Investigating the effect of coir substrate on the growth, yield and quality of sweet pepper (Capsicum annuum) varieties

Text in English with abstracts and keywords in English, Afrikaans and SepediCrop yield is the industry standard for calculating the amount of horticultural produce harvested. As a result, producing sufficient quantities of quality biochemical ingredients can help to solve food security and nutritional issues. To ensure an adequate food supply, the use of organic substrate, as opposed to natural soils, is preferred by many growers for greenhouse cultivation of crops such as peppers. The aim of the study was to determine the effect of coconut coir substrate on the yield and biochemical constituents of pepper varieties grown under greenhouse conditions. Two sweet peppers varieties (Sondela and Ilanga) were grown in fertigated coconut coir (experiment) or loamy soil (control) under greenhouse conditions for two consecutive growing seasons in 2021 and 2022. The number of pepper fruits, as well as their dried weight and selected biochemical contents, were investigated. Quantification was done using the concentration of dry matter and selected biochemical constituents from freeze-dried fruit samples. Results illustrated that the treatment combination of coconut coir and variety (Ilanga) resulted in a higher fruit number when compared to other treatments. Biochemical constituents such as vitamins, total phenols, total flavonoids, copper, iron and zinc were superior in fruits grown under coir substrate when compared to loamy soil (control). Therefore, farmers are encouraged to grow sweet peppers varieties under coconut coir substrate for better yield, nutritional quality and profit maximisation.Opbrengste is die standaard waarvolgens die bedryf bepaal hoeveel tuinbouprodukte geoes is. Die vervaardiging van voldoende hoeveelhede eersteklas biochemiese bestanddele kan voedselveiligheid verseker en voedingstekorte aanvul. Die meeste kwekers verkies ’n organiese substraat bo natuurlike grond om gewasse soos soetrissies in kweekhuise te verbou omdat die gewasse sodoende genoegsame voeding ontvang. Hierdie studie wou vasstel of ʼn klapperhaarsubstraat enige uitwerking het op die opbrengs en biochemiese samestelling van soetrissievariëteite wat in ʼn kweekhuis verbou word. Twee soetrissievariëteite (Sondela en Ilanga) is in twee opeenvolgende seisoene (2021 en 2022) in ʼn kweekhuis in bemeste klapperhaar en ook in leemgrond (die kontrole) geplant. Die aantal soetrissievrugte, hulle droë gewig asook ʼn keur van hul biochemiese bestanddele is ontleed. Die kwantifisering is gedoen op grond van ʼn konsentrasie droë materie en ʼn keur van die biochemiese bestanddele van vriesgedroogde vrugtemonsters. Daar is bevind dat die kombinasie van klapperhaar en variëteit (Ilanga) ʼn groter opbrengs as enige ander behandeling lewer. Die biochemiese bestanddele van vrugte wat in ʼn klapperhaarsubstraat gekweek is, soos vitamiene, totale fenol, totale flavonoïed, koper, yster en sink, was van ʼn hoër gehalte as dié van vrugte wat in leemgrond (die kontrole) gekweek is. Boere word dus aangeraai om soetrissievariëteite in ʼn klapperhaarsubstraat te kweek met die oog op ʼn hoër opbrengs, groter voedingswaarde en ʼn maksimumwins.Palo ya tšweletšo ya temo ya dibjalo tšeo di bunnwego ke maemo ao a šomišwago ke intasteri go lekola ditšweletšwa tša temo tšeo di bunnwego. Ka lebaka leo, go tšweletša palo ye e lekanego ya metswako ya boleng ya dikhemikhale tša phepo ya dibjalo go ka thuša go rarolla mathata a tšhireletšo ya dijo le mathata a tša phepo. Tšhomišo ya manyora a tlhago ka ntlong ya go godiša dibjalo tše bjalo ka dipherefere go netefatša gore go na le kabo ya dijo ye e lekanego, ke mokgwa wo o šomišwago ke bontši bja balemi bakeng sa mabu a tlhago. Maikemišetšo a nyakišišo ye e be e le go laetša khuetšo ya morole wa khokhonate go puno le metswako ya dikhemikhale tša phepo ya dibjalo go mehuta ya pherefere ye bjetšwego ka gare ga ntlo ya go godiša dibjalo. Mehuta e mebedi ya pherefere e bose (Sondela le Ilanga) e bjetšwe ka gare ga morole wa khokhonate wo o nontšhitšwego le go nošetšwa le mobu wa serota goba seloko (taolo) ka gare ga ntlo ya go godiša ka dihla tše pedi tša go latelana [2021 le 2022]. Palo ya dienywa tša pherefere, gammogo le boima bja tše di omilego le metswako ye e kgethilwego tša dikhemikhale tša phepo ya dibjalo, di ile tša nyakišišwa. Tekanyo e dirilwe ka go šomiša motswako wa dikarolo tša kgolo ya dibjalo tšeo di omilego le dikarolo tše di kgethilwego tša dikhemikhale tša phepo ya dibjalo go tšwa go disampole tša dienywa tše di omišitšwego le go kgahlišwa ka setšidifatši. Dipoelo tša nyakišišo di laeditše gore mokgwa wa go tswaka morole wa khokhonate le mehuta e mengwe (Ilanga) go bile le puno ye kgolo ya dienywa ge go bapetšwa le mekgwa e mengwe. Dikarolo tša dikhemikhale tša phepo ya dibjalo bjalo ka dibithamini, palomoka ya diphenole, palomoka ya difolavonoite, koporo, tšhipi le zinki di hweditšwe go dienywa tša go bjalwa ka fase ga manyora ge e bapetšwa le dienywa tša go bjalwa mmung wa serota goba seloko (taolo). Bjalo, balemi ba hlohleletšwa go bjala mehuta ya go fapana ya di pherefere tše di bose ka fase ga morole wa khokhonate go tšweletša puno e kaone, boleng bja phepo le go oketša letseno.Agriculture and  Animal HealthM. Sc. (Agriculture

Acceleration and Deceleration in Curvature Induced Phantom Model of the Late and Future Universe, Cosmic Collapse as Well as its Quantum Escape

Here, cosmology of the late and future universe is obtained from $f(R)$-gravity with non-linear curvature terms $R^2$ and $R^3$ ($R$ being the Ricci scalar curvature). It is different from $f(R)$-dark enrgy models, where non-linear curvature terms are taken as gravitational alternative of dark energy. In the present model, neither linear nor no-linear curvature terms are taken as dark energy. Rather, dark energy terms are induced by curvature terms in the Friedmann equation derived from $f(R)$-gravitational equations. It has advantage over $f(R)$- dark energy models in the sense that the present model satisfies WMAP results and expands as $\sim t^{2/3}$ during matter-dominance. So, it does not have problems due to which $f(R)$-dark energy models are criticized. Curvature-induced dark energy, obtained here, mimics phantom. Different phases of this model, including acceleration and deceleration during phantom phase, are investigated here.It is found that expansion of the universe will stop at the age $(3.87 t_0 + 694.4 {\rm kyr})$ ($t_0$ being the present age of the universe) and after this epoch, it will contract and collapse by the time $(336.87 t_0 + 694.4 {\rm kyr})$. Further,it is shown that universe will escape predicted collapse (obtained using classical mechanics) on making quantum gravity corrections relevant near collapse time due to extremely high energy density and large curvature analogous to the state of very early universe. Interestingly, cosmological constant is also induced here, which is very small in classical domain, but very high in quantum domain.Comment: 33 page

Fluoroscopic findings of swallowing: comparison between preterm and full-term infants

OBJETIVO: Descrever os achados fluoroscópicos da deglutição de recém-nascidos pré-termo de zero a seis meses de idade, assim como as doenças e os sinais e sintomas clínicos relacionados à alteração na deglutição, e compará-los com os respectivos dados obtidos de recém-nascidos de termo. MÉTODOS: Foram analisados, retrospectivamente, os dados das avaliações fluoroscópicas realizadas no período de um ano em lactentes de zero a seis meses de idade e aos respectivos prontuários. Participaram 40 sujeitos, divididos em dois grupos: Grupo Pré-Termo, constituído de 23 recém-nascidos pré-termo; e Grupo de Termo, constituído por 17 recém-nascidos de termo. RESULTADOS: Os principais achados fluoroscópicos da deglutição observados em ambos os grupos foram refluxo para a nasofaringe e refluxo gastresofágico. Não houve diferença entre os grupos para a presença de alteração na deglutição . O Grupo Pré-Termo apresentou mais problemas cardíacos do que o Grupo de Termo. Não houve diferença entre os grupos para problemas neurológicos e respiratórios. Em relação aos sinais e sintomas clínicos sugestivos de alteração na deglutição, o Grupo Pré-Termo apresentou mais dessaturação de oxigênio e o Grupo de Termo mais vômitos. CONCLUSÃO: Os principais achados fluoroscópicos da deglutição encontrados em recém-nascidos pré-termo de zero a seis meses de idade foram refluxo para a nasofaringe e refluxo gastresofágico. Novos estudos de seguimento desta população devem ser realizados para confirmar a hipótese de que as alterações na deglutição observadas ocorreram devido à imaturidade na função de deglutição.PURPOSE: To describe the fluoroscopic findings of swallowing in preterm infants with zero to six months of age, as well as the related diseases and clinical signs and symptoms, and to compare these findings with data obtained from full-term infants. METHODS: The retrospective findings of fluoroscopic studies carried out in infants with zero to six months of age and their respective files were analyzed. Participants were 40 subjects divided into two groups: Preterm Group, composed by 23 preterm infants, and Full-Term Group, with 17 infants born full-term. RESULTS: Nasopharyngeal and gastroesophageal reflux were the main fluoroscopic findings of swallowing in both groups. There was no difference between the groups regarding the presence of swallowing disorders. The Preterm Group presented more cardiac problems than the Full-Term Group. No differences were found between the groups regarding neurologic and respiratory problems. With respect to clinical signs and symptoms suggestive of swallowing disorders, the Preterm Group presented more oxygen desaturation and the Full-Term Group, more vomiting. CONCLUSION: Nasopharyngeal reflux and gastroesophageal reflux were the main fluoroscopic findings of swallowing in preterm infants with zero to six months of age. New follow-up studies with this population must be carried out to confirm the hypothesis that the swallowing alterations observed were due to immaturity in the swallowing function

Reionization Constraints on the Contribution of Primordial Compact Objects to Dark Matter

Many lines of evidence suggest that nonbaryonic dark matter constitutes roughly 30% of the critical closure density, but the composition of this dark matter is unknown. One class of candidates for the dark matter is compact objects formed in the early universe, with typical masses M between 0.1 and 1 solar masses to correspond to the mass scale of objects found with microlensing observing projects. Specific candidates of this type include black holes formed at the epoch of the QCD phase transition, quark stars, and boson stars. Here we show that accretion onto these objects produces substantial ionization in the early universe, with an optical depth to Thomson scattering out to z=1100 of approximately tau=2-4 [f_CO\epsilon_{-1}(M/Msun)]^{1/2} (H_0/65)^{-1}, where \epsilon_{-1} is the accretion efficiency \epsilon\equiv L/{\dot M}c^2 divided by 0.1 and f_CO is the fraction of matter in the compact objects. The current upper limit to the scattering optical depth, based on the anisotropy of the microwave background, is approximately 0.4. Therefore, if accretion onto these objects is relatively efficient, they cannot be the main component of nonbaryonic dark matter.Comment: 12 pages including one figure, uses aaspp4, submitted to Ap

Cutting frequency and height on the quality of Megathyrsus maximus (cv. Gattonpanic)

El estudio que se presenta a continuación tuvo como objetivo evaluar la frecuencia e intensidad de la calidad nutricional en la materia seca (MS) del pasto Megathyrsus maximus (cv. Gatton panic), y fue desarrollado en la Cabaña Doña Anita, provincia del Chaco, Argentina. Se empleó un diseño completamente al azar con un arreglo factorial de 2 alturas de corte (A = 0,15 y 0,30 m), 3 frecuencias (F = 30, 45 y 90 días) y 2 tiempos (T = 90 y 180 días) con cinco repeticiones para cada uno (60 unidades experimentales). Se determinó el porcentaje de MS, proteína bruta (PB), fibra detergente ácido (FDA), fibra detergente neutra (FDN) y digestibilidad (DI). En el caso de la PB, se encontró una interacción entre las variables A x T y F x T. Para la interacción T x A, los cortes realizados en menor tiempo presentaron diferencia significativa (p&nbsp:&lt:&nbsp:0,05) en las dos alturas. Para la interacción T x F en la combinación 90 x 30, hay diferencia significativa (p &lt: 0,05) respecto a las restantes combinaciones. Respecto a la FDN, para la variable altura, el contenido de esta se incrementa al aumentar aquella (p &lt: 0,05) debido a un mayor alargamiento de tallos y hojas. En cuanto a la FDA se observaron diferencias (p &lt: 0,05) entre los valores para la interacción T x A para 180 días con 0,15 y 0,30 m. Para la digestibilidad, se encontraron las diferencias significativas (p &lt: 0,05) en la interacción de T x A. Se concluye que el mayor contenido de proteína bruta se obtuvo con la frecuencia de 30 días. La FDN y la FDA aumentaron con el mayor tiempo y la altura de la pastura

Quantum driven Bounce of the future Universe

It is demonstrated that due to back-reaction of quantum effects, expansion of the universe stops at its maximum and takes a turnaround. Later on, it contracts to a very small size in finite future time. This phenomenon is followed by a " bounce" with re-birth of an exponentially expanding non-singular universe

Revealing the Nature of Dark Energy Using Bayesian Evidence

We apply the Bayesian concept of `evidence' to reveal systematically the nature of dark energy from present and future supernova luminosity distance measurements. We express the unknown dark energy equation of state w(z) as a low order polynomial in redshift and use evidence to find the polynomial order, thereby establishing the minimum order required by the data. We apply this method to the current supernova data, and with a prior -1 < w(z) < 1 and Omega_m = 0.3 \pm 0.05, obtain a large probability of 91% for the cosmological constant model, with the remaining 9% assigned to the two more complex models tested. We also investigate the use of evidence for future supernova data sets such as distances obtainable from surveys like the Supernova Acceleration Probe (SNAP). Given a low uncertainty on the present day matter density we find that, if the underlying dark energy model is only modestly evolving, then a constant $w(z)$ fit is sufficient. However, if the evolution of the dark energy equation of state to linear order is larger than |w_1| ~ 0.5, then the evolution can be established with statistical significance. For models where we can assume the prior -1 < w(z) < 1, the correct polynomial order can be established even for modestly evolving equations of state.Comment: 7 pages, 6 figures, submitted to MNRA

Probing Early Structure Formation with Far-Infrared Background Correlations

The large-scale structure of high-redshift galaxies produces correlated anisotropy in the far-infrared background (FIRB). In regions of the sky where the thermal emission from Galactic dust is well below average, these high-redshift correlations may be the most significant source of angular fluctuation power over a wide range of angular scales, from about 7' to about 3 degrees, and frequencies, from about 400 to about 1000 GHz. The strength of this signal should allow detailed studies of the statistics of the FIRB fluctuations, including the shape of the angular power spectrum at a given frequency and the degree of coherence between FIRB maps at different frequencies. The FIRB correlations depend upon and hence constrain the redshift-dependent spectral energy distributions, number counts, and clustering bias of the galaxies and active nuclei that contribute to the background. We quantify the accuracy to which Planck and a newly proposed balloon-borne mission EDGE could constrain models of the high-redshift universe through the measurement of FIRB fluctuations. We conclude that the average bias of high-redshift galaxies could be measured to an accuracy of less than approximately 1% or, for example, separated into 4 redshift bins with about 10% accuracy.Comment: 15 emulateapj pages, including 9 figures, submitted to Ap

Detectability of Cosmic Topology in Flat Universes

Recent observations seem to indicate that we live in a universe whose spatial sections are nearly or exactly flat. Motivated by this we study the problem of observational detection of the topology of universes with flat spatial sections. We first give a complete description of the diffeomorphic classification of compact flat 3-manifolds, and derive the expressions for the injectivity radii, and for the volume of each class of Euclidean 3-manifolds. There emerges from our calculations the undetectability conditions for each (topological) class of flat universes. To illustrate the detectability of flat topologies we construct toy models by using an assumption by Bernshtein and Shvartsman which permits to establish a relation between topological typical lengths to the dynamics of flat models.Comment: 17 pages, 1 figure, latex2e. New references added. Inserted clarifying points. To appear in Phys. Lett. A (2003) in the present for

Curvature Inspired Cosmological Scenario

Using modified gravity with non-linear terms of curvature, $R^2$ and $R^{(r +2)}$ (with $r$ being the positive real number and $R$ being the scalar curvature), cosmological scenario,beginning at the Planck scale, is obtained. Here, a unified picture of cosmology is obtained from $f(R)-$ gravity. In this scenario, universe begins with power-law inflation, followed by deceleration and acceleration in the late universe as well as possible collapse of the universe in future. It is different from $f(R)-$ dark energy models with non-linear curvature terms assumed as dark energy. Here, dark energy terms are induced by linear as well as non-linear terms of curvature in Friedmann equation being derived from modified gravity.It is also interesting to see that, in this model, dark radiation and dark matter terms emerge spontaneously from the gravitational sector. It is found that dark energy, obtained here, behaves as quintessence in the early universe and phantom in the late universe. Moreover, analogous to brane-tension in brane-gravity inspired Friedmann equation, a tension term $\lambda$ arises here being called as cosmic tension. It is found that, in the late universe, Friedmann equation (obtained here) contains a term $- \rho^2/2\lambda$ ($\rho$ being the phantom energy density) analogous to a similar term in Friedmann equation with loop quantum effects, if $\lambda > 0$ and brane-gravity correction when $\lambda < 0.$Comment: 19 Pages. To appear in Int. J. Thro. Phy