Podcasts about granulation

David Huycke is an internationally renowned Belgian silversmith, best known for his innovative approach to metalwork, specifically the use of granulation techniques in larger sculptural silverware. In this episode, Huycke discusses his creative process, sources of inspiration, and how he approaches testing and developing new techniques and methods. •Click here for video, show notes, links, and other resources. •Learn more about MJSA

Michael Malice joins the show to talk about his new book, "Simmer: A Novel." Lexman and Malice discuss the cementite in simmer, the arhythmia in the novel, and the invariants of the story. They also discuss the sestets and granulation of the novel.

Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO by S. Sulis et al. on Tuesday 29 November Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. In this study, we aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. For the first time, we observed two bright stars (Teff = 5833 K and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise dependent variations. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14398v1

Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO by S. Sulis et al. on Monday 28 November Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. In this study, we aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. For the first time, we observed two bright stars (Teff = 5833 K and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise dependent variations. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.14398v1

This postpartum series is in partnership with Ergobaby. Check out their baby carriers at ergobaby.com. Know Your Options Online Childbirth Course Use code 100OFF for $100 off enrollment Beyond the First Latch Course (comes free with KYO course) Support The Birth Hour via Patreon!

What is improv, if not breaking apart something into little pieces of material? Please, don't reflect on that sentence, it makes less sense the longer you thing about it. The theme is "granulation", and we go from a hostile intern takeover of the sugar factory to a behind-the-scenes look at acclaimed actor Hayden Christenson's award-winning performance as Anakin Skywalker. Enjoy the whole episode in one go or listen to three-second segments once daily over the course of the year.

A conversation with artist, craftsman, researcher and educator Dr David Huycke on his innovative work with granulation and metal. An insight into the considered practice of an artist balancing craft, poetry and profession.

An Organic PioneerMark Nuzum is a pioneer in the organic fertilizer business and has been our business partner here at EarthWorks for over 25 years. Mark and I talk about what goes on to get a quality organic fertilizer into a bag so that you can easily spread it on your property. It is not as easy as you think but a fascinating conversation.

It's time for some hygroscopic science in today's Pressing Questions segment! Then we visit our old friends the pet pals of Pleasantville in our Wildcard segment.

Neerav wanted to know why some things dissolve faster than others, so we spoke to University of Cambridge chemist Ljiljana Fruk to find out... Like this podcast? Please help us by supporting the Naked Scientists

déc 2006 - SR remix Des pastilles en morceaux devenues poudre. Granulation de micro-éléments, grainons féconds de futures masses, gouttelettes, maillons de futures vagues. - Réalisation et mix : Rodolphe Alexis A télécharger sur http://www.silenceradio.org/grid.php?sound=118

Healing and repair go hand-in-hand. Healing can be defined as process of restoration to normal structure and function. Repair is defined as to remedy, replace or heal as in a wound or a lost part. Join this discussion on Healing and repair and let's talk about it..Topics: - Process of Healing - Cell Types- Repair by C.T.- Granulation of Tissue- Phases of tissue healing- Normal Wound Healing- Factors Affecting Healing- Diabetic Gangrene- Gas Gangrene- Bone FracturesReference: Pathology Review (3rd Edition) J.R. La Rose

This week we learn about using emotional granulation to help us cope with life a little better. Do you want to be happier? Listen today and learn a simple trick that can help you deal with your emotions and become calmer and happier.

In kühlen Sternen wie der Sonne wird die nuklear erzeugte Energie aus dem Inneren an die Oberfläche transportiert. Diese kann dann in den freien Weltraum entfliehen, und so können wir das Sternenlicht letztlich beobachten. Die theoretische Modellierung des photosphärischen Übergangsbereiches – vom konvektiven zum radiativen Energietransport – ist aufgrund der inhärenten dreidimensionalen (3D) Natur der Konvektion und der komplexen, nicht-linearen und nicht-lokalen Interaktionen des Strahlungsfelds mit dem stellaren Plasma sehr anspruchsvoll. Theoretische Atmosphärenmodelle stellen die fundamentale Basis für die Untersuchung von Sternen dar, daher sind Astronomen für ihr Verständnis der Sterne auf diese letztlich angewiesen. Die üblicherweise verwendeten eindimensionalen (1D) Atmosphärenmodelle beinhalten verschiedene Vereinfachungen. Insbesondere wird die Konvektion für gewöhnlich mit der Mischungswegtheorie berechnet, trotz ihrer wohlbekannten Fehler, da derzeit keine deutlich besseren Alternativen vorhanden sind. Der einzige Ausweg, um dieses Problem zu überwinden ist, die zeitabhängigen, dreidimensionalen, hydrodynamischen Gleichungen, welche mit einem realistischen Strahlungstransport gekoppelt sind, zu lösen. Aufgrund der in den vergangenen Jahrzehnten rasch gestiegenen Rechenleistung wurden bedeutende Fortschritte mit Simulationen für 3D Strahlungshydrodynamik (RHD) von Atmosphären erzielt. Diese Modelle sind außerordentlich leistungsfähig, und besitzen eine enorme Vorhersagekraft, wie präzise Vergleiche mit Sonnenbeobachtungen wiederholt beweisen konnten. Ausgestattet mit diesen ausgereiften Methoden möchte ich als Ziel meiner Dissertation die drei folgenden Fragen näher untersuchen: Was sind die Eigenschaften der Atmosphären von kühlen Sternen? Welche Unterschiede sind zwischen den 1D und 3D Modellen vorhanden? Wie verändern sich die Vorhersagen für die Sternstrukturen und Spektrallinien? Um mich dieser Aufgabenstellung systematisch anzunehmen, habe ich das Stagger-Gitter berechnet. Das Stagger-Gitter ist ein umfangreiches Gitter aus 3D RHD Atmosphärenmodellen von kühlen Sternen, welches einen großen stellaren Parameterbereich abdeckt. In der vorliegenden Dissertation beschreibe ich die Methoden, welche angewendet wurden, um die vielen Atmosphärenmodelle zu berechnen. Zudem werden die allgemeinen Eigenschaften der resultierenden 3D Modelle, auch deren zeitliche und räumliche Mittelwerte detailliert dargestellt und diskutiert. Die Unterschiede zwischen den 1D und 3D Schichtungen, sowie die Details der stellaren Granulation (die Manifestation der Konvektion unterhalb der Sternoberfläche) werden ebenfalls umfangreich erläutert und beschrieben. Des Weiteren habe ich folgende Anwendungen für die 3D Atmosphärenmodelle untersucht: Berechnung theoretischer Spektrallinien, wichtig für die Bestimmung von Sternparametern, Spektroskopie und Häufigkeiten-Analyse; die sogenannte Randverdunkelung, notwendig für die Analyse interferometrischer Beobachtungen und Suche nach extrasolaren Planeten; und die Kalibrierung der Mischungsweglänge, womit 1D-Sternmodelle verbessert werden können. Die Qualität der hochauflösenden Beobachtungen hat inzwischen die der theoretischen 1D Atmosphärenmodelle aufgrund der technischen Entwicklungen in den vergangenen Jahren überschritten. Daher hat sich der Bedarf an besseren Simulationen für Atmosphärenmodelle erhöht. Durch die Bereitstellung eines umfangreichen Gitters aus 3D RHD Atmosphärenmodellen wurde dazu ein erheblicher Beitrag geleistet. Damit werden wir den Anforderungen an die Theorie für die derzeitigen und zukünftigen Beobachtungen gerecht werden, und können somit zu einem besseren Verständnis der kühlen Sterne beitragen.

How do wounds heal? What stitch would you use to close a wound and why? When would you not close a wound? What do you do when a wound looks infected? Seem like easy questions but would you be able to answer them?? In the first of a series of podcasts on plastic surgery, Benjamin Baker talks to Jill Arrowsmith about aspects of wound healing. Types of wounds healing are discussed. Primary closure, delayed primary closure healing by secondary intention are explained as well as granulation tissue, types of suture and what suture to use and why. How wounds heal is explained as well as hypertrophic scars and keloid formation. How to recognise and manage wound infection is also covered in this podcast. Mapped to medical finals and ISCP curriculum this podcast is essential listening for medical students and trainees in surgery. Benjamin Baker is an Academic Foundation Doctor at the University of Nottingham, Royal Derby Hospital. Jill Arrowsmith is a Consultant Plastic and Reconstructive Surgeon at the renowned Pulvertaft Hand Centre, Royal Derby Hospital, UK

Transcript -- Scientists investigate sun spots, solar flares and arcs using x-ray telescopes, featuring the Big Bear Observatory in LA.

Scientists investigate sun spots, solar flares and arcs using x-ray telescopes, featuring the Big Bear Observatory in LA.

Transcript -- Scientists investigate sun spots, solar flares and arcs using x-ray telescopes, featuring the Big Bear Observatory in LA.

Scientists investigate sun spots, solar flares and arcs using x-ray telescopes, featuring the Big Bear Observatory in LA.

Human skin wounds (66) inflicted between 20 h and 7 months prior to biopsy were studied. In order to identify the type of cellular differentiation of the fibroblastic cells in the granulation tissue, alpha-smooth muscle actin and desmin were immunohistochemically localized. The value of any presumed time-dependent appearance and/or disappearance of positively stained cells was tested for the estimation of wound age. In skin specimens with a wound age less than 5 days (n =15) no typical granulation tissue had developed and no alpha-actin-positive myofibroblasts could be detected. The first appearance of positively reacting myofibroblasts was noted in a 5-day-old wound. In 57% of the lesions with a wound age between 5 and 31 days (25 out of 44 cases) typical granulation tissue formation was present and myofibroblasts with positive reaction for alpha-smooth muscle actin could be identified. Numerous positively reacting cells could generally be found in wounds aged between 16 and 31 days, but also in wounds less than 16 days old. In 29% of the cases with a wound age of more than 31 days (2 out of 7 cases) alpha-sma-positive myofibroblasts also occured. Fibroblastic cells positive for desmin could not be seen at all in our series. Our results demonstrate the appearance of alpha-sma-positive myofibroblasts with the initial formation of typical granulation tissue in human skin lesions as early as approximately 5 days after wounding. In contrast to recent experimental results these cells remained detectable in wounds aged more than 2 months in some cases. The immunohistochemical detection of actin-positive cells, therefore, demonstrates whether an unknown skin wound is aged approximately 5 days or more. Even though a time-dependent decrease of myofibroblasts in human granulation tissue after 31 days in human wounds seems probable, the extended presence (up to about 2 months) of these cells allows no further exact age determination of older wounds.