Visible Imaging on the Pluto Fast Flyby Mission

Objectives for visible imaging of the Pluto-Charon system, as prescribed by the Outer Planets Science Working Group, are to acquire (1) global observations (FOV of approximately 5000 IFOV's) at 1 km/line-pair for the purpose of characterizing surface morphology and geology, (2) global observations in 3-5 broadband colors at 5-10 km/line-pair for studies of surface properties and composition as it relates to morphology, and (3) selected observations at higher spatial resolution for study of surface processes. Several factors of the Pluto Fast Flyby mission make these difficult to achieve. These factors along with other aspects of the mission are discussed

Planetary geomorphology research: FY 1990-1991

Progress in the following research areas is discussed: (1) volatile ice sublimation in a simulated Martian polar environment; (2) a global synthesis of Venusian tectonics; (3) a summary of nearly a decade of field studies of eolian processes in cold volcanic deserts; and (4) a model for interpretation of Martian sediment distribution using Viking observations. Some conclusions from the research are presented

Dome craters on Ganymede

Voyager observations reveal impact craters on Ganymede that are characterized by the presence of broad, high albedo, topographic domes situated within a central pit. Fifty-seven craters with central domes were identified in images covering approx. 50% of the surface. Owing to limitations in resolution, and viewing and illumination angles, the features identified are most likely a subset of dome craters. The sample appears to be sufficiently large to infer statistically meaningful trends. Dome craters appear to fall into two distinct populations on plots of the ratio of dome diameter to crater rim diameter, large-dome craters and small-dome craters. The two classes are morphologically distinct from one another. In general, large dome craters show little relief and their constituent landforms appear subdued with respect to fresh craters. The physical attributes of small-dome craters are more sharply defined, a characteristic they share with young impact craters of comparable size observed elsewhere in the solar system. Both types of dome craters exhibit central pits in which the dome is located. As it is difficult to produce domes by impact and/or erosional processes, an endogenic origin for the domes is reasonably inferred. Several hypotheses for their origin are proposed. These hypotheses are briefly reviewed

The effect of desiccation on the emission of volatile bromocarbons from two common temperate macroalgae

Exposure of intertidal macroalgae during low tide has been linked to the emission of a variety of atmospherically-important trace gases into the coastal atmosphere. In recent years, several studies have investigated the role of inorganic iodine and organoiodides as antioxidants and their emission during exposure to combat oxidative stress, yet the role of organic bromine species during desiccation is less well understood. In this study the emission of dibromomethane (CH2Br2) and bromoform (CHBr3) during exposure and desiccation of two common temperate macroalgae, Fucus vesiculosus and Ulva intestinalis, is reported. Determination of the impact exposure may have on algal physiological processes is difficult as intertidal species are adapted to desiccation and may undergo varying degrees of desiccation before their physiology is affected. For this reason we include comparisons between photosynthetic capacity (Fv/Fm) and halocarbon emissions during a desiccation time series. In addition, the role of rewetting with freshwater to simulate exposure to rain was also investigated. Our results show that an immediate flux of bromocarbons occurs upon exposure, followed by a decline in bromocarbon emissions. We suggest that this immediate bromocarbon pulse may be linked to volatilisation or emissions of existing bromocarbon stores from the algal surface rather than the production of bromocarbons as an antioxidant response

Forecasting Data Center Resource Usage With Artificial Neural Networks

Abstract. This thesis theoretical part presents some traditional time series forecasting methods (ARIMA) and recurrent neural network methods (LSTM and GRU) combined with convolution layer. The training process (backpropagation) of neural network is also explained in this thesis, and different algorithms to optimize the learning. Multiple metrics for evaluating forecast accuracy, and data preprocessing techniques are also introduced in theory section. The practical side of this thesis focuses on predicting real-world resource usage data of data center. In the analysis section grid search for optimal hyperparameters of the models is performed. Based on the results found in hyperparameter optimization multiple different neural network architectures are compared with each other taking into account forecasting accuracy and the computational complexity of training the model. The main result is that the recurrent neural network architecture GRU with convolution layer outperforms other models in forecast accuracy and in the time required to train the model. Proposed model can be effectively applied to load prediction as a part of data center computing cluster.Tiivistelmä. Tämä työ esittelee koneoppimismenetelmiä sekä tilastollisia menetelmiä aikasarjojen ennustamiseen palvelinkeskus kontekstissa. Työn teoriosuus lähtee liikkelle aikasarjojen esikäsittelystä, jossa esitellään aikasarjojen differensointi sekä minimi-maksimi menetelmä aikasarjojen skaalaukselle. Tällä skaalausmenetelmällä saadaan eri skaalalla olevat aikasarjat vertailukelpoisiksi syötteiksi neuroverkolle. Aikasarjojen esikäsittelyn jälkeen työ siirtyy aikasarjojen ennustamisen pariin. Mallintamismenetelmänä esitellään perinteinen tilastotieteen ARIMA -malli ja koneoppismenetelmänä kaksi erilaista takaisinkytkettyä neuroverkkoarkkitehtuuria, LSTM ja GRU. Ennen takaisinkytkettyjen neuroverkkojen esittelyä työ kertoo neuroverkkojen perusidean, ja millä tavalla neuroverkot oppivat. Lisäksi koneoppimispuolelta esitellään kuvantunnistuksesta tuttu konvoluutiokerrosta hyödyntävä neuroverkkoarkkitehtuuri muokattuna aikasarjoille sopivaksi. Neuroverkkojen esittelyn jälkeen syvennetään neuroverkkojen ominaisuuksiin ja opetukseen liittyviä yksityiskohtia: Työssä esitellään kolme usein neuroverkoissa käytettyä epälineaarista aktivaatiofunktiota neuroverkon opetusvaiheessa tarvittavineen derivaattoineen. Tämän jälkeen työ esittelee kaksi optimointialgoritmia neuroverkon parametrien päivittämistä varten, ja yhden optimointialgoritmin jota käytetään ARIMA -mallin parametrien optimoimiseen. Lopuksi teoriaosuudessa esitellään erilaisia aikasarjoihin ja ennustevirheen suuruuteen liittyviä tunnuslukuja. Teoriaosuuden jälkeen seuraa työn käytännön osuus. Tässä osuudessa käytetään ensin perättäishakua löytämään parhaat mahdolliset hyperparametrien arvot eri neuroverkkoarkkitehtuureille. Perättäishaulla saatuja tuloksia käytetään hyödyksi ennustaessa tulevaa oikean palvelinkeskuksen resurssin käyttöastetta kaikilla teoriaosuudessa esiteltyjen menetelmien avulla. Tämän jälkeen käytännön osuudessa vertaillaan eri mallien ennustetarkuutta, sekä mallien opetukseen kuluvaa aikaa. Tärkeimpänä tuloksena työssä saatiin esille, että takaisinkytketty neuroverkkoarkkitehtuuri GRU konvoluutiokerroksella antoi tarkimmat ennusteet tulevalle palvelinkeskuksen resurssien tarpeelle, lyhentäen samalla mallin opettamiseen tarvittavaa aikaa

Galaxy destruction and diffuse light in clusters

Deep images of the Centaurus and Coma clusters reveal two spectacular arcs of diffuse light that stretch for over 100 kpc, yet are just a few kpc wide. At a surface brightness of m_b \sim 27-28th arcsec^-2, the Centaurus arc is the most striking example known of structure in the diffuse light component of a rich galaxy cluster. We use numerical simulations to show that the Centaurus feature can be reproduced by the tidal debris of a spiral galaxy that has been tidally disrupted by the gravitational potential of NGC 4709. The surface brightness and narrow dimensions of the diffuse light suggest that the disk was co-rotating with its orbital path past pericentre. Features this prominent in clusters will be relatively rare, although at fainter surface brightness levels the diffuse light will reveal a wealth of structure. Deeper imaging surveys may be able to trace this feature for several times its presently observed extent and somewhere along the tidal debris, a fraction of the original stellar component of the disk will remain bound, but transformed into a faint spheroidal galaxy. It should be possible to confirm the galactic origin of the Centaurus arc by observing planetary nebulae along its length with redshifts close to that of NGC 4709.Comment: Replaced with version accepted by MNRAS (Dec. 1999): Added missing reference (to pg. 4 & reference list). Section 3 shortened; removed three figures. Now 8 pages long, with 8 figures. Low resolution images included, high resolution version available at http://star-www.dur.ac.uk:80/~calcaneo/cenarc.htm

Galilean satellite geomorphology

Research on this task consisted of the development and initial application of photometric and photoclinometric models using interactive computer image processing and graphics. New programs were developed to compute viewing and illumination angles for every picture element in a Voyager image using C-matrices and final Voyager ephemerides. These values were then used to transform each pixel to an illumination-oriented coordinate system. An iterative integration routine permits slope displacements to be computed from brightness variations, and correlated in the cross-sun direction, resulting in two dimensional topographic data. Figure 1 shows a 'wire-mesh' view of an impact crater on Ganymede, shown with a 10-fold vertical exaggeration. The crater, about 20 km in diameter, has a central mound and raised interior floor suggestive of viscous relaxation and rebound of the crater's topography. In addition to photoclinometry, the computer models that have been developed permit an examination on non-topographically-derived variations in surface brightness

Report of the Terrestrial Bodies Science Working Group. Volume 2: Mercury

The objectives and rationale for scientific investigation of Mercury are explored. Knowledge already obtained by astronomical observations and Mariner 10 spacecraft is reviewed and measurements required for the principal scientific goals are described. The use of low thrust propulsion systems is recommended so that maximum scientific return may be achieved and the reconnaissance phase of Mercury exploration may be completed in a single mission. Accelerated development is recommended on solar electric propulsion, solar sails, passive and active cooling mechanisms, and single rough landers

Report of the Terrestrial Bodies Science Working Group. Volume 4: The moon

A rationale for furture exploration of the moon is given. Topics discussed include the objectives of the lunar polar orbiter mission, the mission profile, and general characteristics of the spacraft to be used

Report of the Terrestrial Bodies Science Working Group. Volume 3: Venus

The science objectives of Pioneer Venus and future investigations of the planet are discussed. Concepts and payloads for proposed missions and the supporting research and technology required to obtain the desired measurements from space and Earth-based observations are examined, as well as mission priorities and schedules