Late-onset spinal motor neuronopathy- a new neuromuscular disease

The aim of this study was to clarify the clinical phenotype of late-onset spinal motor neuronopathy (LOSMoN), an adult-onset autosomal dominant lower motor neuron disorder identified first in two families in Eastern Finland, in order to clarify its genetic background. Motor neuron disorders (MNDs) are characterized by dysfunction and premature death of motor neurons in the brain and spinal cord. MNDs can manifest at any age of the human lifespan, ranging from pre- or neonatal forms such as spinal muscular atrophy type I (SMA I) to those preferentially affecting the older age groups exemplified by sporadic amyotrophic lateral sclerosis (ALS). With a combination of genetic linkage analysis and genome sequencing using DNA from a total of 55 affected members of 17 families and a whole genome scan, we were able to show that LOSMoN is caused by the c.197G>T p.G66V mutation in the gene CHCHD10. This study showed that LOSMoN has very characteristic features that help to differentiate it from other more malignant forms of motor neuron disease, such as ALS, which was erroneously diagnosed in many patients in our cohort. Lack of fibrillations in the first dorsal interosseus muscle on EMG and extensive grouping of non-atrophic type IIA/2A fibers on muscle biopsy were shown to be common findings in LOSMoN, but rare or absent in ALS patients. The results of this study will help clinicians recognize the characteristic phenotype of LOSMoN disease and thus improve their diagnostic accuracy, and will also allow physicians to provide adequate genetic counseling for patients.

Genesis and distribution of Mississippi Valley-type ore assemblages in Middle Silurian strata, Niagara Peninsula, Ontario /

Presently non-commercial occurrences of Mississippi Valley-type ore assemblages in the Middle Silurian strata of the Niagara Peninsula have been studied. Based on this detailed study, a new poly-stage genetic model is proposed which relates ore mineralization in carbonate environments to the evolution of the sedimentary basin. Sulphide ore mineralization occurred during two episodes: 1. During the late diagenesis stage, which is characterized by compaction-maturation of the sediments, the initial mineralization took place by upward and outward movement of connate waters. Metals were probably supplied from all the sediments regardless of their specific lithologies. However, clay minerals were possibly the main contributors. The possible source of sulphur was from petroleum-type hydrocarbons presently mixed with the sediments at the site of ore deposition. Evidence for this is the fact that the greatest abundance of ore minerals is in petroliferous carbonates. The hydrocarbons probably represent liquids remaining after upward migration to the overlying Guelph-Salina reservoirs. The majority of sphalerite and galena formed during this period, as well as accessory pyrite, marcasite, chalcopyrite, chalcocite, arsenopyrite, and pyrrhotite; and secondary dolomite, calcite, celestite, and gypsum. 2. During the presently ongoing surface erosion and weathering phase, which is marked by the downward movement of groundwater, preexisting sulphides were probably remobilized, and trace amounts of lead and zinc were leached from the host material, by groundwaters. Metal sulphides precipitated at, or below, the water table, or where atmospheric oxygen could raise the Eh of groundwaters to the point where soluble metal complexes are unstable and native sulphur co-precipitates with sphalerite and galena. This process, which can be observed today, also results in the transport and deposition of the host rock material. Breakdown of pre-existing sulphide and sulphate, as well as hydrocarbon present in the host rock, provided sulphur necessary for sulphide precipitation. The galena and sphalerite are accompanied by dolomite, calcite, gypsum, anglesite, native sulphur and possibly zincite.

The cloning and reconstitution of a bovine adenovirus type 2 E3 deletion mutant and the sequencing and analysis of the early 4 region

Recombinant Adenoviruses (Ads) have been shown to have potential applications in three areas: gene therapy, high level protein expression and recombinant vaccines.' At least three different locations within the Ad genome can be deleted and subsequently used for the insertion of foreign sequences. These include the Early 3 (E3), Early 1 (E1) and Early 4 (E4) regions. Viral vectors of this type have been well studied in Human Ads 2 and 5, however one has not yet been constructed for Bovine Adenovirus Type 2 (BAV2). The E3 region is located between 76.6 and 86 m.u. on the r-strand and is transcribed in a rightward direction. The gene products of the Early 3 region (E3) have been shown to be non-essential for viral replication, in vitro, but are required for host immunosurveillance. This study represents the cloning and reconstitution of a BAV2 E3 deletion mutant. A deletion of 1800bp was made within the E3 region of BAV2 and the thymidine kinase gene was subsequently inserted in the deleted area . . The plasmid pdlE3-4tk1 (23.4Kbp) was constructed and used to to facilitate homologous recombination with the wild type BAV2 to produce a mutant. Southern Blotting and Hybridization results suggest the presence of a BAV2 E3 deletion mutant with thymidine kinase sequences present. The E4 region of Human Adenovirus types 2 and 5 is located at the extreme right end of the genome (91.3 map units - 99.1 map units) and is transcribed in a leftward direction giving rise to a complicated set of differentially spliced mRNAs. Essentially there are 7 open reading frames (ORFs) encoding for at least 7 polypeptides. The gene products encoded by the E4 region have been shown to be essential for the expression of late viral genes, host cell shutoff and normal viral growth. We have cloned and sequenced the right end segment between 90.5 map units and 100 map units of the BAV2 genome. The results show several open reading frames which encode polypeptides exhibiting homology to three polypeptides encoded by the E4 region of human adenovirus type 2. These include the 14kDa protein encoded by ORF1, the 34kDa protein encoded by ORF6 and the 13kDa protein encoded by ORF3. The nucleotide sequence, restriction enzyme map, and ORF map of the E4 region could be very useful in future molecular manipulation of this region and could possibly explain the slow growth rate of BAV2 in MDBK cells.

Étude spectroscopique d'étoiles naines blanches riches en hélium de type DB et DBA

De nouveaux modèles d'atmosphère sont présentés, incluant les profils de raie d'hélium neutre améliorés de Beauchamp (1995) et le formalisme de probabilité d'occupation pour ce même atome. Ces modèles sont utilisés pour calculer une grille de spectres synthétiques correspondant à des atmosphères riches en hélium et contenant des traces d'hydrogène. Cette grille est utilisée pour déterminer les paramètres atmosphériques principaux des étoiles de notre échantillon, soient la température effective, la gravité de surface et l'abondance d'hydrogène. Notre échantillon contient des spectres visibles de haut rapport signal-sur-bruit pour 102 naines blanches riches en hélium, dont 29 ont été observés au cours de ce projet, ce qui en fait le plus grand échantillon de spectres de qualité de naines blanches riches en hélium. Des spectres synthétiques ont été calculés en utilisant différentes valeurs du paramètre α de la théorie de la longueur de mélange dans le but de calibrer empiriquement la valeur de ce paramètre pour les DB. Afin d'améliorer la précision sur les paramètres atmosphériques de quelques étoiles, nous avons utilisé des spectres couvrant la raie Hα pour mieux déterminer l'abondance d'hydrogène. Finalement, nous avons calculé la distribution de masse de notre échantillon et la fonction de luminosité des DB. La distribution de masse montre une coupure à 0.5 fois la masse solaire qui est prédite par les modèles d'évolution stellaire et dévoile une masse moyenne significativement plus élevée pour les étoiles de type DBA. La masse moyenne de l'ensemble des DB et DBA est très proche de celle des DA. La fonction de luminosité nous permet de calculer que le rapport du nombre de DB sur le nombre de DA vaut environ 25%.

Calculs de modèles d'atmosphères hors-ETL avec métaux pour les étoiles de type sdO : le cas particulier de SDSS J1600+0748

Nous présentons nos grilles de modèles d'atmosphères pour les étoiles sous-naines chaudes de type O (sdO) soit : des modèles classiques hors-ETL H, He, des modèles hors-ETL avec, en plus, du C, N, O et finalement des modèles incluant C, N, O, Fe. En utilisant les raies de Balmer et d'hélium dans le domaine du visible, nous avons fait des comparaisons entre les spectres théoriques de nos différentes grilles afin de caractériser les effets des métaux. On trouve que ces effets dépendent à la fois de la température et de la gravité. De plus, l'abondance d'hélium a une influence importante sur les effets des métaux; une abondance d'hélium faible (log N(He)/N(H) < -1,5) occasionne des effets assez importants alors qu'une abondance plus élevée tend à réduire ces mêmes effets. Nous avons aussi trouvé que l'ajout du fer (en abondance solaire) ne cause que des changements relativement faibles à la structure en température et, par le fait même, aux profils des raies d'hydrogène et d'hélium, par rapport aux changements déjà produits par le C, N, O (en abondance solaire). Nous avons utilisé nos grilles pour faire une analyse spectroscopique du spectre à haut signal sur bruit (180) et basse résolution (9 Å) de SDSS J160043.6+074802.9 obtenu au télescope Bok. Notre meilleure ajustement a été obtenu avec notre grille de spectres synthétiques incluant C, N, O et Fe en quantité solaire, menant aux paramètres suivants : Teff = 68 500 ± 1770 K, log g = 6,09 ± 0,07, and log N(He)/N(H) = -0,64 ± 0,05, où les incertitudes proviennent uniquement de la procédure d'ajustement. Ces paramètres atmosphériques, particulièrement la valeur de l'abondance d'hélium, placent notre étoile dans une région où les effets des métaux ne sont pas très marqués.

Évaluation des coûts de traitement de la tyrosinémie de type I

Réalisé dans le cadre d'un mandat de l'Unité d'évaluation des technologies et des modes d'intervention en santé (UETMIS) du CHU Sainte-Justine

A zooarchaeological analysis of a late Dorset faunal assemblage from the KcFs-2 site (Nunavik, Quebec).

Ce mémoire consiste en une analyse zooarchéologique d’un assemblage faunique provenant d’un site Dorsétien des Îles Nuvuk dans l’Arctique canadien. Les données fauniques ont été analysées statistiquement en appliquant des indices d’utilité économique et des indices de densité des os. Une étude concernant le niveau de conservation de l’assemblage a révélé peu d’évidence de modification taphonomique des spécimens. Les analyses fauniques ont permis d’identifier une stratégie de subsistance de type généraliste et basée sur l’exploitation de mammifères marins, surtout des phoques annelés, pratiquée par les occupants du site de KcFs-2. Une prédominance d’individus immatures (phoques annelés) dans l’assemblage indique une abondance de ressources marines dans les régions du nord de la Baie d’Hudson et du détroit d’Hudson au moment de l’occupation, ce qui est aussi manifeste dans des études antérieures concernant les économies des peuples du Paléoesquimau tardif pour la période donnée. L’occupation du site de KcFs-2 s’est produite durant la période du Dorsétien récent au Nunavik (1500-800 B.P.), et la séquence est définie comme ayant été multi-saisonnière (de l’hiver à l’été). L’analyse des produits de l’industrie osseuse (têtes de harpons et sculptures en ivoire) a permis de confirmer l’affiliation culturelle des occupants.

Étude de la fonction de luminosité des étoiles naines blanches de type DA dans le relevé Kiso

Mémoire numérisé par la Division de la gestion de documents et des archives de l'Université de Montréal

Étude de la variabilité spectroscopique d’un échantillon d’étoiles Wolf-Rayet de type WC9

Nous savons que la grande majorité des étoiles WC9 produit de la poussière à base de carbone. Cette dernière doit se former dans des zones de très haute densité afin de survivre à l’environnement hostile qu’est celui du vent d’une étoile WR. Les étoiles WC appartenant à un système binaire WR + O produisent de la poussière quand les vents des deux étoiles entrent en collision et forment une zone de choc pouvant augmenter la densité du gaz d’un facteur 1000. Par contre, plusieurs étoiles WC9 n’ont, à ce jour, montré aucun signe de la présence d’un compagnon. Le but du projet est de tenter d’identifier un mécanisme alternatif responsable de la formation de poussière dans les étoiles WC9 n’appartenant pas à un système binaire. Nous présentons les résultats d’une campagne d’observation visant à caractériser la variabilité spectroscopique d’un échantillon de huit étoiles WC9 et une étoile WC8d. Nos résultats indiquent que la majorité des étoiles montrent des variations à grande échelle dans la raie d’émission C III 5696, soit à un niveau d’au moins 5% du flux de la raie et que les structures dans le vent ont une dispersion de vitesses de l’ordre de 150-300 km/s. De manière générale, les variations de vitesse radiales sont anti-corrélées avec le coefficient d’asymétrie de la raie, ce qui semble infirmer la présence d’un compagnon. Des observations en photométrie de l’étoile WR103 montrent une période de 9.1 ± 0.6 jours qui s’accorde avec les variations spectroscopiques et qui ne semble pas, de manière évidente, d’origine binaire.

Dispersion de la couleur J-K des naines brunes de type L2

Les naines brunes sont des objets de masse intermédiaire entre celle nécessaire pour former une étoile et celle d'une planète. Les naines brunes sont classées, des plus chaudes aux plus froides, en types spectraux L, T et Y, caractérisés par une couleur J-K moyenne qui varie de 1.2 à 1.8 pour les étoiles de type L0 à L8, et de 1.8 à -0.5 pour les étoiles de type L8 à T8. Par ailleurs, la couleur J-K de certains types spectraux présente une dispersion de l'ordre d'une magnitude. Ce travail tente de faire la lumière sur la nature de cette grande dispersion, présente dans la couleur J-K des naines brunes de type L2. Les observations ont été réalisées avec la caméra infrarouge CPAPIR à l'Observatoire du Mont Mégantic. Nous avons ciblé un total de 22 naines brunes qui ont été observées en K, et 12 parmi celles-ci ont aussi été observées en J. Chacune des naines brunes a été calibrée à l'aide d'une étoile standard, ce qui rend nos résultats indépendants des données 2MASS. Nous observons une corrélation entre les couleurs J-K de nos données et de celles de 2MASS. Cela montre que la grande dispersion en J-K de nos données et des données 2MASS est due aux propriétés physiques des naines brunes et non à des erreurs observationnelles. L'examen des facteurs qui pourraient être responsables de cette grande dispersion, soit la classification spectrale, la métallicité, la gravité de surface, une binarité non résolue, la présence de nuages de condensats et la rotation, montre que la gravité de surface serait le facteur le plus susceptible d'être responsable de la grande dispersion des valeurs de J-K.

Daughters of Lilith : transgressive femininity in Bram Stoker’s late gothic fiction

Daughters of Lilith: Transgressive Femininity in Bram Stoker’s Late Gothic Fiction explore le thème de la transgression féminine dans quatre romans gothiques de Bram Stoker. En combinant les études féministes et les études de genre, cette thèse examine les différents visages de la dissidence féminine à travers Dracula (1897), The Jewel of Seven Stars (1903), The Lady of the Shroud (1909) et The Lair of the White Worm (1911). Dans ces textes, la transgression est incarnée par la femme hystérique, la mère monstrueuse, la femme exotique et la New Woman. De plus, le traitement de ces stéréotypes féminins révèle une certaine tolérance envers la dissension féminine chez l’auteur. Souvent perçu comme un écrivain conservateur, Stoker est plutôt qualifié de progressiste dans cette thèse. L’inclusion de personnages féminins forts et déterminés à travers ses romans ainsi que ses rapports avec plusieurs féministes et proto-féministes dans sa vie privée témoignent de sa libéralité envers les femmes. Sa largeur d’esprit semble d’ailleurs évoluer tout au long de sa carrière ainsi qu’avec la progression du mouvement suffragiste britannique, une période mouvante à la fin du dix-neuvième et au début du vingtième siècle.

Emergence of a new type of porcine circovirus (PCV) in swine: a type 1 and type 2 PCV recombinant.

In late September 2008, tissue samples from piglets experiencing an acute outbreak of porcine reproductive and respiratory syndrome (PRRS) were submitted to the Veterinary diagnostic service of the University of Montreal. Several diagnostic assays were performed including a multiplex real-time quantitative PCR assay (mrtqPCR) for the detection and differentiation of porcine circovirus (PCV) type 2a and 2b genotypes in the lung and lymph nodes. The pig samples were found to be positive for PCV2a using the mrtqPCR but odd results were obtained. The Ct values obtained with mrtqPCR probes targeting the ORF1 and ORF2 of PCV2 were not as expected which suggested the presence of genomic variations in the PCV2 viral genome. Ultimately, a total of three diagnostic cases with mrtqPCR unusual results were investigated. After virus isolation and sequence analyses, a new type of PCV was identified in those three cases. Based on sequence analyses, this new PCV genome contains the ORF1 of PCV1 and the ORF2 of PCV2a and its entire viral genome nucleotide identity compared to PCV1, PCV2a and 2b are 86.4%, 88.7% and 86.5%, respectively. It is proposed to name this new PCV by taking into account the nomenclature of Segales et al. (2008) and by indicating the origin of the ORF1 at first and the origin of the ORF2 in second. Consequently, the name proposed for this new PCV is PCV1/2a. The prevalence of PCV1/2a seems to be very low in Quebec, Canada (2.5% of PCV positive cases), and its origin is now in debate.

Studies on Quasinormal Modes and Late-time Tails in Black Hole Spacetimes

This thesis Entitled Studies on Quasinormal modes and Late-time tails black hole spacetimes. In this thesis, the signature of these new theories are probed on the evolution of field perturbations on the black hole spacetimes in the theory. Chapter 1 gives a general introduction to black holes and its perturbation formalism. Various concepts in the area covered by the thesis are also elucidated in this chapter. Chapter 2 describes the evolution of massive, charged scalar field perturbations around a Reissner-Nordstrom black hole surrounded by a static and spherically symmetric quintessence. Chapter 3 comprises the evolution of massless scalar, electromagnetic and gravitational fields around spherically symmetric black hole whose asymptotes are defined by the quintessence, with special interest on the late-time behavior. Chapter 4 examines the evolution of Dirac field around a Schwarzschild black hole surrounded by quintessence. Detailed numerical simulations are done to analyze the nature of field on different surfaces of constant radius . Chapter 5is dedicated to the study of the evolution of massless fields around the black hole geometry in the HL gravity.

Study on period search methods of variable stars: Application to ASAS and CRTS databases

Study on variable stars is an important topic of modern astrophysics. After the invention of powerful telescopes and high resolving powered CCD’s, the variable star data is accumulating in the order of peta-bytes. The huge amount of data need lot of automated methods as well as human experts. This thesis is devoted to the data analysis on variable star’s astronomical time series data and hence belong to the inter-disciplinary topic, Astrostatistics. For an observer on earth, stars that have a change in apparent brightness over time are called variable stars. The variation in brightness may be regular (periodic), quasi periodic (semi-periodic) or irregular manner (aperiodic) and are caused by various reasons. In some cases, the variation is due to some internal thermo-nuclear processes, which are generally known as intrinsic vari- ables and in some other cases, it is due to some external processes, like eclipse or rotation, which are known as extrinsic variables. Intrinsic variables can be further grouped into pulsating variables, eruptive variables and flare stars. Extrinsic variables are grouped into eclipsing binary stars and chromospheri- cal stars. Pulsating variables can again classified into Cepheid, RR Lyrae, RV Tauri, Delta Scuti, Mira etc. The eruptive or cataclysmic variables are novae, supernovae, etc., which rarely occurs and are not periodic phenomena. Most of the other variations are periodic in nature. Variable stars can be observed through many ways such as photometry, spectrophotometry and spectroscopy. The sequence of photometric observa- xiv tions on variable stars produces time series data, which contains time, magni- tude and error. The plot between variable star’s apparent magnitude and time are known as light curve. If the time series data is folded on a period, the plot between apparent magnitude and phase is known as phased light curve. The unique shape of phased light curve is a characteristic of each type of variable star. One way to identify the type of variable star and to classify them is by visually looking at the phased light curve by an expert. For last several years, automated algorithms are used to classify a group of variable stars, with the help of computers. Research on variable stars can be divided into different stages like observa- tion, data reduction, data analysis, modeling and classification. The modeling on variable stars helps to determine the short-term and long-term behaviour and to construct theoretical models (for eg:- Wilson-Devinney model for eclips- ing binaries) and to derive stellar properties like mass, radius, luminosity, tem- perature, internal and external structure, chemical composition and evolution. The classification requires the determination of the basic parameters like pe- riod, amplitude and phase and also some other derived parameters. Out of these, period is the most important parameter since the wrong periods can lead to sparse light curves and misleading information. Time series analysis is a method of applying mathematical and statistical tests to data, to quantify the variation, understand the nature of time-varying phenomena, to gain physical understanding of the system and to predict future behavior of the system. Astronomical time series usually suffer from unevenly spaced time instants, varying error conditions and possibility of big gaps. This is due to daily varying daylight and the weather conditions for ground based observations and observations from space may suffer from the impact of cosmic ray particles. Many large scale astronomical surveys such as MACHO, OGLE, EROS, xv ROTSE, PLANET, Hipparcos, MISAO, NSVS, ASAS, Pan-STARRS, Ke- pler,ESA, Gaia, LSST, CRTS provide variable star’s time series data, even though their primary intention is not variable star observation. Center for Astrostatistics, Pennsylvania State University is established to help the astro- nomical community with the aid of statistical tools for harvesting and analysing archival data. Most of these surveys releases the data to the public for further analysis. There exist many period search algorithms through astronomical time se- ries analysis, which can be classified into parametric (assume some underlying distribution for data) and non-parametric (do not assume any statistical model like Gaussian etc.,) methods. Many of the parametric methods are based on variations of discrete Fourier transforms like Generalised Lomb-Scargle peri- odogram (GLSP) by Zechmeister(2009), Significant Spectrum (SigSpec) by Reegen(2007) etc. Non-parametric methods include Phase Dispersion Minimi- sation (PDM) by Stellingwerf(1978) and Cubic spline method by Akerlof(1994) etc. Even though most of the methods can be brought under automation, any of the method stated above could not fully recover the true periods. The wrong detection of period can be due to several reasons such as power leakage to other frequencies which is due to finite total interval, finite sampling interval and finite amount of data. Another problem is aliasing, which is due to the influence of regular sampling. Also spurious periods appear due to long gaps and power flow to harmonic frequencies is an inherent problem of Fourier methods. Hence obtaining the exact period of variable star from it’s time series data is still a difficult problem, in case of huge databases, when subjected to automation. As Matthew Templeton, AAVSO, states “Variable star data analysis is not always straightforward; large-scale, automated analysis design is non-trivial”. Derekas et al. 2007, Deb et.al. 2010 states “The processing of xvi huge amount of data in these databases is quite challenging, even when looking at seemingly small issues such as period determination and classification”. It will be beneficial for the variable star astronomical community, if basic parameters, such as period, amplitude and phase are obtained more accurately, when huge time series databases are subjected to automation. In the present thesis work, the theories of four popular period search methods are studied, the strength and weakness of these methods are evaluated by applying it on two survey databases and finally a modified form of cubic spline method is intro- duced to confirm the exact period of variable star. For the classification of new variable stars discovered and entering them in the “General Catalogue of Vari- able Stars” or other databases like “Variable Star Index“, the characteristics of the variability has to be quantified in term of variable star parameters.

Impact of sward type, cutting date and conditioning temperature on mass and energy flows in the integrated generation of solid fuel and biogas from semi-natural grassland

Energy production from biomass and the conservation of ecologically valuable grassland habitats are two important issues of agriculture today. The combination of a bioenergy production, which minimises environmental impacts and competition with food production for land with a conversion of semi-natural grasslands through new utilization alternatives for the biomass, led to the development of the IFBB process. Its basic principle is the separation of biomass into a liquid fraction (press fluid, PF) for the production of electric and thermal energy after anaerobic digestion to biogas and a solid fraction (press cake, PC) for the production of thermal energy through combustion. This study was undertaken to explore mass and energy flows as well as quality aspects of energy carriers within the IFBB process and determine their dependency on biomass-related and technical parameters. Two experiments were conducted, in which biomass from semi-natural grassland was conserved as silage and subjected to a hydrothermal conditioning and a subsequent mechanical dehydration with a screw press. Methane yield of the PF and the untreated silage was determined in anaerobic digestion experiments in batch fermenters at 37°C with a fermentation time of 13-15 and 27-35 days for the PF and the silage, respectively. Concentrations of dry matter (DM), ash, crude protein (CP), crude fibre (CF), ether extract (EE), neutral detergent fibre (NDF), acid detergent fibre (ADF), acid detergent ligning (ADL) and elements (K, Mg, Ca, Cl, N, S, P, C, H, N) were determined in the untreated biomass and the PC. Higher heating value (HHV) and ash softening temperature (AST) were calculated based on elemental concentration. Chemical composition of the PF and mass flows of all plant compounds into the PF were calculated. In the first experiment, biomass from five different semi-natural grassland swards (Arrhenaterion I and II, Caricion fuscae, Filipendulion ulmariae, Polygono-Trisetion) was harvested at one late sampling (19 July or 31 August) and ensiled. Each silage was subjected to three different temperature treatments (5°C, 60°C, 80°C) during hydrothermal conditioning. Based on observed methane yields and HHV as energy output parameters as well as literature-based and observed energy input parameters, energy and green house gas (GHG) balances were calculated for IFBB and two reference conversion processes, whole-crop digestion of untreated silage (WCD) and combustion of hay (CH). In the second experiment, biomass from one single semi-natural grassland sward (Arrhenaterion) was harvested at eight consecutive dates (27/04, 02/05, 09/05, 16/05, 24/05, 31/05, 11/06, 21/06) and ensiled. Each silage was subjected to six different treatments (no hydrothermal conditioning and hydrothermal conditioning at 10°C, 30°C, 50°C, 70°C, 90°C). Energy balance was calculated for IFBB and WCD. Multiple regression models were developed to predict mass flows, concentrations of elements in the PC, concentration of organic compounds in the PF and energy conversion efficiency of the IFBB process from temperature of hydrothermal conditioning as well as NDF and DM concentration in the silage. Results showed a relative reduction of ash and all elements detrimental for combustion in the PC compared to the untreated biomass of 20-90%. Reduction was highest for K and Cl and lowest for N. HHV of PC and untreated biomass were in a comparable range (17.8-19.5 MJ kg-1 DM), but AST of PC was higher (1156-1254°C). Methane yields of PF were higher compared to those of WCD when the biomass was harvested late (end of May and later) and in a comparable range when the biomass was harvested early and ranged from 332 to 458 LN kg-1 VS. Regarding energy and GHG balances, IFBB, with a net energy yield of 11.9-14.1 MWh ha-1, a conversion efficiency of 0.43-0.51, and GHG mitigation of 3.6-4.4 t CO2eq ha-1, performed better than WCD, but worse than CH. WCD produces thermal and electric energy with low efficiency, CH produces only thermal energy with a low quality solid fuel with high efficiency, IFBB produces thermal and electric energy with a solid fuel of high quality with medium efficiency. Regression models were able to predict target parameters with high accuracy (R2=0.70-0.99). The influence of increasing temperature of hydrothermal conditioning was an increase of mass flows, a decrease of element concentrations in the PC and a differing effect on energy conversion efficiency. The influence of increasing NDF concentration of the silage was a differing effect on mass flows, a decrease of element concentrations in the PC and an increase of energy conversion efficiency. The influence of increasing DM concentration of the silage was a decrease of mass flows, an increase of element concentrations in the PC and an increase of energy conversion efficiency. Based on the models an optimised IFBB process would be obtained with a medium temperature of hydrothermal conditioning (50°C), high NDF concentrations in the silage and medium DM concentrations of the silage.