Kokorunkoaseman kautta tehtyjen tilauserien analysointi ja ohjaus sahateollisuudessa

Tutkimuksessa analysoitiin erään sahateollisuusyrityksen sahatavarakauppoja, joihin katkottiin tukkeja yrityksen kokorunkoasemalla. Tavoite oli kaksijakoinen: ensinnäkin analysoida runkoaseman toimintaa ja laskea katkonnan kokonais-, sekä kuutiokohtaisia kustannuksia eri runkomäärillä. Toiseksi pyrittiin luomaan tilauseräkohtainen kustannuslaskentamalli sellaisille sahatavarakaupoille, joihin kuuluu pituusehtoja. Kustannuslaskentamallissa sovellettiin lähinnä toimintolaskennan tapaa siltä osin, kuin sitä voitiin divergoivaan valmistusprosessiin soveltaa. Teoreettisen tutkimuksen pääpaino on hinnoittelussa, koska laskentamallin tarkoitus on avustaa myyntiä hintapäätöksiä tehdessä. Hinnoittelusta käsitellään eri hinnoittelustrategiat, -menetelmät, sekä mitä yrityksen tulee ottaa huomioon hinnoittelussa sellaisissa tilanteissa, kun markkinatilanteet vaihtelevat. Teoriaosuudessa käsitellään myös erilaisia kustannuslaskentatapoja, joista pääpaino annetaan toimintolaskennalle. Lopuksi on analysoitu laskentamallista saatavia hyötyjä, sekä sitä mihin sitä voidaan parhaiten käyttää. Vastaavasti arvioitiin millaisia puutteita laskentamallista löytyy, mitä kehittämisen kohteita siinä voisi olla.

Gaia photometry for white dwarfs

Context. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint only the nearby (~ 20 pc) sample is reasonably complete. The Gaia space mission will drastically increase the sample of known white dwarfs through its 5-6 years survey of the whole sky up to magnitude V = 20-25. Aims. We provide a characterisation of Gaia photometry for white dwarfs to better prepare for the analysis of the scientific output of the mission. Transformations between some of the most common photometric systems and Gaia passbands are derived. We also give estimates of the number of white dwarfs of the different galactic populations that will be observed. Methods. Using synthetic spectral energy distributions and the most recent Gaia transmission curves, we computed colours of three different types of white dwarfs (pure hydrogen, pure helium, and mixed composition with H/He = 0.1). With these colours we derived transformations to other common photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbers of white dwarfs predicted to be observed by Gaia. Results. We provide relationships and colour-colour diagrams among different photometric systems to allow the prediction and/or study of the Gaia white dwarf colours. We also include estimates of the number of sources expected in every galactic population and with a maximum parallax error. Gaia will increase the sample of known white dwarfs tenfold to about 200 000. Gaia will be able to observe thousands of very cool white dwarfs for the first time, which will greatly improve our understanding of these stars and early phases of star formation in our Galaxy.

All-sky search algorithms for monochromatic signals in bar gravitational wave detector data

In this paper we design and develop several filtering strategies for the analysis of data generated by a resonant bar gravitational wave (GW) antenna, with the goal of assessing the presence (or absence) therein of long-duration monochromatic GW signals, as well as the eventual amplitude and frequency of the signals, within the sensitivity band of the detector. Such signals are most likely generated in the fast rotation of slightly asymmetric spinning stars. We develop practical procedures, together with a study of their statistical properties, which will provide us with useful information on the performance of each technique. The selection of candidate events will then be established according to threshold-crossing probabilities, based on the Neyman-Pearson criterion. In particular, it will be shown that our approach, based on phase estimation, presents a better signal-to-noise ratio than does pure spectral analysis, the most common approach.

Cost Models for Routing and Wavelength Assignment in Wavelength-Division Multiplexing Optical Net

WDM (Wavelength-Division Multiplexing) optiset verkot on tällä hetkellä suosituin tapa isojen määrän tietojen siirtämiseen. Jokaiselle liittymälle määrätään reitin ja aallonpituus joka linkin varten. Tarvittavan reitin ja aallon pituuden löytäminen kutsutaan RWA-ongelmaksi. Tämän työn kuvaa mahdollisia kustannuksen mallein ratkaisuja RWA-ongelmaan. Olemassa on paljon erilaisia optimoinnin tavoitteita. Edellä mainittuja kustannuksen malleja perustuu näillä tavoitteilla. Kustannuksen malleja antavat tehokkaita ratkaisuja ja algoritmeja. The multicommodity malli on käsitelty tässä työssä perusteena RV/A-kustannuksen mallille. Myöskin OB käsitelty heuristisia menetelmiä RWA-ongelman ratkaisuun. Työn loppuosassa käsitellään toteutuksia muutamalle mallille ja erilaisia mahdollisuuksia kustannuksen mallein parantamiseen.

Executive functions profile in extreme eating/weight conditions: from anorexia nervosa to obesity

Extreme weight conditions (EWC) groups along a continuum may share some biological risk factors and intermediate neurocognitive phenotypes. A core cognitive trait in EWC appears to be executive dysfunction, with a focus on decision making, response inhibition and cognitive flexibility. Differences between individuals in these areas are likely to contribute to the differences in vulnerability to EWC. The aim of the study was to investigate whether there is a common pattern of executive dysfunction in EWC while comparing anorexia nervosa patients (AN), obese subjects (OB) and healthy eating/weight controls (HC).

Aktive Mobilität und Gesundheit : Hintergrundbericht für den nationalen Gesundheitsbericht 2015

Zu Fuss gehen und Velofahren tragen viel zu einer gesundheitsfördernden Bewegung bei. Die vielfältigen positiven Gesundheitseffekte regelmässiger Bewegung sind heute umfassend belegt. Ob in der Freizeit oder im Alltag, zu Fuss gehen und Velofahren - so genannte aktive Mobilität - können viel zu einer gesundheitsfördernden Bewegung beitragen. Zahlreiche Faktoren beeinflussen indessen die Neigung, zu Fuss zu gehen oder mit dem Velo zu fahren, darunter Wegeigenschaften, Alter, Fitness, aber auch Verkehrssicherheit und ganz allgemein die Merkmale von Quartieren und Städten. Die veränderbaren strukturellen Faktoren, insbesondere die Verkehrsinfrastruktur und -Sicherheit stehen im Zentrum zeitgemässer Förderung der aktiven Mobilität. Aus Sicht der Gesundheitspolitik ist eine intersektorielle Zusammenarbeit zwischen Gesundheitssektor und Verkehrs- und Städteplanung erstrebenswert. Bei den Überlegungen werden dadurch auch Gesundheitsfolgen fokussiert.

Long-term X-ray variability of the microquasar system LS5039/RX J1826.2-1450

We report on the results of the spectral and timing analysis of a BeppoSAX observation of the microquasar system LS 5039/RX J1826.2-1450. The source was found in a low-flux state with Fx(1-10 keV)= 4.7 x 10^{-12} erg cm^{-2} s^{-1}, which represents almost one order of magnitude lower than a previous RXTE observation 2.5 years before. The 0.1--10 keV spectrum is described by an absorbed power-law continuum with photon-number spectral index Gamma=1.8+-0.2 and hydrogen column density of NH=1.0^{+0.4}_{-0.3} x 10^{22} cm^{-2}. According to the orbital parameters of the system the BeppoSAX observation covers the time of an X-ray eclipse should one occur. However, the 1.6-10 keV light curve does not show evidence for such an event, which allows us to give an upper limit to the inclination of the system. The low X-ray flux detected during this observation is interpreted as a decrease in the mass accretion rate onto the compact object due to a decrease in the mass-loss rate from the primary.

On the multiwavelength spectrum of the microquasar 1E1740.7-2942

The microquasar 1E 1740.7-2942 is a source located in the direction of the Galactic Center. It has been detected at X-rays, soft gamma-rays, and in the radio band, showing an extended radio component in the form of a double-sided jet. Although no optical counterpart has been found so far for 1E 1740.7-2942, its X-ray activity strongly points to a galactic nature. Aims.We aim to improve our understanding of the hard X-ray and gamma-ray production in the system, exploring whether the jet can emit significantly at high energies under the light of the present knowledge. Methods.We have modeled the source emission, from radio to gamma-rays, with a cold-matter dominated jet model. INTEGRAL data combined with radio and RXTE data, as well as EGRET and HESS upper-limits, are used to compare the computed and the observed spectra. Results.From our modeling, we find out that jet emission cannot explain the high fluxes observed at hard X-rays without violating at the same time the constraints from the radio data, favoring the corona origin of the hard X-rays. Also, 1E 1740.7-2942 might be detected by GLAST or AGILE at GeV energies, and by HESS and HESS-II beyond 100 GeV, with the spectral shape likely affected by photon-photon absorption in the disk and corona photon fields.

Studying the non-thermal lobes of IRAS 16547-4247 through a multi-wavelength approach

In recent years, massive protostars have turned out to be a possible population of high-energy emitters. Among the best candidates is IRAS 16547-4247, a protostar that presents a powerful outflow with clear signatures of interaction with its environment. This source has been revealed to be a potential high-energy source because it displays non-thermal radio emission of synchrotron origin, which is evidence of relativistic particles. To improve our understanding of IRAS 16547-4247 as a high-energy source, we analyzed XMM-Newton archival data and found that IRAS 16547-4247 is a hard X-ray source. We discuss these results in the context of a refined one-zone model and previous radio observations. From our study we find that it may be difficult to explain the X-ray emission as non-thermal radiation coming from the interaction region, but it might be produced by thermal Bremsstrahlung (plus photo-electric absorption) by a fast shock at the jet end. In the high-energy range, the source might be detectable by the present generation of Cherenkov telescopes, and may eventually be detected by Fermi in the GeV range.

Primavistan Java-koodin obfuskointiprosessi

Tässä insinöörityössä suunniteltiin ja toteutettiin Gordion-talousohjaus Oy:n Primavista-ohjelmiston koodin suojaaminen. Yrityksellä oli jo pitkään ollut tarve Java-kielisen ohjelmakoodinsa suojaamiselle, etenkin Primavistan käytön tullessa laajentumaan useisiin eri maihin. Koodin suojaamisella hankaloitetaan mahdollista takaisinkääntämistä, jossa valmiin ohjelman ajettavat tiedostot käännetään takaisin niiden lähdekoodiksi. Tällöin lähdekoodia pystytään tarkastelemaan tai jopa muokkaamaan. Suomen tekijänoikeuslain mukaan takaisinkääntäminen ei ole sallittua. Työ aloitettiin tutkimalla erilaisia Java-koodin suojausmenetelmiä. Primavistan koodin suo-jausmenetelmäksi valittiin obfuskointi, joka on suosituin Java-koodin suojausmenetelmä. Erilaisia tekniikoita käyttäen tämä menetelmä sotkee Javan tavukoodia tehden takaisinkäännetystä koodista erittäin vaikeasti ymmärrettävää. Työssä vertailtiin nykyisiä obfuskointityökaluja itse tehdyn testisovelluksen avulla. Vertai-un parhaaksi työkaluksi osoittautui kaupallinen tuote Zelix KlassMaster. Ohjelma todettiin toimivaksi myös Primavistan suhteen, minkä jälkeen se päätettiin hankkia yritykselle. Koko Primavistan koodin obfuskointi toteutettiin Zelix KlassMasteria ja sen useita eri ob-fuskointitekniikoita käyttäen. Tämän jälkeen obfuskointi liitettiin Primavistan Ant-buildiin kiinteäksi osaksi koodin rakennusprosessia. Koska obfuskointi tekee huomattavia muu-toksia tavukoodiin, obfuskoidun Primavistan toiminta oli testattava huolellisesti. Testauk-sessa huomattiin pieniä virhetilanteita, jotka korjaamalla ohjelman toiminta lopulta todettiin normaaliksi. Viimeisessä työvaiheessa kaikki obfuskoinnissa tarvittavat tiedostot siirrettiin versionhallintaan kaikkien yrityksen kehitystiimin jäsenten käytettäviksi. Työn tuloksena saatiin onnistuneesti obfuskoiduksi koko Primavistan koodi. Obfuskointi-prosessista kehitettiin pysyvä käytäntö, jonka mukaisesti obfuskointi tehdään aina Prima-vistan rakennusvaiheessa. Jatkossa kaikki asiakkaille toimitettavat Primavistan versiot tulevat olemaan obfuskoituja sovelluksia.

Gamma-ray emission from massive young stellar objects

Context.Massive stars form in dense and massive molecular cores. The exact formation mechanism is unclear, but it is possible that some massive stars are formed by processes similar to those that produce the low-mass stars, with accretion/ejection phenomena occurring at some point of the evolution of the protostar. This picture seems to be supported by the detection of a collimated stellar wind emanating from the massive protostar IRAS 16547-4247. A triple radio source is associated with the protostar: a compact core and two radio lobes. The emission of the southern lobe is clearly non-thermal. Such emission is interpreted as synchrotron radiation produced by relativistic electrons locally accelerated at the termination point of a thermal jet. Since the ambient medium is determined by the properties of the molecular cloud in which the whole system is embedded, we can expect high densities of particles and infrared photons. Because of the confirmed presence of relativistic electrons, inverse Compton and relativistic Bremsstrahlung interactions are unavoidable. Aims.We aim to make quantitative predictions of the spectral energy distribution of the non-thermal spots generated by massive young stellar objects, with emphasis on the particular case of IRAS 16547-4247. Methods.We study the high-energy emission generated by the relativistic electrons which produce the non-thermal radio source in IRAS 16547-4247. We also study the result of proton acceleration at the terminal shock of the thermal jet and make estimates of the secondary gamma rays and electron-positron pairs produced by pion decay. Results.We present spectral energy distributions for the southern lobe of IRAS 16547-4247, for a variety of conditions. We show that high-energy emission might be detectable from this object in the gamma-ray domain. The source may also be detectable in X-rays through long exposures with current X-ray instruments. Conclusions.Gamma-ray telescopes such as GLAST, and even ground-based Cherenkov arrays of new generation can be used to study non-thermal processes occurring during the formation of massive stars.

A microquasar model applied to unidentified gamma-ray sources

Among unidentified gamma-ray sources in the galactic plane, there are some that present significant variability and have been proposed to be high-mass microquasars. To deepen the study of the possible association between variable low galactic latitude gamma-ray sources and microquasars, we have applied a leptonic jet model based on the microquasar scenario that reproduces the gamma-ray spectrum of three unidentified gamma-ray sources, 3EG J1735-1500, 3EG J1828+0142 and GRO J1411-64, and is consistent with the observational constraints at lower energies. We conclude that if these sources were generated by microquasars, the particle acceleration processes could not be as efficient as in other objects of this type that present harder gamma-ray spectra. Moreover, the dominant mechanism of high-energy emission should be synchrotron self-Compton (SSC) scattering, and the radio jets may only be observed at low frequencies. For each particular case, further predictions of jet physical conditions and variability generation mechanisms have been made in the context of the model. Although there might be other candidates able to explain the emission coming from these sources, microquasars cannot be excluded as counterparts. Observations performed by the next generation of gamma-ray instruments, like GLAST, are required to test the proposed model.

Optical spectroscopy of microquasar candidates at low Galactic latitudes

We report optical spectroscopic observations of a sample of 6 low-galactic latitude microquasar candidates selected by cross-identification of X-ray and radio point source catalogs for |b|<5 degrees. Two objects resulted to be of clear extragalactic origin, as an obvious cosmologic redshift has been measured from their emission lines. For the rest, none exhibits a clear stellar-like spectrum as would be expected for genuine Galactic microquasars. Their featureless spectra are consistent with being extragalactic in origin although two of them could be also highly reddened stars. The apparent non-confirmation of our candidates suggests that the population of persistent microquasar systems in the Galaxy is more rare than previously believed. If none of them is galactic, the upper limit to the space density of new Cygnus X-3-like microquasars within 15 kpc would be 1.1\times10^{-12} per cubic pc. A similar upper limit for new LS 5039-like systems within 4 kpc is estimated to be 5.6\times10^{-11} per cubic pc.

Abstracts of the refereed articles

Riitta Hänninen : The Meaning of Freedom in Snowboarding Culture, Inka Juslin : Dance narration and the feminine mimesis in Ob-Ugrian women•s dances, Pirjo Kristiina Virtanen : Multidimensional tradition : distinctions of native youths and their indigenous traditions in Brazilian Amazonia, Tea Virtanen : Pastoralists in Mecca : the moral economy of Mbororo pilgrimage

EVN+MERLIN observations of microquasar candidates at low galactic latitudes

In an attempt to increase the number of known microquasars, Paredes et al. (2002) have presented a long-term project focused on the search for new objects of this type. They performed a cross-identification between X-ray and radio catalogs under very restrictive selection criteria for sources with |b|<5 degrees, and obtained a sample of 13 radio-emitting X-ray sources. Follow-up observations of 6 of these sources with the VLA provided accurate coordinates, which were used to discover optical counterparts for all of them. We have observed these six sources with the EVN and MERLIN at 5 GHz. Five of the six objects have been detected and imaged, presenting different morphologies: one source has a two-sided jet, three sources have one-sided jets, and one source is compact. With all the presently available information, we conclude that two of the sources are promising microquasar candidates in our Galaxy.