination lines; H2 pure rotational emission lines; low ionization potential ionic lines excited by starburst activity and high excitation lines (up to ⋍ 300eV) excited by the visually obscured AGN.
The ISO Perspective on Normal Galaxies
Authors: Helou G.
Published: March 2016

Based on results from the first half of its mission, ISO (Kessler et al. 1996) is contributing to our understanding of normal galaxies by offering effective gauges of the physical conditions within the interstellar medium (ISM) of galaxies. ISO data permit a more precise and detailed characterization of the radiation, dust and gas deep within many more galaxies than had been previously possible. This in turn yields new insight into the regulation mechanisms of star formation and galaxy evolution. Apart from these ISM diagnostics, ISO also contributes a vastly improved empirical description of galaxies at all infrared wavelengths, which will be critical in guiding the search for the origins and early life of galaxies.
ISO Results on Star Formation and Early Stellar Evolution
Authors: Montmerle Thierry , Nordh Lennart
Published: March 2016

With all its instruments, ISO is sensitive to temperatures in the range ~ 30 – 2000 K. This range is particularly adapted to studies of dense interstellar matter (gas and dust) in cold clouds, and to material associated with very early stages of stellar evolution: circumstellar matter around low-mass stars (disks, envelopes), outflows generated by them and interactions with the surrounding medium.
ISO Observations of Circumstellar Material
Authors: Habing H.J.
Published: March 2016

Circumstellar matter is found almost exclusively around young stars that have not yet reached the main sequence and around old stars that have left this sequence. Some main sequence stars still carry the remnants of a disk of dustlike material as a remnant of their time of formation.
Does a therapist's reflective ability predict the accuracy of their self-evaluation of competence in cognitive behavioural therapy?
Authors: Loades Maria E. , Myles Pamela J.
Published: March 2016

Accurately evaluating how competently one is performing can be a precursor to seeking training and supervision, therefore contributing to safe, effective practice. Little is known about what predicts accurate self-evaluation. Prior research findings are inconsistent, with overestimation of self-rated competence in some studies and underestimation in others. We aimed to explore the relationship between therapists' reflective ability and the level of agreement between self-rated competence and competence rated by an experienced CBT assessor. Thirteen trainees undertaking a postgraduate CBT diploma submitted a series of recordings accompanied by self-ratings using the Cognitive Therapy Scale – Revised (CTS-R) and related written reflective analyses. Independent assessors marked the written analyses using a standardized marking scheme and rated the therapy sessions using the CTS-R. Trainees tended to overestimate or underestimate their competence in comparison to the independent assessors. The level of agreement between the assessors' ratings and self-evaluation of competence tended to improve during training, while reflective ability did not. Reflective ability was significantly related to level of agreement between self-rated and assessor-rated competence. Trainees do not consistently demonstrate the bias for overestimating their competence previously found in qualified therapists. During training, the tendency of an individual to over- or underestimate their competence may not remain stable, but tends to become more consistent with ratings undertaken by an experienced CBT assessor. Trainees who were rated as more reflective, tended to agree more closely with independent assessors on evaluation of competence. Therefore, enhancing reflective ability may help therapists to more accurately self-evaluate their competence.
Zum Verlauf „normalen“ Trauerns
Authors: Wittkowski Joachim , Scheuchenpflug Rainer
Published: March 2016

Zusammenfassung. Gegenstand der Untersuchung ist die Frage, ob bei Erwachsenen Unterschiede in der Ausprägung verschiedener Aspekte des Trauerns in Abhängigkeit von der Dauer des Trauerprozesses bestehen. Bei einer Stichprobe von 521 trauernden Personen, die das Würzburger Trauerinventar bearbeiteten, zeigt sich innerhalb der ersten zwei Jahre nach Verlust für akute emotionale und kognitive Beeinträchtigungen (BEEIN) sowie für das Empfinden der Nähe zur verstorbenen Person (NÄHE) ein umgekehrt u-förmiger Verlauf mit nachfolgend weiterer Abnahme. Frauen weisen in beiden Skalen höhere Werte auf als Männer. Deskriptiv zeigt sich für Persönlichkeitsentwicklung/Wachstum (WACHS) sowie Empathie für andere (EMPATH) nach einem anfänglichen Absinken eine kontinuierliche Intensitätszunahme über einen Zeitraum von zwei Jahren hinaus. Die Ergebnisse werden u. a. im Kontext des Konzepts der fortdauernden Bindungen diskutiert, und es werden Schlussfolgerungen für die klinische Praxis aufgezeigt.
Evaluative Priming in the Pronunciation Task
Authors: Klauer Karl Christoph , Becker Manuel , Spruyt Adriaan
Published: March 2016

Abstract. We replicated and extended a study by Spruyt and Hermans (2008) in which picture primes engendered an evaluative-priming effect on the pronunciation of target words. As preliminary steps, we assessed data reproducibility of the original study, conducted Pilot Study I to identify highly semantically related prime-target pairs, reanalyzed the original data excluding such pairs, conducted Pilot Study II to demonstrate that we can replicate traditional associative priming effects in the pronunciation task, and conducted Pilot Study III to generate relatively unrelated sets of prime pictures and target words. The main study comprised three between-participants conditions: (1) a close replication of the original study, (2) the same condition excluding highly related prime-target pairs, and (3) a condition based on the relatively unrelated sets of prime pictures and target words developed in Pilot Study III. There was little evidence for an evaluative priming effect independent of semantic relatedness.
Exploring the Subjective Feeling of Fluency
Authors: Forster Michael , Leder Helmut , Ansorge Ulrich
Published: March 2016

Abstract. According to the processing fluency theory, higher ease of processing a stimulus leads to higher feelings of fluency and more positive evaluations. However, it is unclear whether feelings of fluency are positive or an unspecific activation and whether feelings of fluency are directly attributed to the stimulus even without much positive feelings. In two experiments, we tested how variations in the ease of processing influenced feelings of fluency and affect, in terms of evaluations (Exp. 1) and physiological responses (Exp. 2). Higher feelings of fluency were associated with more positive stimulus ratings and did not affect stimulus arousal ratings, but perceivers’ feelings showed higher felt arousal ratings and left felt valence ratings unaffected. Physiological indices only showed small effects of a subtle positive reaction. These findings show that feelings of fluency can be sources of positive object evaluations, but do not affect one’s own positive feelings.
The Influence of Presentation Order on Category	Transfer
Authors: Mathy Fabien , Feldman Jacob
Published: March 2016

Abstract. This study of supervised categorization shows how different kinds of category representations are influenced by the order in which training examples are presented. We used the well-studied 5-4 category structure of Medin and Schaffer (1978) , which allows transfer of category learning to new stimuli to be discriminated as a function of rule-based or similarity-based category knowledge. In the rule-based training condition (thought to facilitate the learning of abstract logical rules and hypothesized to produce rule-based classification), items were grouped by subcategories and randomized within each subcategory. In the similarity-based training condition (thought to facilitate associative learning and hypothesized to produce exemplar classification), transitions between items within the same category were determined by their featural similarity and subcategories were ignored. We found that transfer patterns depended on whether the presentation order was similarity-based, or rule-based, with the participants particularly capitalizing on the rule-based order.
Sleeping Beauty transposase structure allows rational design of hyperactive variants for genetic engineering
Authors: Voigt Franka , Wiedemann Lisa , Zuliani Cecilia , Querques Irma , Sebe Attila , Mátés Lajos , Izsvák Zsuzsanna , Ivics Zoltán , Barabas Orsolya
Published: March 2016

Sleeping Beauty (SB) is a prominent Tc1/mariner superfamily DNA transposon that provides a popular genome engineering tool in a broad range of organisms. It is mobilized by a transposase enzyme that catalyses DNA cleavage and integration at short specific sequences at the transposon ends. To facilitate SB’s applications, here we determine the crystal structure of the transposase catalytic domain and use it to model the SB transposase/transposon end/target DNA complex. Together with biochemical and cell-based transposition assays, our structure reveals mechanistic insights into SB transposition and rationalizes previous hyperactive transposase mutations. Moreover, our data enables us to design two additional hyperactive transposase variants. Our work provides a useful resource and proof-of-concept for structure-based engineering of tailored SB transposases.
Towards repurposing the yeast peroxisome for compartmentalizing heterologous metabolic pathways
Authors: DeLoache William C. , Russ Zachary N. , Dueber John E.
Published: March 2016

Compartmentalization of enzymes into organelles is a promising strategy for limiting metabolic crosstalk and improving pathway efficiency, but improved tools and design rules are needed to make this strategy available to more engineered pathways. Here we focus on the Saccharomyces cerevisiae peroxisome and develop a sensitive high-throughput assay for peroxisomal cargo import. We identify an enhanced peroxisomal targeting signal type 1 (PTS1) for rapidly sequestering non-native cargo proteins. Additionally, we perform the first systematic in vivo measurements of nonspecific metabolite permeability across the peroxisomal membrane using a polymer exclusion assay. Finally, we apply these new insights to compartmentalize a two-enzyme pathway in the peroxisome and characterize the expression regimes where compartmentalization leads to improved product titre. This work builds a foundation for using the peroxisome as a synthetic organelle, highlighting both promise and future challenges on the way to realizing this goal.