scholarly journals Internal water storage capacity of terrestrial planets and the effect of hydration on the M-R relation

2021 ◽  
Author(s):  
Oliver Shah ◽  
Ravit Helled ◽  
Yann Alibert ◽  
Klaus Mezger
Keyword(s):  
Mass Fraction ◽  
Bulk Composition ◽  
Deep Ocean ◽  
Mass Range ◽  
Variable Boundary ◽  
Water Storage Capacity ◽  
Surface Ocean ◽  
Theoretical Mass ◽  
The Galaxy ◽  
Physical And Chemical

<p>The discovery of low density exoplanets in the super-Earth mass regime suggests that ocean planets could be abundant in the galaxy. Understanding the chemical interactions between water and Mg-silicates or iron is essential for constraining the interiors of water-rich planets. Hydration effects have, however, been mostly neglected by the astrophysics community so far. As such effects are unlikely to have major impacts on theoretical mass-radius relations, this is justified as long as the measurement uncertainties are large. However, upcoming missions, such as the PLATO mission (scheduled launch 2026), are envisaged to reach a precision of up to ≈ 3% and ≈ 10% for radii and masses, respectively. As a result, we may soon enter an area in exoplanetary research where various physical and chemical effects such as hydration can no longer be ignored. We have constructed interior models for planets that include reliable prescriptions for hydration of the cores and mantles. These models can be used to refine previous results for which hydration has been neglected and to guide future characterization of observed exoplanets. We have developed numerical tools to solve for the structure of multi-layered planets with variable boundary conditions and compositions. Here we have considered three types of planets: dry interiors, hydrated interiors, and dry interiors plus surface ocean, where the ocean mass fraction corresponds to the mass fraction of the H<sub>2</sub>O equivalent in the hydrated case. We find H and OH storage capacities in the hydrated planets equivalent to 0 - 6 wt% H<sub>2</sub>O corresponding to up to ≈800 km deep ocean layers. In the mass range 0.1 ≤ M/M<sub>⊕</sub> ≤ 3, the effect of hydration on the total radius is found to be ≤ 2.5%, whereas the effect of separation into an isolated surface ocean is ≤ 5 %. Furthermore, we find that our results are very sensitive to the bulk composition.</p>

scholarly journals Internal water storage capacity of terrestrial planets and the effect of hydration on the M-R relation

2021 ◽  
Vol 646 ◽  
pp. A162
Author(s):  
O. Shah ◽  
Y. Alibert ◽  
R. Helled ◽  
K. Mezger
Keyword(s):  
Mass Fraction ◽  
Bulk Composition ◽  
Deep Ocean ◽  
Mass Range ◽  
Variable Boundary ◽  
Water Storage Capacity ◽  
Surface Ocean ◽  
Theoretical Mass ◽  
The Galaxy ◽  
Physical And Chemical

Context. The discovery of low density exoplanets in the super-Earth mass regime suggests that ocean planets could be abundant in the galaxy. Understanding the chemical interactions between water and Mg-silicates or iron is essential for constraining the interiors of water-rich planets. Hydration effects have, however, been mostly neglected by the astrophysics community so far. As such effects are unlikely to have major impacts on theoretical mass-radius relations, this is justified as long as the measurement uncertainties are large. However, upcoming missions, such as the PLATO mission (scheduled launch 2026), are envisaged to reach a precision of up to ≈3 and ≈10% for radii and masses, respectively. As a result, we may soon enter an area in exoplanetary research where various physical and chemical effects such as hydration can no longer be ignored. Aims. Our goal is to construct interior models for planets that include reliable prescriptions for hydration of the cores and mantles. These models can be used to refine previous results for which hydration has been neglected and to guide future characterization of observed exoplanets. Methods. We have developed numerical tools to solve for the structure of multi-layered planets with variable boundary conditions and compositions. Here we consider three types of planets: dry interiors, hydrated interiors, and dry interiors plus surface ocean, where the ocean mass fraction corresponds to the mass fraction of the H2O equivalent in the hydrated case. Results. We find H and OH storage capacities in the hydrated planets equivalent to 0−6 wt% H2O corresponding to up to ≈800 km deep ocean layers. In the mass range 0.1 ≤ M∕M⊕≤ 3, the effect of hydration on the total radius is found to be ≤2.5%, whereas the effect of separation into an isolated surface ocean is ≤5%. Furthermore, we find that our results are very sensitive to the bulk composition.

Statistical criteria of stellar population types

1966 ◽  
Vol 24 ◽  
pp. 101-110
Author(s):  
W. Iwanowska
Keyword(s):  
Stellar Population ◽  
Chemical Properties ◽  
Spectrophotometric Study ◽  
Physical And Chemical Properties ◽  
Population Type ◽  
The Galaxy ◽  
Distribution Parameters ◽  
Physical And Chemical ◽  
Statistical Criteria ◽  
And Chemical Properties

In connection with the spectrophotometric study of population-type characteristics of various kinds of stars, a statistical analysis of kinematical and distribution parameters of the same stars is performed at the Toruń Observatory. This has a twofold purpose: first, to provide a practical guide in selecting stars for observing programmes, second, to contribute to the understanding of relations existing between the physical and chemical properties of stars and their kinematics and distribution in the Galaxy.

Authenticity Identification of Carbonated Alcochol-Free Beverages

Food Industry ◽  
2020 ◽  
Vol 5 (1) ◽  
pp. 16-22
Author(s):  
Irina Reznichenko ◽  
Maria Kondratieva
Keyword(s):  
Mass Fraction ◽  
Soft Drinks ◽  
Alcoholic Beverages ◽  
Consumer Market ◽  
Score System ◽  
Regulatory Documents ◽  
Chemical Indicators ◽  
Physico Chemical ◽  
Alcoholic Drinks ◽  
Physical And Chemical

The article concerns the counterfeiting problem of non-alcoholic drinks sold on the consumer market of the Russian Federation; provides data on drinks fraud methods (assortment, qualitative, quantitative and informational types). Strengthening quality control of soft drinks is one of the main directions of providing consumers with qualitative products. The authors presented authenticity identification results of carbonated soft drinks sold on the Kemerovo consumer market for compliance with the current regulatory documents requirements; run the consumer criteria analysis for the drinks identification of various brands. They obtained data on the labeling and packaging identification of selected non-alcoholic carbonated drinks samples for the compliance with current regulatory documents. A man recorded the compliance. There was an absence of the quantitative counterfeiting identification. The study described results of the organoleptic and physico-chemical quality indicators research. According to the GOST 28188-2014 “Non-Alcoholic Beverages. General Technical Conditions” the authors evaluated beverages quality by such physical and chemical indicators as the mass fraction of dry substances, acidity, and the mass fraction of carbon dioxide. The researchers run the organoleptic indicators analysis according to a score system. Authenticity identification of the selected drinks samples showed that there are no signs of counterfeiting and the products are of high quality.

scholarly journals An optical observational cluster mass function at z ∼ 1 with the ORELSE survey

2021 ◽  
Vol 502 (3) ◽  
pp. 3942-3954
Author(s):  
D Hung ◽  
B C Lemaux ◽  
R R Gal ◽  
A R Tomczak ◽  
L M Lubin ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Large Scale ◽  
Near Infrared ◽  
Function Analysis ◽  
Voronoi Tessellation ◽  
Cosmological Parameters ◽  
Mass Range ◽  
Mass Function ◽  
Cluster Mass ◽  
Theoretical Mass

ABSTRACT We present a new mass function of galaxy clusters and groups using optical/near-infrared (NIR) wavelength spectroscopic and photometric data from the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. At z ∼ 1, cluster mass function studies are rare regardless of wavelength and have never been attempted from an optical/NIR perspective. This work serves as a proof of concept that z ∼ 1 cluster mass functions are achievable without supplemental X-ray or Sunyaev-Zel’dovich data. Measurements of the cluster mass function provide important contraints on cosmological parameters and are complementary to other probes. With ORELSE, a new cluster finding technique based on Voronoi tessellation Monte Carlo (VMC) mapping, and rigorous purity and completeness testing, we have obtained ∼240 galaxy overdensity candidates in the redshift range 0.55 < z < 1.37 at a mass range of 13.6 < log (M/M⊙) < 14.8. This mass range is comparable to existing optical cluster mass function studies for the local universe. Our candidate numbers vary based on the choice of multiple input parameters related to detection and characterization in our cluster finding algorithm, which we incorporated into the mass function analysis through a Monte Carlo scheme. We find cosmological constraints on the matter density, Ωm, and the amplitude of fluctuations, σ8, of $\Omega _{m} = 0.250^{+0.104}_{-0.099}$ and $\sigma _{8} = 1.150^{+0.260}_{-0.163}$. While our Ωm value is close to concordance, our σ8 value is ∼2σ higher because of the inflated observed number densities compared to theoretical mass function models owing to how our survey targeted overdense regions. With Euclid and several other large, unbiased optical surveys on the horizon, VMC mapping will enable optical/NIR cluster cosmology at redshifts much higher than what has been possible before.

scholarly journals Data-Independent Acquisition for the Quantification and Identification of Metabolites in Plasma

Metabolites ◽  
2020 ◽  
Vol 10 (12) ◽  
pp. 514
Author(s):  
Tom van der Laan ◽  
Isabelle Boom ◽  
Joshua Maliepaard ◽  
Anne-Charlotte Dubbelman ◽  
Amy C. Harms ◽  
...  
Keyword(s):  
Mass Spectra ◽  
Mass Range ◽  
Correct Identification ◽  
Hydrophilic Interaction ◽  
Specific Mass ◽  
Structural Isomers ◽  
Data Independent Acquisition ◽  
Targeted Analysis ◽  
Theoretical Mass ◽  
Accurate Quantification

A popular fragmentation technique for non-targeted analysis is called data-independent acquisition (DIA), because it provides fragmentation data for all analytes in a specific mass range. In this work, we demonstrated the strengths and weaknesses of DIA. Two types of chromatography (fractionation/3 min and hydrophilic interaction liquid chromatography (HILIC)/18 min) and three DIA protocols (variable sequential window acquisition of all theoretical mass spectra (SWATH), fixed SWATH and MSALL) were used to evaluate the performance of DIA. Our results show that fast chromatography and MSALL often results in product ion overlap and complex MS/MS spectra, which reduces the quantitative and qualitative power of these DIA protocols. The combination of SWATH and HILIC allowed for the correct identification of 20 metabolites using the NIST library. After SWATH window customization (i.e., variable SWATH), we were able to quantify ten structural isomers with a mean accuracy of 103% (91–113%). The robustness of the variable SWATH and HILIC method was demonstrated by the accurate quantification of these structural isomers in 10 highly diverse blood samples. Since the combination of variable SWATH and HILIC results in good quantitative and qualitative fragmentation data, it is promising for both targeted and untargeted platforms. This should decrease the number of platforms needed in metabolomics and increase the value of a single analysis.

scholarly journals Cosmological simulations of low-mass galaxies: some potential issues

2010 ◽  
Vol 6 (S270) ◽  
pp. 503-506
Author(s):  
Pedro Colín ◽  
Vladimir Avila-Reese ◽  
Octavio Valenzuela
Keyword(s):  
Star Formation ◽  
Adaptive Mesh Refinement ◽  
Mass Fraction ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mesh Refinement ◽  
Adaptive Mesh ◽  
Stellar Mass ◽  
The Galaxy ◽  
Low Mass

AbstractCosmological Adaptive Mesh Refinement simulations are used to study the specific star formation rate (sSFR=SSF/Ms) history and the stellar mass fraction, fs=Ms/MT, of small galaxies, total masses MT between few × 1010 M⊙ to few ×1011 M⊙. Our results are compared with recent observational inferences that show the so-called “downsizing in sSFR” phenomenon: the less massive the galaxy, the higher on average is its sSFR, a trend seen at least since z ~ 1. The simulations are not able to reproduce this phenomenon, in particular the high inferred values of sSFR, as well as the low values of fs constrained from observations. The effects of resolution and sub-grid physics on the SFR and fs of galaxies are discussed.

scholarly journals ИССЛЕДОВАНИЕ ВЛИЯНИЯ ОБРАБОТКИ ГОРЯЧИМ ТУМАНОМ БИОЛОГИЧЕСКИХ ПРЕПАРАТОВ И ГУМИНОВЫХ ПРОДУКТОВ СЕМЯН ЯЧМЕНЯ

2019 ◽  
Author(s):  
M.Yu. KOSTENKO ◽  
G. RYMBALOVICH ◽  
I.N. GORYACHKINA ◽  
R.V. BEZNOSYUK ◽  
G.A. BORISOV
Keyword(s):  
Mass Fraction ◽  
Treatment Options ◽  
Experimental Studies ◽  
Metabolic Energy ◽  
Potassium Humate ◽  
Protein Mass ◽  
Biological Yield ◽  
Small Grains ◽  
Humic Products ◽  
Physical And Chemical

Целью исследований явилась оценкавлияния обработки горячим туманом биологического препарата Азотовит и гуминовых продуктовГумат калия, Экоростсемян ячменя перед посевом, а также сравнение результатов с общепринятымитехнологиями обработки с помощью протравителя семян этими же препаратами. Для полноты исследований обработку производили и химическим препаратом Атик. Высокодисперсный аэрозоль получали с помощью генератора горячего тумана GreenFogBF-130.Обработку производилис помощью устройства с наклонными полками, по которым зерно многократно пересыпалось под действием силы тяжести и подвергалось перемешиванию и воздействию горячего тумана. В результате разницы температур холодного семенного материала и горячего тумана происходил фазовый переход тумана в жидкость, что позволяло получить тонкую плёнку на обрабатываемой поверхности семянячменя.Это способствовало обеззараживанию и активизации физико-химических процессов в зерне. Экспериментальные исследования включали восемь вариантов обработки и один без обработки (контроль). Оценивались результаты продуктивности и структура урожая: число растений на 1 м2, число сорных растений на 1 м2, число продуктивных стеблей (колосьев) на 1 м2, кустистость на 1 м2, продуктивная кустистость на 1 м2,среднее число зерен в колосе, масса 1000 зерен, высота стеблей, биологическая урожайность. В соответствии с ГОСТ 53900-2010 Ячмень кормовой, ГОСТ 5060-86 Ячмень пивоваренный, ГОСТ 28672-90 Ячмень.Требования при заготовках и поставках,ТРТС 021/2011 О безопасности пищевой продукции из качественных показателей рассматривались массовая доля влаги, массовая доля протеина, массовая доля клетчатки, массовая доля сахара, массовая доля жира, массовая доля золы, массовая доля крахмала, обменная энергия, крупность, мелкие зерна, сорная и зерновая примесь, фузариозные зерна, общая токсичность, микотоксиндезоксиниваленол (DON). Лучшие показатели были получены в результате аэрозольной обработки гуминовыми продуктами Гумат калия и Экорост.The aim of the research was to assess the effect of hot mist treatment of the biological preparation Azotovit and humic products potassium HUMATE, barley seeds Ecorost before sowing, as well as to compare the results with conventional technologies of treatment with the help of seed protectant with the same drugs. To complete the research and produce treatment chemicals of Atik. The highly dispersed aerosol was obtained using The greenfogbf-130 hot mist generator. The treatment was carried out using a device with inclined shelves, on which the grain was repeatedly poured under the influence of gravity and was subjected to mixing and the influence of hot fog. As a result of the temperature difference between the cold and hot mist of the seed material, a phase transition of the mist into a liquid occurred, which allowed to obtain a thin film on the treated surface of the barley seeds. This contributed to the disinfection and activation of physical and chemical processes in the grain. Experimental studies included eight treatment options and one without treatment (control). The results of productivity and crop structure were evaluated: the number of plants per 1 m2, the number of weeds per 1 m2, the number of productive stems (ears) per 1 m2, bushiness per 1 m2, productive bushiness per 1 m2, the average number of grains per ear, the weight of 1000 grains, the height of stems, biological yield. In accordance with GOST 53900-2010 barley fodder, barley brewing GOST 5060-86, GOST 28672-90 Barley. Requirements for procurement and supply, TR CU 021/2011 on food safety from qualitative indicators considered the mass fraction of moisture, mass fraction of protein, mass fraction of fiber, mass fraction of sugar, mass fraction of fat, mass fraction of ash, mass fraction of starch, metabolic energy, size, small grains, weed and grain admixture, Fusarium grains, total toxicity, mycotoxindeoxynivalenol (don). The best results were obtained as a result of aerosol treatment with humic products potassium HUMATE and Ecorost.

Insights into the ocean’s biological carbon pump: What makes marine snow falling into the deep ocean?

2021 ◽  
Author(s):  
Frederic Le Moigne
Keyword(s):  
Carbon Cycle ◽  
Global Analysis ◽  
Deep Ocean ◽  
Ecosystem Structure ◽  
Faecal Pellets ◽  
Surface Ocean ◽  
Mesopelagic Zone ◽  
Carbon Pump ◽  
Biological Carbon Pump

<p>The oceanic biological carbon pump (BCP) regulates the Earth carbon cycle by transporting part of the photosynthetically fixed CO<sub>2</sub> into the deep ocean. Suppressing this mechanism would result in an important increase of atmospheric CO<sub>2</sub> level. The BCP occurs mainly in the form of organic carbon particles (POC) sinking out the surface ocean. Various types of particles are produced in surface ocean. They all differ in production, sinking and decomposition rates, vertically and horizontally. The amount of POC transported to depths via these various export pathways as well as their decomposition pathways all have different ecological origins and therefore may response differently to climate change. Here I will briefly review some of the processes driving both particle export out of the euphotic zone (0-100m) as well as particles transport within the mesopelagic zone (100-1000m). In the early 2000s, strong correlations between POC and mineral (calcite an opal) fluxes observed in the deep ocean have inspired the inclusion of “ballast effect” parameterizations in carbon cycle models. These relationships were first considered as being universal. However global analysis of POC and mineral ballast fluxes showed that mineral ballasting is important in regions like the high-latitude North Atlantic but that in most places (some of which efficiently exporting) the unballasted fraction often dominates the export flux. In such regions, we later showed that zooplankton-mediated export (presence of faecal pellets) and surface microbial abundance were important drivers of the efficiency of particles export. Similar trends were found globally by including bacteria and zooplankton abundances to a global reanalysis of the global variations of the POC export efficiency. This implies that the whole ecosystem structure from bacteria to fishes, rather than just the phytoplankton community, is important in setting the strength of the biological carbon pump. Further down in the water column (mesopelagic zone), processes impacting the transport of particles are less clear. Sinking particles experience a number of biotic and abiotic transformations during their descent. These includes solubilization, remineralisation, fragmentation, ingestion/active transport, breakdown among others. While some potential factors such as O<sub>2</sub> concentration and temperature have been proposed as powerful controls, global evidences are often inconsistent. In the award talk, I will review current challenges related to the role of particles consumption by zooplankton and fishes as well as the role of particles attached prokaryotes (bacteria and archaea) in setting the efficiency of the carbon transport in the mesopelagic zone.</p>

scholarly journals Probing gaseous halos of galaxies with radio jets

2019 ◽  
Vol 627 ◽  
pp. A113 ◽  
Author(s):  
Martin G. H. Krause ◽  
Martin J. Hardcastle ◽  
Stanislav S. Shabala
Keyword(s):  
Low Frequency ◽  
Mass Range ◽  
Mass Scale ◽  
Radio Luminosity ◽  
Marked Rise ◽  
Radio Jets ◽  
Upper Limit ◽  
The Galaxy ◽  
Galaxy Masses ◽  
Halo Gas

Context. Gaseous halos play a key role in understanding inflow, feedback, and the overall baryon budget in galaxies. Literature models predict transitions of the state of the gaseous halo between cold and hot accretion, winds, fountains, and hydrostatic halos at certain galaxy masses. Since luminosities of radio AGN are sensitive to halo densities, any significant transition would be expected to show up in the radio luminosities of large samples of galaxies. The LOw Frequency ARray (LOFAR) Two-Metre Sky Survey (LoTSS) has identified a galaxy stellar mass scale, 1011 M⊙, above which the radio luminosities increase disproportionately. Aims. We investigate if radio luminosities of galaxies, especially the marked rise at galaxy masses around 1011 M⊙, can be explained with standard assumptions regarding jet powers, scaling between black hole mass and galaxy mass, and gaseous halos. Methods. Based on observational data and theoretical constraints, we developed models for the radio luminosity of radio AGN in halos under infall, galactic wind, and hydrostatic conditions. We compared these models to LoTSS data for a large sample of galaxies in the mass range between 108.5 M⊙ and 1012 M⊙. Results. Under the assumption that the same characteristic upper limit to jet powers known from high galaxy masses holds at all masses, we find the maximum radio luminosities for the hydrostatic gas halos to lie close to the upper envelope of the distribution of the LOFAR data. The marked rise in radio luminosity at 1011 M⊙ is matched in our model and is related to a significant change in halo gas density around this galaxy mass, which is a consequence of lower cooling rates at a higher virial temperature. Wind and infall models overpredict the radio luminosities for small galaxy masses and have no particular steepening of the run of the radio luminosities predicted at any galaxy mass. Conclusions. Radio AGN could have the same characteristic Eddington-scaled upper limit to jet powers in galaxies of all masses in the sample if the galaxies have hydrostatic gas halos in phases when radio AGN are active. We find no evidence of a change of the type of galaxy halo with the galaxy mass. Galactic winds and quasi-spherical cosmological inflow phases cannot frequently occur at the same time as powerful jet episodes unless the jet properties in these phases are significantly different from what we assumed in our model.

scholarly journals DIALib-QC an assessment tool for spectral libraries in data-independent acquisition proteomics

2020 ◽  
Vol 11 (1) ◽  
Author(s):  
Mukul K. Midha ◽  
David S. Campbell ◽  
Charu Kapil ◽  
Ulrike Kusebauch ◽  
Michael R. Hoopmann ◽  
...  
Keyword(s):  
Quality Control ◽  
Assessment Tool ◽  
Software Tool ◽  
Mass Range ◽  
Systematic Evaluation ◽  
Label Free ◽  
Mass Spectral ◽  
Data Independent Acquisition ◽  
Theoretical Mass ◽  
Spectral Libraries

Abstract Data-independent acquisition (DIA) mass spectrometry, also known as Sequential Window Acquisition of all Theoretical Mass Spectra (SWATH), is a popular label-free proteomics strategy to comprehensively quantify peptides/proteins utilizing mass spectral libraries to decipher inherently multiplexed spectra collected linearly across a mass range. Although there are many spectral libraries produced worldwide, the quality control of these libraries is lacking. We present the DIALib-QC (DIA library quality control) software tool for the systematic evaluation of a library’s characteristics, completeness and correctness across 62 parameters of compliance, and further provide the option to improve its quality. We demonstrate its utility in assessing and repairing spectral libraries for correctness, accuracy and sensitivity.

Sign in / Sign up

Export Citation Format

Share Document