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Context: Convection and mass loss by stellar winds are two dynamical processes that shape asymptotic giant branch (AGB) stars and their evolution. Observations and earlier 3D models indicate that giant convection cells cause high-contrast surface intensity patterns, and contribute to the origin of clumpy dust clouds. Aims: We study the formation and resulting properties of dust-driven winds from AGB stars, using new global 3D simulations. Methods: The dynamical stellar interiors, atmospheres, and wind acceleration zones of two M-type AGB stars were modeled with the CO5BOLD code. These first global 3D simulations are based on frequency-dependent gas opacities, and they feature time-dependent condensation and evaporation of silicate grains. Results: Convection and pulsations emerge self-consistently, allowing us to derive wind properties (e.g., mass-loss rates and outflow velocities), without relying on parameterized descriptions of these processes. In contrast to 1D models with purely radial pulsations, the shocks induced by convection and pulsation in the 3D models cover large parts, but not the entirety, of the sphere, leading to a patchy, nonspherical structure of the atmosphere. Since dust condensation critically depends on gas density, new dust clouds form mostly in the dense wakes of atmospheric shocks, where the grains can grow efficiently. The resulting clumpy distribution of newly formed dust leads to a complex 3D morphology of the extended atmosphere and wind-acceleration zone, with simultaneous infall and outflow regions close to the star. Highly nonspherical isotherms and short-lived cool pockets of gas in the stellar vicinity are prominent features. Efficient dust formation sets in closer to the star than spherical averages of the temperature indicate, in dense regions where grain growth rates are higher than average. This can lead to weak outflows in situations where corresponding 1D models do not produce winds. For stars where the overall conditions fo

We used adaptive optics imaging and integral field spectroscopy from the Very Large Telescope, together with images from the Hubble Space Telescope, to study the near-infrared (NIR) evolution of the equatorial ring (ER) of SN 1987A. We studied the NIR flux and morphology over time in order to lay the groundwork for James Webb Space Telescope observations of the system. We also studied the differences in the interacting ring structure and flux between optical, NIR, and other wavelengths, and between line and continuum emission, to constrain the underlying physical processes. For the most part, the evolution is similar in the NIR and optical. The morphology of the ER has been skewed toward the west side (with roughly two-thirds of the NIR emission originating there) since around 2010. A steady decline in the ER flux, broadly similar to the mid-infrared and the optical, has been ongoing since roughly this time as well. The expansion velocity of the ER hotspots in the NIR is fully consistent with the optical. However, continuum emission forms roughly 70% of the NIR luminosity, and has been stronger outside the hotspot-defined extent of the ER (relative to the hotspots themselves) than the optical emission or the NIR line emission since 2012–2013, suggesting a faster-expanding continuum component. We find that this outer NIR emission can have a significant synchrotron contribution. Even if emission from hot dust (~2000 K) is dominant within the ER, the mass of this dust must be vanishingly small (a few times 10−12 M⊙) compared to the total dust mass in the ER (≳10−5 M⊙) to account for the observed HKs flux. The NIR continuum emission, however, expands more slowly than the more diffuse 180-K dust emission that dominates in the MIR, indicating a different source, and the same hot dust component cannot account for the J-band emission.

This paper is the first of a series whose aim is to perform a systematic study of A-type supergiant atmospheres and winds. Here we present a spectral atlas of 41 A-supergiants observed by us in high and medium resolution in the visible asd ultraviolet. The atlas consists of profiles of the H alpha, H beta, H gamma, H delta, H epsilon, Ca II (H and K), Na I (D1 and D2), Mg II4481, Mg II [uv1] and Fe II [uv1, uv2; uv3, uv62, uv63, uv161] lines for 41 stars with spectral types ranging from B9 to A9 and luminosity classes Ia, Iab and Ib, and provides the basic data for a thoughtful study of these stars. The overall characteristics of the sample as well as the data reduction procedures are described. We also present some examples of spectral variability., Unidad Deptal. de Astronomía y Geodesia, Fac. de Ciencias Matemáticas, TRUE, pub

© 2007. The American Astronomical Society. All rights reserved. The authors thank the anonymous referee for his/ her critical comments and valuable suggestions that have significantly improved this paper. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work has been partially performed at the California Institute of Technology and the Department of Molecular and Infrared Astrophysics of the Instituto de Estructura de la Materia, CSIC, and has been partially supported by National Science Foundation grant 9981546 to Owens Valley Radio Observatory and the Spanish MCyT under project DGES/AYA2003- 02785. R. S. is thankful for partial financial support for this work from a NASA/ADP grant. A. G. d. P. is financed by the MAGPOP EU Marie Curie Research Training Network and partially by the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2003-01676. M. M. and R. S. acknowledge financial support for this work from NASA LTSA and ADP awards RTOP 399-20-40-06 and RTOP 399-20-00-08, and HST/GO award GO 09101.01-A. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA Astrophysics Data System., We present high angular resolution images of the post-AGB nebula IRAS 18276-1431 (also known as OH 17.7-2.0) obtained with the Keck II adaptive optics (AO) system in its natural guide star (NGS) mode in the K_P, L_P, and M_S near-infrared bands. We also present supporting optical F606W and F814W HST images as well as interferometric observations of the 12^CO J = 1-0, 13^CO J = 1-0, and 2.6 mm continuum emission with OVRO. The envelope of IRAS 18276-1431 displays a clear bipolar morphology in our optical and NIR images with two lobes separated by a dark waist and surrounded by a faint 4.5'' × 3.4'' halo. Our K_P-band image reveals two pairs of radial "searchlight beams" emerging from the nebula center and several intersecting, arclike features. From our CO data we derive a mass of M > 0.38 (D/3 kpc)^2 M_☉ and an expansion velocity V_exp = 17 km s^-1 for the molecular envelope. The density in the halo follows a radial power law ∝r^-3, which is consistent with a mass-loss rate increasing with time. Analysis of the NIR colors indicates the presence of a compact central source of ~300-500 K dust illuminating the nebula in addition to the central star. Modeling of the thermal IR suggests a two-shell structure in the dust envelope: (1) an outer shell with inner and outer radius R_in ~ 1.6 × 10^16 and R_out ≥1.25 × 10^17 cm, dust temperature T_dust ~ 105-50 K, and a mean mass-loss rate of M ≈ 10^3 M_☉ yr^-1; and (2) an inner shell with R_in ~ 6.3 × 10 cm, T_dust ~ 500-105 K, and M ~ 3 × 10^-5 M_☉ yr^-1. An additional population of big dust grains (radius a ≥0.4 mm) with T_dust = 150-20 K and mass M_dust = (0.16-1.6) × 10^-3 (D/3 kpc)^2 M_☉ can account for the observed submillimeter and millimeter flux excess. The mass of the envelope enclosed within R_out = 1.25 × 10^17 cm derived from SED modeling is ~1 (D/3 kpc)^2 M_☉., W. M. Keck Foundation, National Science Foundation, Owens Valley Radio Observatory, Ministerio de Ciencia y Tecnología, (MCYT), España, Astrophysics Data Analysis program (ADP), NASA, Spanish Programa Nacional de Astronomía y Astrofísica, LTSA (Long Term Space Astrophysics program), NASA, National Aeronautics and Space Administration (NASA), HST/GO award, Unión Europea. FP6, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

An optical study (high resolution images and long-slit spectra in the Her range) of the Serpens reflection nebula (SRN) is presented. The SRN is a bipolar nebula illuminated by the low mass pre-main-sequence (PMS) star Serpens/SVS 2. The Ho profile of Serpens/SVS 2 is shown to be very broad (the width at a 10% of the peak intensity is 13.1 Angstrom (similar to 600 km/s)). The profile has three emission peaks centered at -137, 5 and 100 km/s. The relative strength of the peaks varies with the slit orientation. The blue and redshifted components have similar intensities at low inclinations (PA = -55 degrees and PA = -30 degrees) while at high inclinations the blueshifted component is weaker than the redshifted suggesting a significant contribution of absorption by low latitude outflowing gas. These profiles could be produced in a rotating, latitude dependent wind with the outflow axis parallel to the disk axis. The nebular H alpha profile is double peaked; it has a blue and a redshifted component at the same velocities as the star. The profile shows no significant variations along a given PA; the emission is best explained by single scattering of the stellar radiation. The absence of the 0-velocity emission component is suggestive of the presence of warm absorbing gas within a few stellar radii. There are several knots of gas and dust embedded within the north-western (NW) nebular lobe. These knots are connected by a faint emission, defining a helical path around the major axis of the nebula. This area is also characterized by an unusually large polarization that reaches a 30-40% at 0.95 mu m that is consistent with a concentration of large and reflecting dust grains that are presumably ice coated carbon grains. This region coincides with a ridge of hot (T similar or equal to 35 K) dust detected by IRAS along: the major axis of the SRN., Unidad Deptal. de Astronomía y Geodesia, Fac. de Ciencias Matemáticas, TRUE, pub

We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS captured the prominent early shock-cooling peak of SN 2021zby within the first similar to 10 days after explosion with a 30 minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock-cooling phase. Using a multiband model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of similar to 0.30-0.65 M-circle dot and an envelope radius of similar to 120-300 R-circle dot. These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked feature, such as SNe 1993J, 2011dh, 2016gkg, and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock-cooling light curve, while the multiband observations, particularly UV, are also necessary to fully constrain the progenitor properties.

Climate tipping points occur when change in a part of the climate system becomes self-perpetuating beyond a warming threshold, leading to substantial Earth system impacts. Synthesizing paleoclimate, observational, and model-based studies, we provide a revised shortlist of global ?core? tipping elements and regional ?impact? tipping elements and their temperature thresholds. Current global warming of ~1.1°C above preindustrial temperatures already lies within the lower end of some tipping point uncertainty ranges. Several tipping points may be triggered in the Paris Agreement range of 1.5 to

We present a spectroscopic analysis of the most nearby Type I superluminous supernova (SLSN-I), SN 2018bsz. The photometric evolution of SN 2018bsz has several surprising features, including an unusual pre-peak plateau and evidence for rapid formation of dust greater than or similar to 200 d post-peak. We show here that the spectroscopic and polarimetric properties of SN 2018bsz are also unique. While its spectroscopic evolution closely resembles SLSNe-I, with early O II absorption and C II P Cygni profiles followed by Ca, Mg, Fe, and other O features, a multi-component H alpha profile appearing at similar to 30 d post-maximum is the most atypical. The H alpha is at first characterised by two emission components, one at similar to+3000 km s(-1) and a second at similar to - 7500 km s(-1), with a third, near-zero-velocity component appearing after a delay. The blue and central components can be described by Gaussian profiles of intermediate width (FWHM similar to 2000-6000 km s(-1)), but the red component is significantly broader (FWHM greater than or similar to 10000 km s(-1)) and Lorentzian. The blue H alpha component evolves towards a lower-velocity offset before abruptly fading at similar to + 100 d post-maximum brightness, concurrently with a light curve break. Multi-component profiles are observed in other hydrogen lines, including Pa beta, and in lines of Ca II and He I. Spectropolarimetry obtained before (10.2 d) and after (38.4 d) the appearance of the H lines shows a large shift on the Stokes Q - U plane consistent with SN 2018bsz undergoing radical changes in its projected geometry. Assuming the supernova is almost unpolarised at 10.2 d, the continuum polarisation at 38.4 d reaches P similar to 1.8%, implying an aspherical configuration. We propose that the observed evolution of SN 2018bsz can be explained by highly aspherical, possibly disk-like, circumstellar material (CSM) with several emitting regions. After the supernova explosion, the CSM is quickl

Plant litter is the major source of energy and nutrients in stream ecosystems and its decomposition is vital for ecosystem nutrient cycling and functioning. Invertebrates are key contributors to instream litter decomposition, yet quantification of their effects and drivers at the global scale remains lacking. Here, we systematically synthesized data comprising 2707 observations from 141 studies of stream litter decomposition to assess the contribution and drivers of invertebrates to the decomposition process across the globe. We found that (1) the presence of invertebrates enhanced instream litter decomposition globally by an average of 74%; (2) initial litter quality and stream water physicochemical properties were equal drivers of invertebrate effects on litter decomposition, while invertebrate effects on litter decomposition were not affected by climatic region, mesh size of coarse-mesh bags or mycorrhizal association of plants providing leaf litter; and (3) the contribution of invertebrates to litter decomposition was greatest during the early stages of litter mass loss (0-20%). Our results, besides quantitatively synthesizing the global pattern of invertebrate contribution to instream litter decomposition, highlight the most significant effects of invertebrates on litter decomposition at early rather than middle or late decomposition stages, providing support for the inclusion of invertebrates in global dynamic models of litter decomposition in streams to explore mechanisms and impacts of terrestrial, aquatic, and atmospheric carbon fluxes.

Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of six years, spectra of similar to 10(5) stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra.Aims. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B, and A type, with a formal cutoff of T-eff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra in order to determine the stellar parameters and abundances of these stars.Methods. The procedure used was similar to that of other working groups in GES. A number of groups (called Nodes) each independently analyse the spectra via state-of-the-art techniques and codes. Specific for the analysis in WG13 was the large temperature range covered (T-eff approximate to 7000-50 000 K), requiring the use of different analysis codes. Most Nodes could therefore only handle part of the data. Quality checks were applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them to one another. For each star the Node values were then homogenised into a single result: the recommended parameters and abundances.Results. Eight Nodes each analysed part of the data. In total 17 693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. The elements studied are He, C, N, O, Ne, Mg, Al, Si, and Sc. Abundances for at least one of these elements were determined for 292 stars.Conclusions. The hot-star data analysed here, as well as the GES data in general, will be of considerable use in future studies of stellar evolution and open clusters.

A significant fraction of new metals produced in stars enter the interstellar medium in the form of dust grains. Including dust and wind formation in stellar evolution models of late-stage low- and intermediate-mass stars provides a way to quantify their contribution to the cosmic dust component. In doing so, a correct physical description of dust formation is of course required, but also a reliable prescription for the mass-loss rate. Here, we present an improved model of dust-driven winds to be used in stellar evolution codes and insights from recent detailed numerical simulations of carbon-star winds including drift (decoupling of dust and gas). We also discuss future directions for further improvement., QC 20210629

Asymptotic giant branch stars (AGB) are cool, luminous stars withan initial mass of approximately 0.8 to 8 solar masses. Towards theend of their lives they undergo heavy mass loss, a process thoughtto be caused by dust-driven winds. When it comes to carbon-richAGB stars, i.e. stars with an atmosphere dominated by carbonaceousmolecules and dust, it is believed that the wind is mainly driven byphoton absorption on amorphous carbon grains.This project will focus on how mass loss in carbon-rich AGB stars(C-type) is inuenced by their metallicity. In order to investigate themetallicity-dependence of mass loss I will use state-of-the-art radiationhydrodynamicalwind models that cover a range of typical parametersand metallicities. Since winds of AGB stars are driven by radiationpressure on dust, such wind models can also be used to investigatehow much AGB stars contribute to the dust production in the ISM asa function of metallicity.The aim of this study is to compare theoretical photometric predictionsfrom wind models for C-type AGB stars, at solar and sub-solarmetallicities, to observed photometry. In order to do this the absolutemagnitudes for various lters (GAIA, HST, Vista, WISE, Spitzer andJWST) need to be computed based on synthetic spectra from thesewind models.Once all the theoretical results are obtained these will be comparedto observational data from various surveys of AGB stars in the Largeand Small Magellanic Clouds, covering visual, near-infrared and midinfraredwavelength regions., Asymptotiska jättegrenstjärnor är svala, luminösa stjärnor medstartmassor av ungefär 0.8 till 8 solmassor. De genomgår stora massförluster mot slutet av deras liv, en process som tros orsakas av stoftdrivnavindar. När det gäller kolrika AGB-stjärnor, dvs. stjärnor meden atmosfär som domineras av kolhaltiga molekyler och stoft, tros detatt vinden huvudsakligen drivs av fotonabsorption på amorfa kolkorn.Detta projekt kommer att fokusera på hur massförlust i kolrikaAGB-stjärnor (C-typ) påverkas av deras metallicitet. För att undersöka metallicitet beroendet av massförlust använder jag strålningshydrodynamiskavindmodeller som täcker typiska parametrar och metalliciteter.Eftersom vindar av AGB-stjärnor drivs av strålningstryckpå stoftkorn, kan sådana vindmodeller också användas för att undersöka hur mycket AGB-stjärnor som bidrar till stoftproduktionen i ISMsom en funktion av metallicitet.Syftet med denna studie är att jämföra teoretiska fotometriska förutsägelser från vindmodeller för C-typ AGB-stjärnor, vid sol- och lägremetalliciteter, med observerade fotometriska värden. För att göra dettamåste de absolut magnituderna för olika lter (Gaia, HST, Vista,WISE, Spitzer och JWST) beräknas baserat på syntetiska spektra fråndessa vindmodeller.När alla teoretiska resultat har fåtts fram kommer de att jämförasmed observationell data från olika studier av AGB-stjärnor i den Storaoch Lilla Magellanska Molnet, som täcker våglängder från visuellt tillmid-infrarött.

© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 155 autores. We would like to thank the Referee for useful comments and the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish Ministry of Economy and Competitiveness (MINECO) (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy and the Japanese Japan Society of for the Promotion of Science (JSPS) and Ministry of Education, Culture, Sports, Science and Technology (MEXT) is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia 'Severo Ochoa' SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia 'María de Maeztu' MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the German Research Fundation (DFG) Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. This work is also supported by the grant through the Polish National Research Centre No. 2014/15/B/ST9/04043., A population of globular clusters (GCs) has been recently established by the Fermi-LAT telescope as a new class of GeV gamma-ray sources. Leptons accelerated to TeV energies, in the inner magnetospheres of MSPs or in their wind regions, should produce gamma-rays through the inverse Compton scattering in the dense radiation field from the huge population of stars. We have conducted deep observations of the GC M15 with the MAGIC telescopes and used 165 h in order to search for gamma-ray emission. A strong upper limit on the TeV gamma-ray flux < 3.2 x 10(-13) cm(-2) s(-1) above 300 GeV ( < 0.26 per cent of the Crab nebula flux) has been obtained. We interpret this limit as a constraint on the efficiency of the acceleration of leptons in the magnetospheres of the MSPs. We constrain the injection rate of relativistic leptons, eta(e), from the MSPs magnetospheres and their surrounding. We conclude that eta(e) must be lower than expected from the modelling of high-energy processes in MSP inner magnetospheres. For leptons accelerated with the power-law spectrum in the MSP wind regions, eta(e) is constrained to be much lower than derived for the wind regions around classical pulsars. These constraints are valid for the expected range of magnetic field strengths within the GC and for the range of likely energies of leptons injected from the inner magnetospheres, provided that the leptons are not removed from the GC very efficiently due to advection process. We discuss consequences of these constraints for the models of radiation processes around millisecond pulsars., Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia Severo Ochoa, Unidad de Excelencia María de Maeztu, German BMBF, German MPG, Italian INFN, Italian INAF, Swiss National Fund SNF, Indian Department of Atomic Energy, Japanese Japan Society of for the Promotion of Science (JSPS), Ministry of Education, Culture, Sports, Science and Technology (MEXT), Croatian Science Foundation (HrZZ), University of Rijeka, German Research Fundation (DFG) Collaborative Research Centers, Polish National Research Centre, Brazilian MCTIC, Brazilian CNPq, Brazilian FAPERJ, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Stars of initial masses between 0.8-8 M☉ will become "asymptotic giant branch" (AGB) stars during the final stages of their evolution. During this phase, the stars are characterized by low velocity and high-density winds. An AGB star can lose a substantial fraction of its mass through the stellar wind and thereby avoid ending up as a supernova explosion. The AGB stars, therefore, play an important role in enriching the interstellar medium (ISM) with chemical elements and in contributing dust and gas to the ISM. The mass-loss rate on the AGB is a decisive parameter for the lifetime of this evolutionary phase and the fate of low- and intermediate-mass stars. An accurate mass-loss-rate estimation provides an important constraint for wind models aimed to better understand the wind-driving mechanism, as well as for stellar evolution. The stellar wind is driven by radiation pressure on dust grains and blows away dust and gas from the central star. This creates an extended envelope which is expected to be spherical because of the isotropic radiation field of the central star, and the connection between the radiation field and the wind. However, there is growing observational evidence of asymmetrical morphology, e.g., torii, jets, bipolar outflows, in AGB circumstellar envelopes (CSEs). Moreover, proto-planetary nebulae (proto-PNe) and PNe, the next evolutionary phase after the AGB phase, show a wide range of asymmetrical morphologies. In many cases, an embedded binary system has been detected in the gas envelopes. This is pointing to the gravitational effect of the companion as important for the envelope shaping mechanism. The work that this thesis is based on, studies two interesting examples of (post) AGB stars which show complex morphologies of their CSEs. The S-star π1 Gruis shows a CSE structure consisting of an equatorial low-velocity expanding spiral and a fast bipolar outflow. The circumstellar environment of the post-AGB (or post red giant branch, post-RGB) star H

Background: A detrimental consequence of diet-induced weight loss, common in athletes who participate in weight cutting sports, is muscle loss. Dietary omega-3 polyunsaturated fatty acids (n-3PUFA) exhibit a protective effect on the loss of muscle tissue during catabolic situations such as injury-simulated leg immobilization. This study aimed to investigate the influence of dietary n-3PUFA supplementation on changes in body composition and muscle strength following short-term diet-induced weight loss in resistance-trained men. Methods: Twenty resistance-trained young (23 ± 1 years) men were randomly assigned to a fish oil group that supplemented their diet with 4 g n-3PUFA, 18 g carbohydrate, and 5 g protein (FO) or placebo group containing an equivalent carbohydrate and protein content (CON) over a 6 week period. During weeks 1–3, participants continued their habitual diet. During week 4, participants received all food items to control energy balance and a macronutrient composition of 50% carbohydrate, 35% fat, and 15% protein. During weeks 5 and 6, participants were fed an energy-restricted diet equivalent to 60% habitual energy intake. Body composition and strength were measured during weeks 1, 4, and 6. Results: The decline in total body mass (FO = −3.0 ± 0.3 kg, CON = −2.6 ± 0.3 kg), fat free mass (FO = −1.4 ± 0.3 kg, CON = −1.2 ± 0.3 kg) and fat mass (FO = −1.4 ± 0.2 kg, CON = −1.3 ± 0.3 kg) following energy restriction was similar between groups (all p > 0.05; d: 0.16–0.39). Non-dominant leg extension 1 RM increased (6.1 ± 3.4%) following energy restriction in FO (p < 0.05, d = 0.29), with no changes observed in CON (p > 0.05, d = 0.05). Dominant leg extension 1 RM tended to increase following energy restriction in FO (p = 0.09, d = 0.29), with no changes in CON (p > 0.05, d = 0.06). Changes in leg press 1 RM, maximum voluntary contraction and m

We present recent Atacama Large Millimeter/submillimeter Array (ALMA)-based studies of circumstellar envelopes (CSEs) around Asymptotic Giant Branch (AGB) stars and pre-Planetary Nebulae (pPNe). In only a few years of operation, ALMA is revolutionising the field of AGB-to-PN research by providing unprecedentedly detailed information on the complex nebular architecture (at large but also on small scales down to a few ∼10 AU from the centre), dynamics and chemistry of the outflows/envelopes of low-to-intermediate mass stars in their late stages of the evolution. Here, we focus on continuum and molecular line mapping studies with high angular resolution and sensitivity of some objects that are key to understanding the complex PN-shaping process. In particular, we offer (i) a brief summary of ALMA observations of rotating disks in post-AGB objects and (ii) report on ALMA observations of OH 231.8+4.2 providing the most detailed and accurate description of the global nebular structure and kinematics of this iconic object to date.

Physique competitions are events in which competitors are judged on muscular appearance and symmetry. The purpose of this retrospective case study was to describe changes in dietary intake, body mass/composition, and the menstrual cycle during the 20-week competition preparation (PREP) and 20-week post competition recovery (REC) periods of a drug-free amateur female figure competitor (age = 26–27, BMI = 19.5 kg/m2). Dietary intake (via weighed food records) and body mass were assessed daily and averaged weekly. Body composition was estimated via Dual-energy X-ray absorptiometry (DXA) and 7-site skinfold measurements. Energy intake, body mass and composition, and energy availability decreased during the 20-week PREP period (changes of ~298 kcals, 5.1 kg, 6.5% body fat, and 5.4 kcal/kg fat free mass, respectively) and returned to baseline values by end of the 20-week REC period. Menstrual cycle irregularity was reported within the first month of PREP and the last menstruation was reported at week 11 of PREP. Given the potentially adverse health outcomes associated with caloric restriction, future, prospective cohort studies on the physiological response to PREP and REC are warranted in drug-free, female physique competitors.

Physique competitions are events in which competitors are judged on muscular appearance and symmetry. The purpose of this retrospective case study was to describe changes in dietary intake, body mass/composition, and the menstrual cycle during the 20-week competition preparation (PREP) and 20-week post competition recovery (REC) periods of a drug-free amateur female figure competitor (age = 26–27, BMI = 19.5 kg/m2). Dietary intake (via weighed food records) and body mass were assessed daily and averaged weekly. Body composition was estimated via Dual-energy X-ray absorptiometry (DXA) and 7-site skinfold measurements. Energy intake, body mass and composition, and energy availability decreased during the 20-week PREP period (changes of ~298 kcals, 5.1 kg, 6.5% body fat, and 5.4 kcal/kg fat free mass, respectively) and returned to baseline values by end of the 20-week REC period. Menstrual cycle irregularity was reported within the first month of PREP and the last menstruation was reported at week 11 of PREP. Given the potentially adverse health outcomes associated with caloric restriction, future, prospective cohort studies on the physiological response to PREP and REC are warranted in drug-free, female physique competitors.

Atmospheric warming over the Greenland Ice Sheet during the last 2 decades has increased the amount of surface meltwater production, resulting in the migration of melt and percolation regimes to higher altitudes and an increase in the amount of ice content from refrozen meltwater found in the firn above the superimposed ice zone. Here we present field and airborne radar observations of buried ice layers within the near-surface (0-20 m) firn in western Greenland, obtained from campaigns between 1998 and 2014. We find a sharp increase in firn-ice content in the form of thick widespread layers in the percolation zone, which decreases the capacity of the firn to store meltwater. The estimated total annual ice content retained in the near-surface firn in areas with positive surface mass balance west of the ice divide in Greenland reached a maximum of 74 +/- 25 Gt in 2012, compared to the 1958-1999 average of 13 +/- 2 Gt, while the percolation zone area more than doubled between 2003 and 2012. Increased melt and column densification resulted in surface lowering averaging 0.80 +/- 0.39 myr(-1) between 1800 and 2800 m in the accumulation zone of western Greenland. Since 2007, modeled annual melt and refreezing rates in the percolation zone at elevations below 2100 m surpass the annual snowfall from the previous year, implying that mass gain in the region is retained after melt in the form of refrozen meltwater. If current melt trends over high elevation regions continue, subsequent changes in firn structure will have implications for the hydrology of the ice sheet and related abrupt seasonal densification could become increasingly significant for altimetry-derived ice sheet mass balance estimates.

We present a new record of ice thickness change, reconstructed at nearly 100,000 sites on the Greenland Ice Sheet (GrIS) from laser altimetry measurements spanning the period 1993-2012, partitioned into changes due to surface mass balance (SMB) and ice dynamics. We estimate a mean annual GrIS mass loss of 243 +/- 18 Gt.y(-1), equivalent to 0.68 mm.y(-1) sea level rise (SLR) for 2003-2009. Dynamic thinning contributed 48%, with the largest rates occurring in 2004-2006, followed by a gradual decrease balanced by accelerating SMB loss. The spatial pattern of dynamic mass loss changed over this time as dynamic thinning rapidly decreased in southeast Greenland but slowly increased in the southwest, north, and northeast regions. Most outlet glaciers have been thinning during the last two decades, interrupted by episodes of decreasing thinning or even thickening. Dynamics of the major outlet glaciers dominated the mass loss from larger drainage basins, and simultaneous changes over distances up to 500 km are detected, indicating climate control. However, the intricate spatiotemporal pattern of dynamic thickness change suggests that, regardless of the forcing responsible for initial glacier acceleration and thinning, the response of individual glaciers is modulated by local conditions. Recent projections of dynamic contributions from the entire GrIS to SLR have been based on the extrapolation of four major outlet glaciers. Considering the observed complexity, we question how well these four glaciers represent all of Greenland's outlet glaciers.

Observations over the past decade show significant ice loss associated with the speed-up of glaciers in southeast Greenland from 2003, followed by a deceleration from 2006. These short-term, episodic, dynamic perturbations have a major impact on the mass balance on the decadal scale. To improve the projection of future sea level rise, a long-term data record that reveals the mass balance beyond such episodic events is required. Here, we extend the observational record of marginal thinning of Helheim and Kangerdlugssuaq glaciers from 10 to more than 80 years. We show that, although the frontal portion of Helheim Glacier thinned by more than 100m between 2003 and 2006, it thickened by more than 50m during the previous two decades. In contrast, Kangerdlugssuaq Glacier underwent minor thinning of 40-50m from 1981 to 1998 and major thinning of more than 100m after 2003. Extending the record back to the end of the Little Ice Age (prior to 1930) shows no thinning of Helheim Glacier from its maximum extent during the Little Ice Age to 1981, while Kangerdlugssuaq Glacier underwent substantial thinning of 230 to 265 m. Comparison of sub-surface water temperature anomalies and variations in air temperature to records of thickness and velocity change suggest that both glaciers are highly sensitive to short-term atmospheric and ocean forcing, and respond very quickly to small fluctuations. On century timescales, however, multiple external parameters (e. g. outlet glacier shape) may dominate the mass change. These findings suggest that special care must be taken in the projection of future dynamic ice loss.

Mass loss, in the form of slow stellar winds, is a decisive factor for the evolution of cool luminous giants, eventually turning them into white dwarfs. These dense outflows are also a key factor in the enrichment of the interstellar medium with newly produced elements from the interior of these stars. There are strong indications that these winds are accelerated by radiation pressure on dust grains, but the actual grain species responsible for driving the outflows in M-type Asymptotic Giant Branch stars are still a matter of debate. Observations of dust features in the circumstellar environment of these stars suggest that magnesium-iron silicates are possible wind-drivers. However, the optical properties of these silicate grains are strongly influenced by the Fe-content. Fe-bearing condensates heat up strongly when interacting with the radiation field and therefore cannot form close enough to the star to trigger outflows. Fe-free condensates, on the other hand, have a low absorption cross-section at near-IR wavelengths where AGB stars emit most of their flux. To solve this conundrum, it has been suggested that winds of M-type AGB stars may be driven by photon scattering on Fe-free silicate grains with sizes comparable to the wavelength of the flux maximum, rather than by true absorption. In this thesis we investigate dynamical models of M-type AGB stars, using Fe-free silicates as the wind-driving dust species. According to our findings these models produce both dynamic and photometric properties consistent with observations. Especially noteworthy are the large photometric variations in the visual band during a pulsation cycle, seen both in the observed and synthetic fluxes. A closer examination of the models reveals that these variations are caused by changes in the molecular layers, and not by changes in the dust. This is a strong indication that stellar winds of M-type AGB stars are driven by dust materials that are very transparent in the visual and near-infra

We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (600 days) that cannot be powered by 56Ni/56Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (109 cm-3). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was 3 M . Our observations are in agreement with models of pulsational pair-instability SNe described in the literature. © 2014. The American Astronomical Society. All rights reserved..

Many glaciers along the southeast and northwest coasts of Greenland have accelerated, increasing the ice sheet's contribution to global sea-level rise. In this article, we map elevation changes on Upernavik Isstrom (UI), West Greenland, during 2003 to 2009 using high-resolution ice, cloud and land elevation satellite laser altimeter data supplemented with altimeter surveys from NASA's Airborne Topographic Mapper during 2002 to 2010. To assess thinning prior to 2002, we analyze aerial photographs from 1985. We document at least two distinct periods of dynamically induced ice loss during 1985 to 2010 characterized by a rapid retreat of the calving front, increased ice speed, and lowering of the ice surface. The first period occurred before 1991, whereas the latter occurred during 2005 to 2009. Analyses of air and sea-surface temperature suggest a combination of relatively warm air and ocean water as a potential trigger for the dynamically induced ice loss. We estimate a total catchment-wide ice-mass loss of UI caused by the two events of 72.3 +/- 15.8 Gt during 1985 to 2010, whereas the total melt-induced ice-mass loss during this same period is 19.8 +/- 2.8 Gt. Thus, 79% of the total ice-mass loss of the UI catchment was caused by ice dynamics, indicating the importance of including dynamically induced ice loss in the total mass change budget of the Greenland ice sheet.

The mass-loss process is a key ingredient for our understanding in many fields of astrophysics, including stellar evolution and the enrichment of the interstellar medium (ISM) via stellar yields. We combined the capability of the VLTI/MIDI and VLT/VISIR instruments with very recent Herschel/PACS observations to characterize the geometry of mass loss from evolved red giants on the Asymptotic Giant Branch (AGB) at various scales. This paper describes the sample of objects, the observing strategy, the tool for the interpretation, and preliminary MIDI results for two targets: U Ant and θ Aps. © 2012 SPIE., SCOPUS: cp.p, info:eu-repo/semantics/published

Herschel’s PACS instrument observed the environment of the binary system Mira Ceti in the 70 and 160 μm bands. These images reveal bright structures shaped as five broken arcs and fainter filaments in the ejected material of Mira’s primary star, the famous AGB star o Ceti. The overall shape of the IR emission around Mira deviates significantly from the expected alignment with Mira’s exceptionally high space velocity. The observed broken arcs are neither connected to each other nor are they of a circular shape; they stretch over angular ranges of 80 to 100 degrees. By comparing Herschel and GALEX data, we found evidence for the disruption of the IR arcs by the fast outflow visible in both Hα and the far UV. Radial intensity profiles are derived, which place the arcs at distances of 6–85″ (550−8000 AU) from the binary. Mira’s IR environment appears to be shaped by the complex interaction of Mira’s wind with its companion, the bipolar jet, and the ISM., N° article :L4, SCOPUS: ar.j, info:eu-repo/semantics/published

Context. Overall spherically symmetric, geometrically thin gas and dust shells have been found around a handful of asymptotic giant branch (AGB) carbon stars. Their dynamical ages lie in the range of 103 to 104 years. A tentative explanation for their existence is that they have formed as a consequence of mass-loss-rate modulations during a He-shell flash. Aims. The detached shells carry information on their formation process, as well as on the small-scale structure of the circumstellar medium around AGB stars due to the absence of significant line-of-sight confusion. Methods. The youngest detached shells, those around the carbon stars R Scl and U Cam, are studied here in great detail in scattered stellar light with the Advanced Survey Camera on the Hubble Space Telescope. Quantitative results are derived assuming optically thin dust scattering. Results. The detached dust shells around R Scl and U Cam are found to be consistent with an overall spherical symmetry. They have radii of 192 (corresponding to a linear size of 8 × 1016 cm) and 77 (5 × 1016 cm), widths of 12 (5 × 1015 cm) and 06 (4 × 1015 cm), and dust masses of 3 × 10-6 and 3 × 10-7 , respectively. The dynamical ages of the R Scl and U Cam shells are estimated to be 1700 and 700 yr, respectively, and the shell widths correspond to time scales of 100 and 50 yr, respectively. Small-scale structure in the form of less than arcsec-sized clumps is clearly seen in the images of the R Scl shell. Average clump dust masses are estimated to be about 2 × 10-9

A large proportion of northern peatlands consists of Sphagnum-dominated ombrotrophic bogs. In these bogs, peat mosses (Sphagnum) and vascular plants occur in an apparent stable equilibrium, thereby sustaining the carbon sink function of the bog ecosystem. How global warming and increased nitrogen (N) deposition will affect the species composition in bog vegetation is still unclear. We performed a transplantation experiment in which mesocosms with intact vegetation were transplanted southward from north Sweden to north-east Germany along a transect of four bog sites, in which both temperature and N deposition increased. In addition, we monitored undisturbed vegetation in control plots at the four sites of the latitudinal gradient. Four growing seasons after transplantation, ericaceous dwarf shrubs had become much more abundant when transplanted to the warmest site which also had highest N deposition. As a result ericoid aboveground biomass in the transplanted mesocosms increased most at the southernmost site, this site also had highest ericoid biomass in the undisturbed vegetation. The two dominant Sphagnum species showed opposing responses when transplanted southward; Sphagnum balticum height increment decreased, whereas S. fuscum height increment increased when transplanted southward. Sphagnum production did not differ significantly among the transplanted mesocosms, but was lowest in the southernmost control plots. The dwarf shrub expansion and increased N concentrations in plant tissues we observed, point in the direction of a positive feedback toward vascular plant-dominance suppressing peat-forming Sphagnum in the long term. However, our data also indicate that precipitation and phosphorus availability influence the competitive balance between Sphagnum, dwarf shrubs and graminoids.

The asymptotic giant branch (AGB) is the last stage of stellar evolution for stars with masses between 0.8-8 M(sun). This phase is characterised by an intense mass loss, which builds up a circumstellar envelope of dust and gas(CSE). It is through this process that the AGB stars contribute to the chemical evolution of galaxies. In addition, a rich and varied chemistry is active within the CSEs.Observations of circumstellar H2O are of particular interest, as it is expected to be one of the most abundant molecules in the inner envelopes of M-type AGB stars (with C/O<1). The first part of this thesis concerns the modelling of water vapour emission lines from CSEs around M-type AGB stars. Using satellite observations and detailed radiative transfer models, H2O abundances in these stars are determined and compared with theoretical chemical models. The importance of resolved H2O line profiles and excitation through different vibrationally excited states are also demonstrated.The second part of the thesis has its focus on the detached shells of dust and gas observed around a handful of carbon AGB stars (with C/O>1), believed to be an effect of highly time-variable mass loss during a thermal pulse. The detached shells around three sources were observed in stellar light scattered by dust and gas in the shells using ground-based and space telescopes. The observations allow a separation of the scattering agents, and reveal information on the detached shells in unprecedented detail., At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 2: Submitted. Paper 4: In progress.

All stars with a stellar mass of about 0.8–8 MSun will end their lives as asymptotic giant branch (AGB) stars. Through their extensive mass loss the AGB stars constitutes an important source of nuclear processed material. They also provide us with fascinating systems where an interchange of different physical and chemical processes occur, making them excellent astrophysical laboratories. Being the most important process for the evolution of an AGB star, the mass loss is well established, but its details are less well known. On the AGB, the mass-loss rate can span several orders of magnitude, reaching 10−4 MSun yr−1 toward the end of the AGB. It is challenging to find reliable methods to estimate the mass-loss rates of individual objects. Nevertheless, it is important, since the mass-loss rate affects the derived abundances of other molecules in the circumstellar envelope, and therefore the estimates of the amount and composition of the recycled material. In the first part of the thesis the reliability of mass-loss rate estimates is evaluated using two main methods; the observations and radiative transfer analysis of CO radio line emission, and dust radiative transfer combined with a dynamical model. The second part of the thesis focuses on a particular chemical type of AGB stars; the S-type. The S-stars are believed to have approximately the same amount of carbon as oxygen in the photosphere, and to be an intermediate evolutionary stage as the star evolves from an oxygen-rich M-star into a carbon star. As possible transition objects the S-stars might give important clues to the mass-loss mechanisms and to the chemical evolution along the AGB. Using observations of circumstellar radio line emission in combination with detailed radiative transfer analysis, we have estimated mass-loss rates and abundances of chemically important molecules for a sample of 40 S-stars. The results are compared to previous results for M- and carbon stars.

Several observational pieces of evidence indicate that specific evolutionary channels that involve Roche lobe overflow are not correctly accounted for by the classical Roche model. We generalise the concept of the Roche lobe in the presence of extra forces (caused by radiation pressure or pulsations). By computing the distortion of the equipotential surfaces, we are able to evaluate the impact of these perturbing forces on the stability of Roche lobe overflow (RLOF). Radiative forces are parametrised through the constant reduction factor that they impose on the gravitational force from the radiating star (neglecting any shielding in the case of high optical thickness). Forces imparted by pulsation are derived from the velocity profile of the wind that they trigger. We provide analytical expressions to compute the generalised Roche radius. Depending on the extra force, the Roche lobe radius may either stay unchanged, become smaller, or even become meaningless (in the presence of a radiatively- or pulsation-driven wind). There is little impact on the RLOF stability., info:eu-repo/semantics/published

Cosmic dust particles play an important role for the thermal, dynamical and chemical conditions in many astrophysical environments, especially for the star and planet formation process and the late stages of stellar evolution. Dust particles determine the spectral appearance of protostars as well as evolved stars with circumstellar envelopes, and they also dominate the extinction curves of galaxies. The most efficient site of dust formation in the present universe is the cool extended atmospheres of carbon-rich and oxygen-rich AGB stars. Dust production also seems likely to occur in supernova remnants, especially in the early universe, however, the true nature of such supernova dust is not as well described as for AGB stars either observationally or theoretically. Once the dust is formed it will enter the interstellar medium and be an important ingredient for further star- and planet-formation. During star-formation, dust seems to be an important coolant which can lower the temperature in the centre of the molecular clouds and thereby lead to the formation of smaller stars than in a non-dusty cloud. If the star is formed with an accretion disk containing dust grains, the subsequent planet-formation will occur more effectively than in a dustless disk.

We argue that the energy injection of pulsations may be of greater importance to the mass-loss rate of AGB stars than metallicity, and that the mass-loss trend with metallicity is not as simple as sometimes assumed. Using our detailed radiation hydrodynamical models that include dust formation, we illustrate the effects of pulsation energy on wind properties. We find that the mass-loss rate scales with the kinetic energy input by pulsations as long as a dust-saturated wind does not occur, and all other stellar parameters are kept constant. This includes the absolute abundance of condensible carbon (not bound in CO), which is more relevant than keeping the C/O-ratio constant when comparing stars of different metallicity. The pressure and temperature gradients in the atmospheres of stars, become steeper and flatter, respectively, when the metallicity is reduced, while the radius where the atmosphere becomes opaque is typically associated with a higher gas pressure. This effect can be compensated for by adjusting the velocity amplitude of the variable inner boundary (piston), which is used to simulate the effects of pulsation, to obtain models with comparable kinetic-energy input. Hence, it is more relevant to compare models with similar energy-injections than of similar velocity amplitude. Since there is no evidence for weaker pulsations in low-metallicity AGB stars, we conclude that it is unlikely that low-metallicity C-stars have lower mass-loss rates, than their more metal-rich counterparts with similar stellar parameters, as long as they have a comparable amount of condensible carbon.

We present an analysis of archival RXTE data of the X- ray binary source 4U 1538−52/QV Nor. The RXTE ob- servatory made one complete binary cycle observation on January 1997 and 2001, respectively. The X-ray con- tinuum data are well described by an absorbed Nega- tive Positive power laws Exponentials (NPEX) compo- nent modified by an iron emission line at 6.4 keV and a cyclotron absorption line at 20 keV. Using a simple spher- ically symmetric wind model to describe the X-ray ab- sorption variations as a function of orbital phase, we in- ferred a wind mass-loss rate from the companion star of (1.3 − 2.5) × 10−6 M⊙/yr. Our results are consistent with those obtained by the Ginga X-ray observatory. We have also analyzed X-ray flux variations over the binary orbit and we have found a sharp increase at orbital phase 0.34 in both set of data. However, the increase at orbital phase 0.66 is significantly different in the two observa- tions.

Las supergigantes de tipo-A son las estrellas intrínsecamente más brillantes en el visible y, por lo tanto, uno de los mejores indicadores de distancias extragalácticas en potencia. Estas estrellas presentan procesos físicos muy complejos en sus atmósferas con un campo de radiación muy energético y de alta densidad de momento, en combinación con una atmósfera extendida y tenue y un viento estelar. Uno de los mejores trazadores de estas envolturas extensas son las l ' ineas UV de diferentes iones (principalmente Mg I1, Al I1, Si II, e II and Fe II). Los pocos trabajos sobre el espectro UV de estas estrellas muestran que la espectroscopía UV de alta resolución y un análisis de variabilidad son cruciales para progresar en el conocimiento de las atmósferas de las supergigantes de tipo-A. Una cantidad importante de cuestiones permanecen abiertas. Aquí resumimos los resultados más relevantes encontrados en el rango UV y las cuestiones que se derivan para el viento de las supergigantes-A. Simultáneamente se argumenta lo esencial de una misión UV., A-type supergiants are intrinsically the brightest stars at visual wavelengths, and therefore one of the best potential extragalactic distance indicators. These stars present a complex atmospheric physics with a large energy and momentum density of the radiation field, in combination with an extended and tenous atmosphere and a stellar wind. One of the best tracers of these expanding envelopes are the UV lines of different ions (mainly Mg I1, Al I1, Si I1, e II and Fe n). The scarce works on the UV spectrum of these stars show that high resolution UV spectroscopy and variability analysis are crucial to make progress in the understanding of A-type supergiants atmospheres. A number of important issues remain open. We summarize here the major findings on the winds of A-supergiants in the UV range and the derived open questions. Simultaneously, we address the critical importance of a UV mission to solve them.

Peat bogs have historically represented exceptional carbon (C) sinks because of their extremely low decomposition rates and consequent accumulation of plant remnants as peat. Among the factors favoring that peat accumulation, a major role is played by the chemical quality of plant litter itself, which is poor in nutrients and characterized by polyphenols with a strong inhibitory effect on microbial breakdown. Because bogs receive their nutrient supply solely from atmospheric deposition, the global increase of atmospheric nitrogen (N) inputs as a consequence of human activities could potentially alter the litter chemistry with important, but still unknown, effects on their C balance. Here we present data showing the decomposition rates of recently formed litter peat samples collected in nine European countries under a natural gradient of atmospheric N deposition from ¿0.2 to 2 g·m-2.yr -1. We found that enhanced decomposition rates for material accumulated under higher atmospheric N supplies resulted in higher carbon dioxide (CO2) emissions and dissolved organic carbon release. The increased N availability favored microbial decomposition (i) by removing N constraints on microbial metabolism and (ii) through a chemical amelioration of litter peat quality with a positive feedback on microbial enzymatic activity. Although some uncertainty remains about whether decay-resistant Sphagnum will continue to dominate litter peat, our data indicate that, even without such changes, increased N deposition poses a serious risk to our valuable peatland C sinks

A computational study has been carried out to investigate smoldering ignition and propagation in polyurethane foam. The one-dimensional, transient, governing equations for smoldering combustion in a porous fuel are solved accounting for improved solid-phase chemical kinetics. A systematic methodology for the determination of solid-phase kinetics suitable for numerical models has been developed and applied to the simulation of smoldering combustion. This methodology consists in the correlation of a mathematical representation of a reaction mechanism with data from previous thermogravimetric experiments. Genetic-algorithm and trail-and-error techniques are used as the optimization procedure. The corresponding kinetic parameters for two different mechanisms of polyurethane foam smoldering kinetics are quantified: a previously proposed 3-step mechanism and a new 5-step mechanism. These kinetic mechanisms are used to model one-dimensional smoldering combustion, numerically solving for the solid-phase and gas-phase conservation equations in microgravity with a forced flow of oxidizer gas. The results from previously conducted microgravity experiments with flexible polyurethane foam are used for calibration and testing of the model predictive capabilities. Both forward and opposed smoldering configurations are examined. The model describes well both opposed and forward propagation. Specifically, the model predicts the reaction-front thermal and species structure, the onset of smoldering ignition, and the propagation rate. The model results reproduce the most important features of the smolder process and represent a significant step forward in smoldering combustion modeling.

Tato práce se zabývá možnostmi kvantitativního zobrazování ve skenovacím (transmisním) elektronovém mikroskopu (S|T|EM) společně s jejich korelativní aplikací. Práce začíná popisem metody kvantitativního STEM (qSTEM), kde lze stanovenou lokální tloušťku vzorku dát do spojitosti s ozářenou dávkou, a vytvořit tak studii úbytku hmoty. Tato metoda byla použita při studiu ultratenkých řezů zalévací epoxidové pryskyřice za různých podmínek (stáří, teplota, kontrastování, čištění pomocí plazmy, pokrytí uhlíkem, proud ve svazku). V rámci této části jsou diskutovány a demonstrovány možnosti kalibračního procesu detektoru, nezbytné pozadí Monte Carlo simulací elektronového rozptylu a dosažitelná přesnost metody. Metoda je pak rozšířena pro použití detektoru zpětně odražených elektronů (BSE), kde byla postulována, vyvinuta a testována nová kalibrační technika založená na odrazu primárního svazku na elektronovém zrcadle. Testovací vzorky byly různě tenké vrstvy v tloušťkách mezi 1 až 25 nm. Použití detektoru BSE přináší možnost měřit tloušťku nejen elektronově průhledných vzorků jako v případě qSTEM, ale také tenkých vrstev na substrátech - qBSE. Obě výše uvedené metody (qSTEM a qBSE) jsou založeny na intenzitě zaznamenaného obrazu, a to přináší komplikaci, protože vyžadují správnou kalibraci detektoru, kde jen malý posun úrovně základního signálu způsobí významnou změnu výsledků. Tato nedostatečnost byla překonána v případě qSTEM použitím nejpravděpodobnějšího úhlu rozptylu (zachyceného pixelovaným STEM detektorem), namísto integrální intenzity obrazu zachycené prstencovým segmentem detektoru STEM. Výhodou této metody je její použitelnost i na data, která nebyla předem zamýšlena pro využití qSTEM, protože pro aplikaci metody nejsou potřeba žádné zvláštní předchozí kroky. Nevýhodou je omezený rozsah detekovatelných tlouštěk vzorku způsobený absencí píku v závislosti signálu na úhlu rozptylu. Obecně platí, že oblast s malou tloušťkou je neměřitelná stejně tak jako tloušťka příli, This thesis deals with the possibilities of quantitative imaging in scanning (transmission) electron microscope (S|T|EM) together with its correlative applications. It starts with quantitative STEM (qSTEM) method description, where estimated local sample thickness can be related to irradiated dose and create a mass-loss study, which was applied on samples of ultrathin epoxy resin sections at variate conditions (age, temperature, staining, plasma cleaning, carbon covering, probe current). The possibilities of the detector calibration process, the necessary background of the Monte Carlo simulations of electron scattering and achievable accuracy of the method are discussed and demonstrated. The method is then extrapolated for the use of back-scattered electron (BSE) detector, where new detector calibration technique, based on primary beam deflection on electron mirror, was postulated, developed and tested on various thin coating layers with thicknesses in range from 1 to 25 nm. The use of BSE detector brings the opportunity to measure the thickness of not only the electron transparent samples as in case of qSTEM, but also thin layers on substrates – qBSE. Both above-mentioned methods (qSTEM and qBSE) are intensity-based. This brings complication in the need of proper calibration, where just a slight drift of base-signal level causes a significant change of the results. This insufficiency was overcome in case of qSTEM by using the most probable scattering angle (captured by pixelated STEM detector) instead of an integral image intensity captured by an annular segment of STEM detector. The advantage of this method is its applicability post-acquisition, where no special previous actions are needed before each imaging session. The disadvantage is the limited range of detectable thicknesses given by the peak creation in signal/scattering-angle dependency. In general, low thickness region is immeasurable as well as those too thick (usable thickness range for latex is 185 - 1

Tato práce se zabývá možnostmi kvantitativního zobrazování ve skenovacím (transmisním) elektronovém mikroskopu (S|T|EM) společně s jejich korelativní aplikací. Práce začíná popisem metody kvantitativního STEM (qSTEM), kde lze stanovenou lokální tloušťku vzorku dát do spojitosti s ozářenou dávkou, a vytvořit tak studii úbytku hmoty. Tato metoda byla použita při studiu ultratenkých řezů zalévací epoxidové pryskyřice za různých podmínek (stáří, teplota, kontrastování, čištění pomocí plazmy, pokrytí uhlíkem, proud ve svazku). V rámci této části jsou diskutovány a demonstrovány možnosti kalibračního procesu detektoru, nezbytné pozadí Monte Carlo simulací elektronového rozptylu a dosažitelná přesnost metody. Metoda je pak rozšířena pro použití detektoru zpětně odražených elektronů (BSE), kde byla postulována, vyvinuta a testována nová kalibrační technika založená na odrazu primárního svazku na elektronovém zrcadle. Testovací vzorky byly různě tenké vrstvy v tloušťkách mezi 1 až 25 nm. Použití detektoru BSE přináší možnost měřit tloušťku nejen elektronově průhledných vzorků jako v případě qSTEM, ale také tenkých vrstev na substrátech - qBSE. Obě výše uvedené metody (qSTEM a qBSE) jsou založeny na intenzitě zaznamenaného obrazu, a to přináší komplikaci, protože vyžadují správnou kalibraci detektoru, kde jen malý posun úrovně základního signálu způsobí významnou změnu výsledků. Tato nedostatečnost byla překonána v případě qSTEM použitím nejpravděpodobnějšího úhlu rozptylu (zachyceného pixelovaným STEM detektorem), namísto integrální intenzity obrazu zachycené prstencovým segmentem detektoru STEM. Výhodou této metody je její použitelnost i na data, která nebyla předem zamýšlena pro využití qSTEM, protože pro aplikaci metody nejsou potřeba žádné zvláštní předchozí kroky. Nevýhodou je omezený rozsah detekovatelných tlouštěk vzorku způsobený absencí píku v závislosti signálu na úhlu rozptylu. Obecně platí, že oblast s malou tloušťkou je neměřitelná stejně tak jako tloušťka příli, This thesis deals with the possibilities of quantitative imaging in scanning (transmission) electron microscope (S|T|EM) together with its correlative applications. It starts with quantitative STEM (qSTEM) method description, where estimated local sample thickness can be related to irradiated dose and create a mass-loss study, which was applied on samples of ultrathin epoxy resin sections at variate conditions (age, temperature, staining, plasma cleaning, carbon covering, probe current). The possibilities of the detector calibration process, the necessary background of the Monte Carlo simulations of electron scattering and achievable accuracy of the method are discussed and demonstrated. The method is then extrapolated for the use of back-scattered electron (BSE) detector, where new detector calibration technique, based on primary beam deflection on electron mirror, was postulated, developed and tested on various thin coating layers with thicknesses in range from 1 to 25 nm. The use of BSE detector brings the opportunity to measure the thickness of not only the electron transparent samples as in case of qSTEM, but also thin layers on substrates – qBSE. Both above-mentioned methods (qSTEM and qBSE) are intensity-based. This brings complication in the need of proper calibration, where just a slight drift of base-signal level causes a significant change of the results. This insufficiency was overcome in case of qSTEM by using the most probable scattering angle (captured by pixelated STEM detector) instead of an integral image intensity captured by an annular segment of STEM detector. The advantage of this method is its applicability post-acquisition, where no special previous actions are needed before each imaging session. The disadvantage is the limited range of detectable thicknesses given by the peak creation in signal/scattering-angle dependency. In general, low thickness region is immeasurable as well as those too thick (usable thickness range for latex is 185 - 1

Tato práce se zabývá možnostmi kvantitativního zobrazování ve skenovacím (transmisním) elektronovém mikroskopu (S|T|EM) společně s jejich korelativní aplikací. Práce začíná popisem metody kvantitativního STEM (qSTEM), kde lze stanovenou lokální tloušťku vzorku dát do spojitosti s ozářenou dávkou, a vytvořit tak studii úbytku hmoty. Tato metoda byla použita při studiu ultratenkých řezů zalévací epoxidové pryskyřice za různých podmínek (stáří, teplota, kontrastování, čištění pomocí plazmy, pokrytí uhlíkem, proud ve svazku). V rámci této části jsou diskutovány a demonstrovány možnosti kalibračního procesu detektoru, nezbytné pozadí Monte Carlo simulací elektronového rozptylu a dosažitelná přesnost metody. Metoda je pak rozšířena pro použití detektoru zpětně odražených elektronů (BSE), kde byla postulována, vyvinuta a testována nová kalibrační technika založená na odrazu primárního svazku na elektronovém zrcadle. Testovací vzorky byly různě tenké vrstvy v tloušťkách mezi 1 až 25 nm. Použití detektoru BSE přináší možnost měřit tloušťku nejen elektronově průhledných vzorků jako v případě qSTEM, ale také tenkých vrstev na substrátech - qBSE. Obě výše uvedené metody (qSTEM a qBSE) jsou založeny na intenzitě zaznamenaného obrazu, a to přináší komplikaci, protože vyžadují správnou kalibraci detektoru, kde jen malý posun úrovně základního signálu způsobí významnou změnu výsledků. Tato nedostatečnost byla překonána v případě qSTEM použitím nejpravděpodobnějšího úhlu rozptylu (zachyceného pixelovaným STEM detektorem), namísto integrální intenzity obrazu zachycené prstencovým segmentem detektoru STEM. Výhodou této metody je její použitelnost i na data, která nebyla předem zamýšlena pro využití qSTEM, protože pro aplikaci metody nejsou potřeba žádné zvláštní předchozí kroky. Nevýhodou je omezený rozsah detekovatelných tlouštěk vzorku způsobený absencí píku v závislosti signálu na úhlu rozptylu. Obecně platí, že oblast s malou tloušťkou je neměřitelná stejně tak jako tloušťka příli, This thesis deals with the possibilities of quantitative imaging in scanning (transmission) electron microscope (S|T|EM) together with its correlative applications. It starts with quantitative STEM (qSTEM) method description, where estimated local sample thickness can be related to irradiated dose and create a mass-loss study, which was applied on samples of ultrathin epoxy resin sections at variate conditions (age, temperature, staining, plasma cleaning, carbon covering, probe current). The possibilities of the detector calibration process, the necessary background of the Monte Carlo simulations of electron scattering and achievable accuracy of the method are discussed and demonstrated. The method is then extrapolated for the use of back-scattered electron (BSE) detector, where new detector calibration technique, based on primary beam deflection on electron mirror, was postulated, developed and tested on various thin coating layers with thicknesses in range from 1 to 25 nm. The use of BSE detector brings the opportunity to measure the thickness of not only the electron transparent samples as in case of qSTEM, but also thin layers on substrates – qBSE. Both above-mentioned methods (qSTEM and qBSE) are intensity-based. This brings complication in the need of proper calibration, where just a slight drift of base-signal level causes a significant change of the results. This insufficiency was overcome in case of qSTEM by using the most probable scattering angle (captured by pixelated STEM detector) instead of an integral image intensity captured by an annular segment of STEM detector. The advantage of this method is its applicability post-acquisition, where no special previous actions are needed before each imaging session. The disadvantage is the limited range of detectable thicknesses given by the peak creation in signal/scattering-angle dependency. In general, low thickness region is immeasurable as well as those too thick (usable thickness range for latex is 185 - 1

Tato práce se zabývá možnostmi kvantitativního zobrazování ve skenovacím (transmisním) elektronovém mikroskopu (S|T|EM) společně s jejich korelativní aplikací. Práce začíná popisem metody kvantitativního STEM (qSTEM), kde lze stanovenou lokální tloušťku vzorku dát do spojitosti s ozářenou dávkou, a vytvořit tak studii úbytku hmoty. Tato metoda byla použita při studiu ultratenkých řezů zalévací epoxidové pryskyřice za různých podmínek (stáří, teplota, kontrastování, čištění pomocí plazmy, pokrytí uhlíkem, proud ve svazku). V rámci této části jsou diskutovány a demonstrovány možnosti kalibračního procesu detektoru, nezbytné pozadí Monte Carlo simulací elektronového rozptylu a dosažitelná přesnost metody. Metoda je pak rozšířena pro použití detektoru zpětně odražených elektronů (BSE), kde byla postulována, vyvinuta a testována nová kalibrační technika založená na odrazu primárního svazku na elektronovém zrcadle. Testovací vzorky byly různě tenké vrstvy v tloušťkách mezi 1 až 25 nm. Použití detektoru BSE přináší možnost měřit tloušťku nejen elektronově průhledných vzorků jako v případě qSTEM, ale také tenkých vrstev na substrátech - qBSE. Obě výše uvedené metody (qSTEM a qBSE) jsou založeny na intenzitě zaznamenaného obrazu, a to přináší komplikaci, protože vyžadují správnou kalibraci detektoru, kde jen malý posun úrovně základního signálu způsobí významnou změnu výsledků. Tato nedostatečnost byla překonána v případě qSTEM použitím nejpravděpodobnějšího úhlu rozptylu (zachyceného pixelovaným STEM detektorem), namísto integrální intenzity obrazu zachycené prstencovým segmentem detektoru STEM. Výhodou této metody je její použitelnost i na data, která nebyla předem zamýšlena pro využití qSTEM, protože pro aplikaci metody nejsou potřeba žádné zvláštní předchozí kroky. Nevýhodou je omezený rozsah detekovatelných tlouštěk vzorku způsobený absencí píku v závislosti signálu na úhlu rozptylu. Obecně platí, že oblast s malou tloušťkou je neměřitelná stejně tak jako tloušťka příli, This thesis deals with the possibilities of quantitative imaging in scanning (transmission) electron microscope (S|T|EM) together with its correlative applications. It starts with quantitative STEM (qSTEM) method description, where estimated local sample thickness can be related to irradiated dose and create a mass-loss study, which was applied on samples of ultrathin epoxy resin sections at variate conditions (age, temperature, staining, plasma cleaning, carbon covering, probe current). The possibilities of the detector calibration process, the necessary background of the Monte Carlo simulations of electron scattering and achievable accuracy of the method are discussed and demonstrated. The method is then extrapolated for the use of back-scattered electron (BSE) detector, where new detector calibration technique, based on primary beam deflection on electron mirror, was postulated, developed and tested on various thin coating layers with thicknesses in range from 1 to 25 nm. The use of BSE detector brings the opportunity to measure the thickness of not only the electron transparent samples as in case of qSTEM, but also thin layers on substrates – qBSE. Both above-mentioned methods (qSTEM and qBSE) are intensity-based. This brings complication in the need of proper calibration, where just a slight drift of base-signal level causes a significant change of the results. This insufficiency was overcome in case of qSTEM by using the most probable scattering angle (captured by pixelated STEM detector) instead of an integral image intensity captured by an annular segment of STEM detector. The advantage of this method is its applicability post-acquisition, where no special previous actions are needed before each imaging session. The disadvantage is the limited range of detectable thicknesses given by the peak creation in signal/scattering-angle dependency. In general, low thickness region is immeasurable as well as those too thick (usable thickness range for latex is 185 - 1