Wim Penninx

Traditioneel behoort het bepalen van de functionaliteit van een applicatie en de implementatie daarvan tot het terrein van de eigenaren/gebruikers van de applicatie. Architecten beperken hun bijdrage tot infrastructurele randvoorwaarden in relatie tot zaken als operating systemen, databases, security issues. Dit artikel daagt de architect uit zich wel met de functionaliteit en implementatie te bemoeien. Hiermee kan hij voorkomen dat de kosten door extra maatwerk te hoog worden, dat er processen worden uitgevoerd die niet tot de taak van de applicatie-eigenaar behoren, en dat processen op meerdere plaatsen worden uitgevoerd. Dit laatste voorkomt dat gegevens in verschillende bestanden, en inconsistent, opgeslagen worden.

The two Exosat observations of 4U 1702 - 42 are reported. In one of them three bursts are detected. The bursts and the spectral and fast-temporal behavior of the persistent emission are analyzed. It is concluded that 4U 1702 - 42 is an atoll source, which was in the banana state when the bursts were present. The characteristics of the burst are similar to those of 4U 1636 - 53 in the banana state.

This article aims at researching the evolution of J-Z640 using an interdisciplinary approach in order to clarify the leading historical and anthropological events that shaped this particular branch of the human Y chromosome. We compiled a STR (short tandem repeat) and SNP (single nucleotide polymorphism) dataset of 145 known or predicted J-Z640 samples among the customers of Family Tree DNA and Full Genomes Corporation, as well as publicly available samples. Amongst these, we analyzed the results of 41 samples that had undergone Next-Generation Sequencing (NGS) and 32 samples that had undergone SNP testing using Sanger Sequencing. From this data, we constructed a J-Z640 phylogenetic tree that was dated using the method. Our data revealed that Haplogroup J-Z640 is a Y chromosome lineage found most notably, in several minority groups within the Near East such as the Samaritans, Druze, Armenians and Jews. J-Z640 originated during the Bronze Age, most likely in the Levant. During the Br...

X-ray observations of GX 17 + 2 were made in March and April, 1988 with the Large Area Counter of the Ginga satellite. The source was observed in the flaring, normal, and horizontal branches. Quasi-periodic oscillations (QPOs) were oberved in all three of these branches. The relationship between QPO behavior and the X-ray spectral properties of GX 17 + 2 is examined. Continuous variation of QPO behavior is observed as GX 17 + 2 moves from the normal to flaring branch, indicating that the normal-branch QPO and the flaring-branch QPO are probably one physical phenomenon. This QPO behavior is similar to that observed in Sco X-1. Also, it is found that GX 17 + 2 is an example of the Z-type sources defined by Hasinger et al. (1989).

The results of an analysis of two Exosat observations (July 1984, May 1986) of the highly variable X-ray burst source 4U 1608-52 are presented. During both observations the persistent X-ray flux was low (quiescence), and the persistent X-ray spectrum could be well fitted with a power-law model, with approximately the same index, but a somewhat different low-energy cut off. During both observations one type 1 burst was seen. It is shown that the relation between color temperature and effective temperature differs markedly from simple relations derived from theoretical models. A dip in the bolometric flux occurred near the peak of the 1986 burst. Possible models for this dip are discussed.

Updated abstract; in this document i analysed Y-DNA from yfull and ftdna from the Maghreb. I concluded that the present descendants of E-M81 most likely originate from Phoenicia. The majority of males in the Maghreb has a Y-DNA that descends from a male line ancestor that lived in Carthage about 500 BCE. This founding father effect is extremely strong and a similar founding mother effect is absent. About 20% has a Y-DNA that originates in Hejaz (Arabia) and arrived at the Muslim Conquest of the Maghreb. The Berber population has a lower Y-DNA percentage from Hejaz. A timescale correction of yfull +10% is more likely than a timescale of yfull without correction or a timescale correction of yfull +20%.

In a second document (not yet stored), I conclude that it is more likely that the E-M81 male ancestor line has his origin near Carthage than originate in Phoenicia.

INLEIDING De kosten van de ICT-infrastructuur zijn aan-zienlijk. Voor de financiële bedrijfstak in de VS geldt bijvoorbeeld een gemiddeld percentage van 14% van de totale exploitatiekosten (Weil, P. en Broadbent, M., 1998). Om deze kosten te vergelijken, te beheersen en te besturen zijn de afgelopen jaren verschillen-de methoden gepresenteerd, onder termen als TCO (Total Cost of Ownership, de tota-le kosten voor de eigenaar), TEI (Total Economic Impact) en ROI (Return On Investment). De toepassing van verschillende modellen in dezelfde situatie kan tot sterk verschillende resultaten leiden. Bovendien brengen de allereerste modellen de ICT-kosten niet direct in verband met opbrengsten; de laatste jaren verschijnen publicaties die dit manco ophef-fen, zie bijvoorbeeld het IT Beheer Jaarboek 2003 (Bon, J. van, 2003). In veel gevallen blijkt dat intensief rekenwerk in een complex model nodig is om resultaten te verkrijgen, wat vervolgens ten koste gaat van inzicht, overzicht en overdraagbaarheid. In alle gevallen moeten de gegevens van de bestaande financiële administratie onderge-bracht worden in de datastructuur van het model. Echter, kostensoorten zoals hard-of software worden in het algemeen niet gebruikt bij de financiële registratie van mid-delen. Deze eenmalige conversie en invoer is een intensieve maar noodzakelijke actie. Afhankelijk van het model zijn vervolgens de effecten van wijzigingen van b.v. ICT-infrast-ructuur, ander type clients of andere applica-ties eenvoudiger of moeilijker te maken. De auteurs presenteren in dit artikel een een-voudige methode, die zo transparant moge-lijk de ICT-kosten vertaalt naar de opbreng-sten voor de afnemer, waarbij de afnemer b.v. een afdeling of een bedrijfsproces kan zijn. Bij de invoering van de kostencatego-rieën worden de categorieën van Gartner toegepast. OVERZICHT MODELLEN Inleiding Dit hoofdstuk geeft een overzicht van beken-de TCO-, TEI-en ROI-modellen: Gartner, Forrester Research, META Group, GIGA Information Group, Microsoft Windows en TCO, het Bedrijfsmodel voor ICT, en het model van Looijen & van der Vorst. Ze wor-den stuk voor stuk kort toegelicht. Omdat de auteurs het vergroten van kostenbewustzijn door middel van een zo groot mogelijke IT Service Management, best practices Cross References 459 6 ICT-kosten: theorie in praktijk T egenover kosten moeten opbrengsten staan. Het proces om ICT-kosten te vertalen naar opbrengsten blijkt niet eenvoudig te zijn. Hoe doorzichtiger deze vertaling echter is, hoe eerder betrokken partijen kostenbewust worden. Na de behandeling van enkele bekende modellen presenteren de auteurs een aanpak, die zo transparant mogelijk de ICT-kosten vertaalt naar afnemers. Het laatste hoofdstuk schetst hoe het model wordt toegepast in de praktijk. Auteurs: Wim Penninx en Henk Groen (BT Syntegra) 6.5

In beveiliging en risico's worden de volgende onderwerpen besproken: de mogelijke gevolgen van onveiligheid, de oorzaken van de problemen, de toenemende belangstelling voor beveiliging, mogelijke benaderingswijzen van security, enkele beheersaspecten en hoe men een overgang van insecure (onveilig) naar secure kan maken.

In this article of 2012 I showed the results of simulations of population growth in Europe (starting 8000 years before present), respectively Flanders, Brabant and Limburg (FBL) and how it affects the variability of Y-DNA. I showed that the general SNP-variability of the European SNP-variability fits the simulations, if we use a higher population growth than was presented in [1]. The measured STR-variability in FBL fits the population growth of the last 2000 years.  The presentation was held at the XXXth International Congress of Genealogical and Heraldic Sciences in Maastricht, 2012.

Observations obtained with the Infrared Astronomical Satellite (IRAS) of a sample of well studied OH/IR stars, for which accurate distances are available, are presented and analyzed. A bolometric correction is determined as a function of the 12 micron to 25 micron flux ratio and bolometric magnitudes are derived. With help of the 'radio' periods time averaged luminosities could be determined. The luminosity function of stars on the asymptotic giant branch is constructed and compared with the expectation from the distribution of stars on the main-sequence and their lifetimes. The long wavelength emission is used to find the mass loss rates, the optical depth of the circumstellar dust shells, and the dust to gas ratio by mass. The results for this sample, selected on their radio properties, are applicable to a much larger set of IRAS sources for which data from other wavelength regimes are not available.

A method is described which allows, in principle, the gravitational redshift to be determined from the surface of a neutron star from observations of bursts with radius expansion. Results obtained from an application of this method to four burst sources are reported in detail. It is found that the method is very sensitive to systematic errors.

During about 80 h of uninterrupted observations of the X-ray burst source 4 U/MXB 1735-44, made in August 1985 with Exosat, five bursts were observed. The bursts occur at irregular intervals, ranging between 30 min and 36 h. The burst sizes do not scale with the intervals preceding the bursts; in particular the energy in a burst which occurred after an interval of 50 min was only 30 percent less than that of a burst which occurred after more than 20 h. Due to the long uninterrupted observations possible with Exosat, this is the first time for 1735-44 that the burst intervals and the burst characteristics (e.g., fluence) can be compared. The observations show that the model recently proposed by Fujimoto et al. (1987) to explain irregular burst intervals, is not applicable to 1735-44. The amplitude of periodic X-ray flux variations at the 4.65 h orbital period is less than 4 percent.

A detailed analysis is presented of the importance of Comptonization in burst and persistent spectra of the low-mass X-ray binary 4U/MXB 1636-53, and from this analysis it is inferred that the inner accretion flow is geometrically thin. It is found that burst spectra of 1636-53 are very nearly Planckian in shape; from an upper limit to a high-energy excess in these spectra it is inferred that the Thomson scattering optical depth of a possible intervening hot cloud must be less than 1 during bursts, and that the Compton y parameter of that cloud must be less than 0.5. During persistent emission, Thomson optical depth of 4-8, an electron temperature of 2-5 keV, and a value of 0.8-1.1 for y are inferred.

A review of the different groups of radio emitting X-ray sources is given. The sources are described along the lines of their X-ray characteristics. Emphasis is placed on the developments in the X-ray/radio correlations in the Z-sources. Some characteristics of the Z-sources are used to determine their distances. The atoll sources, the other group of the persistent bright low mass X-ray binaries, appear to be weaker at radio wavelengths than the Z-sources.

The IUE results obtained during two multiwave-length campaigns are presented. Simultaneous observations taken with the Japanese X ray satellite Ginga and numerous ground based radio and optical facilities are included. Cyg X-2 and Sco X-1 are low mass X ray binaries. The simultaneous UV/X ray observations show that there is a direct relationship between the strengths of the UV continuum and line fluxes and the placement of the X ray spectrum in one of the spectral branches. The strengths increase monotonically along the Z with the least UV emission in the horizontal branch and the most in the flaring branch. Models predicting UV continuum emission from the X ray heated surface of the companion star and an X ray illuminated accretion disk were developed. The data/model comparison suggests that X ray heating of the accretion disk is the dominant source of UV emission and that the mass accretion rate increases monotonically along the Z.

The low-mass X-ray binary 2S 0921-630 has an orbital period of 9 d and therefore might be a Z source. To test this, we have performed 6 cm continuum observations of the low-mass X-ray binary 2S 0921-630 using the Australia Telescope Compact Array. The source was not detected, and we determined an upper limit of 0.5 mJy (4 sigma) at 4.8 GHz. Comparing with earlier observations, we estimate that the probability that 2S 0921-630 has similar radio properties as prototype Z source Cyg X-2 is about 4 percent.

We present the results of an analysis of simultaneous X-ray (Ginga) and radio Very Large Array (VLA) observations of the Z source GX 340+0. We find GX 340+0 in different X-ray states at the times of the radio observations. We find some evidence for a global correlation between X-ray state and radio flux on a time scale of days; however, this correlation does not hold on shorter time scales.

Recently two groups of luminous low-mass X-ray binaries have been recognized, i.e., the Z sources and the atoll sources, with common X-ray spectral, X-ray timing, optical, ultraviolet and radio behavior. One of the Z-type sources, Sco X-1, is known to have radio lobes. A search was conducted for radio lobes in the Z source GX 17 + 2; none were detected.

During 1989 March 30 to April 2, Circinus X-1 was monitored at 5 GHz by one or other of a pair of two-element Australia Telescope interferometers and the Hartebeesthoek antenna, South Africa, and by the Ginga satellite in the 1-37 keV energy range. The observations show that Cir X-1 now has a very low level of radio emission, unlike the late 1970s and early 1980s, during which intense flare activity often occurred near zero orbital phase. Also, the X-ray behavior is strange in that it does now show the usual spectral states seen in low-mass X-ray binaries, yet exceeds the Eddington limit during flaring episodes.

... (1980). The simultaneous X-ray observations using the Ginga satellite captured two spectral branches (NB and FB) and their associated QPO modes (Hertz et al. 1991). ... KRV91 also obtain an E(B - V) of 0.3 using the average Galactic extinction law of Savage & Mathis (1979). ...

During EXOSAT observations of 4U/MXB 1636-53 in 1985 August, three bursts were observed in 6 hr and 24 bursts in 79 hr of uninterrupted observing. The persistent X-ray flux varied by about a factor of 2.4, the burst intervals by a factor of 24 (from 35 minutes to 14 hr), and the integrated burst fluxes (the burst fluences), and burst

Published data on X-ray bursts is analyzed, assuming that the peak luminosity of X-ray bursts with radius expansion is a standard candle and that the ratio of the anisotropy factors, xi(b) and xi(p) (Sztajno et al., 1987) is the same for all burst sources. It is shown that the effective burst duration, defined as the ratio of burst fluence to maximum burst flux, is strongly anticorrelated with the persistent luminosity. A positive correlation with the persistent luminosity of the ratio of the average persistent flux to the time-averaged burst flux is found. It is concluded that, independent of the accretion rate, after a given waiting time burst sources produce bursts with approximately the same (average) energy. This suggests that continuous stable burning of a sizeable fraction of the nuclear fuel is a general phenomenon on the surface of accreting neutron stars. It is suggested that this fraction is a gradually increasing function of the accretion rate.

... 4.1.3.22 Persistently bright X-ray sources Studiess over the last few years, culminating in the recent work by Hasinger and van der Kliss (1989), have shown that the bright low-mass X-ray binaries can be divided into twoo groups, the so-called 'Z sources' and 'atoll sources'. ...

A search for quasi-periodic oscillations (QPOs) in 4U/MXB 1735-44 was performed using Exosat observations during which the source was in a horizontal branch of the spectral hardness-intensity diagram for about 8 hr and in a normal branch type of behavior for about 46 hr. No QPOs or low-frequency noise was found in the horizontal branch state. It is suggested that this absence is due to either low luminosity or the fact that the companion in 1735-44 is a main-sequence star.

X-ray observations of the Z source GX 340 + 0 with the Ginga Observatory have found the source in three spectral states: the flaring branch (FB), the normal branch (NB) and the horizontal branch (HB). In accordance with previous observations, quasi-periodic oscillations (QPO) with frequencies 32-50 Hz were observed in the HB and near 6 Hz in a portion of the NB. In the HB the power spectra also showed low-frequency noise (LFN). The fractional rms variation of both types of QPO and of the LFN were strongly dependent on the X-ray energy band. Rough values for all three were about 2 percent at about 3 keV and about 8 percent at about 12 keV.

The two Exosat observations of 4U 1702 - 42 are reported. In one of them three bursts are detected. The bursts and the spectral and fast-temporal behavior of the persistent emission are analyzed. It is concluded that 4U 1702 - 42 is an atoll source, which was in the banana state when the bursts were present. The characteristics of the burst are similar to those of 4U 1636 - 53 in the banana state.

The optical counterpart of the Z source GX 349 + 2 was identified with an 18th magnitude star, whose spectrum shows strong H-alpha-emission. If this emission originates from rotating material in an accretion disk around the neutron star, a lower limit to the orbital period of 1.0 x sin-cubed (i) day is derived. If the companion is a giant, for spectral type G5 and M2 upper limits to the orbital period of 11.2 and 19.5 days, respectively are derived. The reddening toward the source is A(v) about 5.

Type-II bursts with durations ranging from about 2 to about 680 seconds are examined to study burst-peak fluxes, burst intervals, integrated energies, and luminosities associated with MXB 1730-335, the Rapid Burster. The data regarding the bursts are compared to develop general correlations between burst variables, and some general characteristics of the neutron star are theorized. As the bursts increase in duration, the flat top of the bursts increases and the number of oscillations during burst decay increase in a limited manner. Strong correlations are observed between bolometric peak fluxes, burst fluxes, and average persistent fluxes. The radiation during a type-II burst is considered to come from a photosphere with a larger radius for higher burst-accretion rates. The observational characteristics of the blackbody radii are employed to derive the magnetic dipole field-strength of the star and source zone of the bursts. Explanations are given for the spectrum of the persistent emission and the observational characteristics of the persistent emission in relation to the bursts.

X-ray observations of GX 17 + 2 were made in March and April, 1988 with the Large Area Counter of the Ginga satellite. The source was observed in the flaring, normal, and horizontal branches. Quasi-periodic oscillations (QPOs) were oberved in all three of these branches. The relationship between QPO behavior and the X-ray spectral properties of GX 17 + 2 is examined. Continuous variation of QPO behavior is observed as GX 17 + 2 moves from the normal to flaring branch, indicating that the normal-branch QPO and the flaring-branch QPO are probably one physical phenomenon. This QPO behavior is similar to that observed in Sco X-1. Also, it is found that GX 17 + 2 is an example of the Z-type sources defined by Hasinger et al. (1989).

This short draft paper was never published. It was written in 2013, distributed in social media and honours the work of Marko Heinila.

For a long time human Y-DNA has been analysed to determine the historic timescales of human phylogenetic trees. Two methods have been used intensively: STR and SNP mutation rates. The characteristics of both are very different. The normalization of each of the two methods has their own challenges. Although the systematic effects of both methods are completely different, the determined differences are limited. I conclude that both methods are useful to determine the historic timescales. The timescales that were determined by Marko Heinila should be corrected in the case of large timescales. Given the good fit of the two methods, it is likely that the systematic errors (that are not discussed in this paper) of both methods are less than 10%.

The Jewish diaspora is present in oral tradition [1]. The large population sizes of Jewish people in Eastern Europe has raised questions whether most of them are descendants of people that became Jewish in the Middle East (following the oral tradition) before the diaspora or became Jewish after the diaspora [2]. Recently a Y-DNA Jewish Ashkenazi branch (Levites, haplogroup R1a) was shown to follow the oral tradition [3]. In this document I will show that this is also the case for the J1-Z644, where the migration route passed Spain. The migration path followed the history from Semitic people in the Middle East to Iberia to Ashkenazi Jews. In these migration steps part of the people stayed in the originating area, and part of the people started a live in a new part of the world. In this document it is shown that haplogroup J1-Z640 originated most-likely in the Middle East. A group of the male descendants people went to Spain. Near the year 900-1100 CE one of these men had three male descendants, which resulted in three branches. The descendant of one of these three went to eastern Europe, which resulted in a large group of Ashkenazi Jewish. The data follow the Jewish migration out of the Middle East, a stay in Spain [1], and a migration to Eastern Europe. It does not follow the theory that most of the descendants of the Ashkenazi Jews became Jewish in the kingdom of the Khazars [2].

The article was written in feb. 2014, but never published (lack of priority).

The article was originally named "J1-Z644: Y-DNA in a successive migration from Semitic to Sephardi to Ashkenazi". It was later realized that the term Sephardi is better replaced by Iberia.

A person can be an employee in a source system for employees and a student in a source system for students. This might result in multiple identities. The pro's and con's are discussed, and a plan to have one identity for a person is discussed.

Er is onderzoek gedaan naar regionale endogamie in het autosomale DNA van Gemert in Noord-Brabant. Endogamie is het kenmerk waarbij huwelijkskandidaten binnen een kleine kring gezocht worden. Dit fenomeen heeft herkenbare kenmerken in het DNA, en is bijvoorbeeld sterk zichtbaar in gesloten populaties, zoals de Ashkenazi Joden in Europa. In dit webinar wordt getoond dat deze endogamie DNA-kenmerken ook meetbaar zijn in een lokale dorpsgemeenschap, zoals Gemert. In deze presentatie deelt hij zijn bevindingen. https://education.myheritage.nl/webinar/regionale-endogamie-in-gemert-nederland/