Podcasts about photochemistry

About the Guest(s): Dr. Kristin Hieshetter is a chiropractor with an extensive background in functional health and integrative medicine. She hosts Functional Health Radio and is known for her innovative approaches using therapies like low-level laser treatment to enhance patient care. Dr. Hieshetter is involved in the Integrative Health Institute, where she educates other healthcare professionals on cutting-edge techniques in functional medicine and neurological treatment. Episode Summary: In this insightful episode of Functional Health Radio, Dr. Kristin Hieshetter shares her experiences with using low-level laser therapy for medical interventions. Having recently encountered a personal family situation, she underscores the potential of these treatments in aiding recovery and fostering faster healing, particularly in the context of her mother's hip surgery. The episode pivots around remarkable treatments Dr. Hieshetter provided using a 7.5 milliwatt low-level laser device, acclaimed for its ability to accelerate healing and reduce infection risks. The discussion further delves into the successful use of low-level laser therapy in a groundbreaking open-heart surgery case involving a 12-year-old boy afflicted with a rare genetic disorder known as BPAN. Dr. Hieshetter shares how the use of this therapy during surgical procedures was facilitated by notable collaboration with renowned cardiac surgeon Dr. Cavarana. This collaboration allowed for the first-ever application of low-level laser therapy in an operating room, evidencing its capacity to safeguard against brain cell death and facilitate extraordinary recovery outcomes. Dr. Hieshetter emphasizes the emerging roles of integrative medicine and the importance of interdisciplinary collaboration in achieving optimal patient health outcomes. Key Takeaways: Low-Level Laser Therapy: This non-invasive treatment helps reduce infection risks, enhance mitochondrial function, and accelerate healing, with successful cases in surgical recoveries. Innovative Surgery Application: Dr. Hieshetter facilitated the first use of low-level laser therapy during a pediatric cardiac surgery, achieving significant positive outcomes by preventing brain cell death. BPAN Genetic Disorder: Highlighted is the impact of this rare condition on brain and tissue function, underscoring the need for advanced integrative treatment options. Interdisciplinary Collaboration: The episode underscores effective cooperation between chiropractors and surgeons, driving medical innovation and enhanced patient care. Advocacy for Integrative Health: Dr. Hieshetter asserts the importance of integrative healthcare solutions, stressing their role in improving the future of patient health management. Notable Quotes: "When you can do something that reduces the risk of infection and speeds healing without any risk or side effect, it's miraculous." "The future of health belongs to the integrators." "This is why my very weak 7.5 milliwatt low-level lasers were able to help my mom." "It's not from heat… Photochemistry became a widely accepted hypothesis to explain the induction of photobiological processes." "We were able to articulate the importance of transcranial low-level laser in brain injury and in TBI and in stroke." Resources: Integrative Health Institute: A professional organization dedicated to teaching functional medicine tools to healthcare providers. Medical University of South Carolina: Location where the groundbreaking surgery took place. Functional Health Mastery Group BPAN Genetic Disorder Information: Insights into the condition discussed within the episode. For a deeper understanding and comprehensive insights into the potential of low-level laser therapy and integrative medicine, tune into the full episode. Functional Health Radio continues to bring you innovative solutions and success stories in the world of functional health. Stay connected for more enlightening content.

References Guerra, DJ.2024. Lecture notes Plant Cell. 2013 Jul; 25(7): 2661–2678 Peer J. 2023; 11: e15696 Gilliland and Massey. 1955. Sid King and the 5 Strings. "Sag, Drag and Fall." https://youtu.be/9KJzeOmHgc4?si=4GjA5H4stZDDl9nT --- Support this podcast: https://podcasters.spotify.com/pod/show/dr-daniel-j-guerra/support

With four seasons under our belt, we've heard some amazing stories about how our guests have found, or often “stumbled” into, their careers in science. We've also had many conversations where past guests have passionately discussed the importance of their early career teachers as well as what teaching does for them in their current careers. This conversation is squarely centered on these two topics, with a good dose of photochemistry mixed in too. We meet Dr. Izzy Lamb, Assistant Professor at Fort Lewis College, which is a small liberal arts school in Colorado with a primarily undergraduate student population. Izzy is entertainingly forthright in admitting that he's often a bit surprised by his success in chemistry given that he was failing the topic in high school and was later accepted to only one of the six graduate programs he applied to. However, our conversation quickly uncovers why Izzy has been successful in what matters most to him—exploring photochemistry and training the next generation of chemists. Join us for this engaging look at how Izzy has built a thriving career in chemistry through perseverance, passion, and knowing what matters most to him. We learn about his career in photocatalysis and how he's now adapting his research to better fit the resources and undergraduate students where he's now working. A passion for teaching students in a way that gets them thinking and equipped to solve real-world problems is his priority, and we learn how he's using a passion for understanding quantum yields of photochemical reactions to help inform more sustainable ways of doing chemistry.Related episodes: Season 1, Ep.2: Reinventing plastics, one reaction at a time Season 3, Ep.1: Fuel the world with light -  the wonders of nano-magnesiumSeason 3, Ep.9: Energy harvesting and self-sustainable greenhousesBonus content!Access bonus content curated by this episode's guest by visiting www.thermofisher.com/chemistry-podcast for links to recent publications, podcasts, books, videos and more.View the video of this episode on www.thermofisher.com/chemistry-podcast.A free thank you gift for our listeners! Visit the episode website and request your free Bringing Chemistry to Life t shirt.Use Podcast Code:  Ba++ery in January 2024 or liV4chem in February We read every email so please share your questions and feedback with us! Email helloBCTL@thermofisher.com About Your HostPaolo Braiuca grew up in the North-East of Italy and holds a PhD in Pharmaceutical Sciences from nearby esteemed University of Trieste, Italy. He developed expertise in biocatalysis during his years of post-doctoral research in Italy and the UK, where he co-founded a startup company. With this new venture, Paolo's career shifted from R&D to business development, taking on roles in commercial, product management, and marketing. He has worked in the specialty chemicals, biotechnology, and pharmaceutical markets in Germany and the UK, where he presently resides. He is currently the Director of Global Market Development in the Laboratory Chemicals Division at Thermo Fisher Scientific™ which put him in the host chair of the Bringing Chemistry to Life podcast. A busy father of four, in what little free time he has, you'll find him inventing electronic devices with the help of his loyal 3D-printer and soldering iron. And if you ask him, he'll call himself a “maker” at heart.

In this podcast episode, MRS Bulletin's Laura Leay interviews Professor Jerry Qi and postdoctoral researcher Mingzhe Li of the Georgia Institute of Technology about their new technique to 3D print silica glass. After using two-photon polymerization to cross-link poly-dimethylsiloxane, Qi's research team used deep UV to convert the polymer into silica glass. The deep UV irradiation is carried out in an oxygen-rich atmosphere. The UV light converts the oxygen to ozone, which then reacts with the polymer, prompting the formation of silica glass. Furthermore, printing of the silica glass is accomplished at the low temperature of 200°C, compared to 1000°C required for current methods of 3D printing. Qi's group fabricated structures of several tens of micrometers in size, with a resolution of a few hundred nanometers. This work was published in a recent issue of Science Advances.

Our look back at the Astrochemical Literature for the month of September 2023, recorded live at the Green Bank Observatory in Green Bank, WV. Your hosts this week are Brett McGuire and Ilsa Cooke.Grab & Go summaries for you this week are on our website: coffee.astrochem.net.Our Double Shot features two more in-depth recaps of papers from this last month:First Glycine Isomer Detected in the Interstellar Medium: Glycolamide (NH2COCH2OH)Rivilla et al. 2023 ApJL 953, L20https://iopscience.iop.org/article/10.3847/2041-8213/ace977Formation of the Methyl Cation by Photochemistry in a Protoplanetary DiskBerné et al. 2023 Nature 621, 56 https://www.nature.com/articles/s41586-023-06307-xWe have an interview with Green Bank Observatory Scientist Will Armentrout about the 20-m telescope on site and how you can use it for science or education.Finally, we take a look back at the first interstellar detection of methanol this month.Check out the ACS Astrocheminar Webseries, restarting this fall (http://astro.phys-acs.org/AstroCheminar.html).Visit Green Bank for a wonderful tourist experience (https://greenbankobservatory.org/visit/) or propose to use their Open Skies telescopes (https://greenbankobservatory.org/science/gbt-observers/proposals/)Special thanks to the Green Bank Observatory Staff this month and to Haley Scolati, for provided a Grab & Go summary of her recently published article. Hosted on Acast. See acast.com/privacy for more information.

People around the globe have protected their skin using a variety of substances throughout history. In the 19th and 20th centuries, deeper understanding of sunlight and the way it affects skin led to more protective sunscreen formulations.  Research: Aldahan AS, Shah VV, Mlacker S, Nouri K. “The History of Sunscreen.” JAMA Dermatol. 2015;151(12):1316. doi:10.1001/jamadermatol.2015.3011 Belmont, Trixie. “Suntans With Pay Off.” The Baltimore Sun. June 13, 1967. https://www.newspapers.com/image/377122417/?terms=%22franz%20greiter%22%20&match=1 Britannica, The Editors of Encyclopaedia. "Johann Wilhelm Ritter". Encyclopedia Britannica, 19 Jan. 2023, https://www.britannica.com/biography/Johann-Wilhelm-Ritter Diffey, B. “Has the sun protection factor had its day?.” BMJ (Clinical research ed.) 320,7228 (2000): 176-7. doi:10.1136/bmj.320.7228.176 Greiter, F. and Gschnait, F. “EFFECT OF UV LIGHT ON HUMANS.” Photochemistry and Photobiology. 1984. 39: 869-873. https://doi.org/10.1111/j.1751-1097.1984.tb08873.x Hodgskiss, Tammy. “What the use of ochre tells us about the capabilities of our African ancestry.” The Conversation. Sept. 7, 2015. https://theconversation.com/what-the-use-of-ochre-tells-us-about-the-capabilities-of-our-african-ancestry-47081 “History of Hamilton.” https://www.hamiltonsunandskin.com.au/history-of-hamilton Leach, Doreen, and Julie Beckwith. “The founders of dermatology: Robert WilIan and Thomas Bateman.” Journal of the Royal College of Physicians of London. Vol. 33, No. 6. November/December 1999. https://www.ncbi.nlm.nih.gov/pmc/articles/PMC9665792/pdf/jrcollphyslond146949-0084.pdf MacEACHERN W.N. and O.F. JILLSON. “A Practical Sunscreen— ‘Red Vet Pet.'” Arch Dermatol. 1964;89(1):147–150. doi:10.1001/archderm.1964.01590250153027 Rathish, Shruthi, and Sebastian Criton. “Robert Willan – A True Pioneer.”  Department of Dermatology, Venereology and Leprosy, Amala Institute of Medical Sciences, Thrissur, Kerala,  April 22, 2019. https://jsstd.org/robert-willan-a-true-pioneer/ Rubin, Penny. “Only on Sun Days.” The Province. January 4, 1975. https://www.newspapers.com/image/501299818/?terms=%22franz%20greiter%22&match=1 “The science of sunscreen.” Harvard Health Publishing.  Feb 15, 2021. https://www.health.harvard.edu/staying-healthy/the-science-of-sunscreen Skin Cancer Foundation. “Ask the Expert: Does a High SPF Protect My Skin Better?”May 1. 2023. https://www.skincancer.org/blog/ask-the-expert-does-a-high-spf-protect-my-skin-better/ “Sunscreen: How to Help Protect Your Skin from the Sun.” FDA. https://www.fda.gov/drugs/understanding-over-counter-medicines/sunscreen-how-help-protect-your-skin-sun#spf “SUNSCREEN IN THE ENVIRONMENT:The History of Sunscreen's Effect on Corals.” Smithsonian Institute Oceans. https://ocean.si.edu/ecosystems/coral-reefs/sunscreen-environment “Sun Tan Free, by the Inch.” The San Francisco Examiner. June 18, 1967. https://www.newspapers.com/image/458648765/?terms=%22franz%20greiter%22&match=1 Svarc, Federico. "A brief illustrated history on sunscreens and sun protection" Pure and Applied Chemistry, vol. 87, no. 9-10, 2015, pp. 929-936. https://doi.org/10.1515/pac-2015-0303 Urbach, Frederick. “The historical aspects of sunscreens.” Journal of Photochemistry and Photobiology B: Biology. Volume 64, Issues 2–3. 2001.Pages 99-104. https://doi.org/10.1016/S1011-1344(01)00202-0. Urbach, F. “Franz Greiter – The Man and His Work.” Photobiology. 1991. https://doi.org/10.1007/978-1-4615-3732-8_82 See omnystudio.com/listener for privacy information.

On April 20, 2010, a drilling rig called Deepwater Horizon exploded, capsizing 36 hours later. Eleven workers were killed and, over the next 87 days, more than 100 million gallons of oil spilled into the Gulf of Mexico in what the EPA has called the largest marine oil spill in history. With public distrust of the companies responsible mounting, scientists had to find a way to study the spill and communicate what they found. So when faced with a crisis of this magnitude, when the stakes are so high, how do you dispel misinformation and effectively communicate what you know? Find links to buy Chris Reddy's book Science Communication in a Crisis: An Insider's Guide here. The Tiny Show & Tell stories are here and here.

The Engines of Our Ingenuity Episode #2604 John Draper's Sister

好久没有上新了，大家有没有想念我们呀！最近AI 的进展实在是太惊人。但是新闻看多了，自然需要有一些来自一线经验深入思考，才能窥见更接近真实的图景。这一期也是Onboard! AI 系列的第三期，接下来还准备了好几期星光熠熠的 AI 专题，请大家关注Onboard！, 不要错过哦！Hello World, who is onboard?这一期，我们将眼界放宽到大语言模型（LLM, Large Language Model）本身能力之外，看看 LLM 周边生态系统，包括硬件和软件工具链，如何随着基础模型的发展，迅速迭代，又相辅相成。嘉宾们来自生成式AI的上下游核心玩家，包括Nvidia, Google Cloud 的生成式AI平台 Vertex AI, 全球最火的AI模型库和社区平台 Huggingface, AI infra 初创公司，聊一聊从他们的视角看到的AI发展的机会，挑战与未来。这一期近2小时的讨论非常硬核，从芯片架构、GPU集群管理，到开发工具，甚至还聊到AI的社会影响，有好几个即兴的精彩话题。术语和英文不少，还请多包涵，在show notes 中尽量为大家做好笔记。话不多说， enjoy! 嘉宾介绍 Jiajia Chen: Senior Product Manager @Nvidia Omniverse, AI infra, Autonomous vehicle data platform; ex-Cisco Han Zhao: Staff software engineer @Google Cloud Vertex AI Tiezhen Wang: Software engineer @Huggingface, ex-Google Tensorflow Ce Gao: Co-founder & CEO @TensorChord, ex-Tencent, Co-chair @Kubeflow 我们都聊了什么 02:12 嘉宾自我介绍, fun fact: 最近看到的有意思的AI产品 06:53 Tiezhen 推荐的自然语言编程工具 Cursor, 嘉宾们激辩编程的未来 13:28 深度碰撞：未来还需要编程吗？ 23:47 Nvidia GTC 2023 上有什么值得关注的新产品？芯片技术的下一代创新在哪里 29:38 各个大厂新出的芯片针对LLM做了哪些优化？ 36:35 管理训练LLM 的大规模GPU集群有哪些挑战？ 47:04 以后我们需要专用的推理芯片吗？ 52:17 开源界有哪些降低LLM训练和部署成本的尝试？LLM 成本下降边界在哪里？ 59:08 LLM 商业生态的未来：开源 vs 闭源？每个企业都需要自己的LLM吗？ 68:50 LLM的发展对于传统的MLOps 工具链各个环节有什么影响？ 78:11 LLM 会带来哪些监管和社会影响？ 90:37 基础模型越来越强大，上层应用和工具如何创造价值？ 100:34 对未来AI发展的期待 我们提到了什么 ChatGPT GitHub Copilot: Your AI pair programmer Cursor: an editor made for programming with AI Tabby: AI Coding Assistant AutoGPT: An experimental open-source attempt to make GPT-4 fully autonomous. HuggingGPT: Solving AI Tasks with ChatGPT and its Friends in HuggingFace NVIDIA cuLitho - Accelerate Computational Lithography NVIDIA H100 GPU NVIDIA NeMo Framework NVIDIA Grace CPU Superchip NVIDIA NVlink: high-speed GPU interconnect Weights & Biases – Developer tools for ML Vicuna: An Open-Source Chatbot Impressing GPT-4 with 90%* ChatGPT Quality Alpaca: A Strong, Replicable Instruction-Following Model 重要名词（感谢 ChatGPT 帮忙！） Large Language Model:大语言模型,指用海量文本训练的语言模型,如GPT-3等。 Foundation Model:基础模型,指一个预训练模型,可以用作下游任务的起点,进行微调和迁移学习。 GPU cluster:GPU集群,多个GPU服务器联网,用来提供高性能的并行计算能力。 Distributed computing: 分布式计算,在多台计算机上协同完成计算任务。 Confidential computing :保密计算,指在不可见和不可获取的方式下处理和分析数据的技术。 Computational lithography: 计算光刻,使用计算方法来精确控制光刻过程,以产生更小更复杂的集成电路。 Electromagnetic Physics:电磁物理学,研究电磁场及其与物质的相互作用。 Photochemistry:光化学,研究光与化学物质相互作用的学科。 Computational geometry:计算几何,研究使用计算机算法解决几何问题的学科。 Topology:拓扑学,研究空间中两个形状或物体之间连续变形的性质。 Stream multiprocessor:流多处理器,GPU中的一种执行单元,包含多个流处理器核心。 Inference:推理,指使用训练好的模型对新数据进行预测和分析的过程。 Model Serving:模型服务,指提供推理API服务,使训练好的模型可以被应用系统调用。 Tensorcore:张量核,NVIDIA GPU中专用于加速机器学习运算的功能单元,如矩阵乘法等。 Vector database:向量数据库,存储和查询高维向量数据的数据库。 参考文章 万字长文，探讨关于ChatGPT的五个最核心问题 OpenAI 联合创始人、首席科学家 Ilya Sutskever 解读大语言模型的底层逻辑与未来边界 NVIDIA GTC 2023 Keynote Product Announcements Nvidia launches new services for training large language models | TechCrunch Large Language Models Get Smarter With Enterprise Data | NVIDIA Blog Jina AI 创始人肖涵博士：揭秘 Auto-GPT 喧嚣背后的残酷真相 欢迎关注M小姐的微信公众号，了解更多中美软件和AI的干货内容！M小姐研习录 (ID: MissMStudy) 大家的点赞、评论、转发是对我们最好的鼓励！如果你有希望我们聊的话题，希望我们邀请的访谈嘉宾，都欢迎在留言中告诉我们哦~

Nitrogen as a Tracer of Giant Planet Formation II : Comprehensive Study of Nitrogen Photochemistry and Implications for Observing NH3 and HCN in Transmission and Emission Spectra by Kazumasa Ohno et al. on Wednesday 30 November Atmospheric nitrogen may provide important constraints on giant planet formation. Following our semi-analytical work (Ohno & Fortney 2022), we further pursue the relation between observable NH3 and an atmosphere's bulk nitrogen abundance by applying the photochemical kinetics model VULCAN across planetary equilibrium temperature, mass, age, eddy diffusion coefficient, atmospheric composition, and stellar spectral type. We confirm that the quenched NH3 abundance coincides with the bulk nitrogen abundance only at sub-Jupiter mass (< 1MJ) planets and old ages (> 1 Gyr) for solar composition atmospheres, highlighting important caveats for inferring atmospheric nitrogen abundances. Our semi-analytical model reproduces the quenched NH3 abundance computed by VULCAN and thus helps to infer the bulk nitrogen abundance from a retrieved NH3 abundance. By computing transmission and emission spectra, we predict that the equilibrium temperature range of 400--1000 K is optimal for detecting NH3 because NH3 depletion by thermochemistry and photochemistry is significant at hotter planets whereas entire spectral features become weak at colder planets. For Jupiter-mass planets around Sun-like stars in this temperature range, NH3 leaves observable signatures of $sim$ 50 ppm at 1.5, 2.1, and 11 $rm {mu}m$ in transmission spectra and > 300--100 ppm at 6 $rm {mu}m$ and 11 $rm {mu}m$ in emission spectra. The photodissociation of NH3 leads HCN to replace NH3 at low pressures. However, the low HCN column densities lead to much weaker absorption features than for NH3. The NH3 features are readily accessible to JWST observations to constrain atmospheric nitrogen abundances, which may open a new avenue to understand the formation processes of giant exoplanets. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16877v1

Nitrogen as a Tracer of Giant Planet Formation II : Comprehensive Study of Nitrogen Photochemistry and Implications for Observing NH3 and HCN in Transmission and Emission Spectra by Kazumasa Ohno et al. on Wednesday 30 November Atmospheric nitrogen may provide important constraints on giant planet formation. Following our semi-analytical work (Ohno & Fortney 2022), we further pursue the relation between observable NH3 and an atmosphere's bulk nitrogen abundance by applying the photochemical kinetics model VULCAN across planetary equilibrium temperature, mass, age, eddy diffusion coefficient, atmospheric composition, and stellar spectral type. We confirm that the quenched NH3 abundance coincides with the bulk nitrogen abundance only at sub-Jupiter mass (< 1MJ) planets and old ages (> 1 Gyr) for solar composition atmospheres, highlighting important caveats for inferring atmospheric nitrogen abundances. Our semi-analytical model reproduces the quenched NH3 abundance computed by VULCAN and thus helps to infer the bulk nitrogen abundance from a retrieved NH3 abundance. By computing transmission and emission spectra, we predict that the equilibrium temperature range of 400--1000 K is optimal for detecting NH3 because NH3 depletion by thermochemistry and photochemistry is significant at hotter planets whereas entire spectral features become weak at colder planets. For Jupiter-mass planets around Sun-like stars in this temperature range, NH3 leaves observable signatures of $sim$ 50 ppm at 1.5, 2.1, and 11 $rm {mu}m$ in transmission spectra and > 300--100 ppm at 6 $rm {mu}m$ and 11 $rm {mu}m$ in emission spectra. The photodissociation of NH3 leads HCN to replace NH3 at low pressures. However, the low HCN column densities lead to much weaker absorption features than for NH3. The NH3 features are readily accessible to JWST observations to constrain atmospheric nitrogen abundances, which may open a new avenue to understand the formation processes of giant exoplanets. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16877v1

Direct Evidence of Photochemistry in an Exoplanet Atmosphere by Shang-Min Tsai et al. on Tuesday 22 November Photochemistry is a fundamental process of planetary atmospheres that is integral to habitability, atmospheric composition and stability, and aerosol formation. However, no unambiguous photochemical products have been detected in exoplanet atmospheres to date. Here we show that photochemically produced sulphur dioxide (SO$_2$) is present in the atmosphere of the hot, giant exoplanet WASP-39b, as constrained by data from the JWST Transiting Exoplanet Early Release Science Program and informed by a suite of photochemical models. We find that SO$_2$ is produced by successive oxidation of sulphur radicals freed when hydrogen sulphide (H$_2$S) is destroyed. The SO$_2$ distribution computed by the photochemical models robustly explains the 4.05 $mu$m spectral feature seen in JWST transmission spectra [Rustamkulov et al.(submitted), Alderson et al.(submitted)] and leads to observable features at ultraviolet and thermal infrared wavelengths not available from the current observations. The sensitivity of the SO$_2$ feature to the enrichment of heavy elements in the atmosphere ("metallicity") suggests that it can be used as a powerful tracer of atmospheric properties, with our results implying a metallicity of $sim$10$times$ solar for WASP-39b. Through providing improved constraints on bulk metallicity and sulphur abundance, the detection of SO$_2$ opens a new avenue for the investigation of giant-planet formation. Our work demonstrates that sulphur photochemistry may be readily observable for exoplanets with super-solar metallicity and equilibrium temperatures $gtrsim$750 K. The confirmation of photochemistry through the agreement between theoretical predictions and observational data is pivotal for further atmospheric characterisation studies. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10490v1

Direct Evidence of Photochemistry in an Exoplanet Atmosphere by Shang-Min Tsai et al. on Tuesday 22 November Photochemistry is a fundamental process of planetary atmospheres that is integral to habitability, atmospheric composition and stability, and aerosol formation. However, no unambiguous photochemical products have been detected in exoplanet atmospheres to date. Here we show that photochemically produced sulphur dioxide (SO$_2$) is present in the atmosphere of the hot, giant exoplanet WASP-39b, as constrained by data from the JWST Transiting Exoplanet Early Release Science Program and informed by a suite of photochemical models. We find that SO$_2$ is produced by successive oxidation of sulphur radicals freed when hydrogen sulphide (H$_2$S) is destroyed. The SO$_2$ distribution computed by the photochemical models robustly explains the 4.05 $mu$m spectral feature seen in JWST transmission spectra [Rustamkulov et al.(submitted), Alderson et al.(submitted)] and leads to observable features at ultraviolet and thermal infrared wavelengths not available from the current observations. The sensitivity of the SO$_2$ feature to the enrichment of heavy elements in the atmosphere ("metallicity") suggests that it can be used as a powerful tracer of atmospheric properties, with our results implying a metallicity of $sim$10$times$ solar for WASP-39b. Through providing improved constraints on bulk metallicity and sulphur abundance, the detection of SO$_2$ opens a new avenue for the investigation of giant-planet formation. Our work demonstrates that sulphur photochemistry may be readily observable for exoplanets with super-solar metallicity and equilibrium temperatures $gtrsim$750 K. The confirmation of photochemistry through the agreement between theoretical predictions and observational data is pivotal for further atmospheric characterisation studies. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10490v1

Direct Evidence of Photochemistry in an Exoplanet Atmosphere by Shang-Min Tsai et al. on Monday 21 November Photochemistry is a fundamental process of planetary atmospheres that is integral to habitability, atmospheric composition and stability, and aerosol formation. However, no unambiguous photochemical products have been detected in exoplanet atmospheres to date. Here we show that photochemically produced sulphur dioxide (SO$_2$) is present in the atmosphere of the hot, giant exoplanet WASP-39b, as constrained by data from the JWST Transiting Exoplanet Early Release Science Program and informed by a suite of photochemical models. We find that SO$_2$ is produced by successive oxidation of sulphur radicals freed when hydrogen sulphide (H$_2$S) is destroyed. The SO$_2$ distribution computed by the photochemical models robustly explains the 4.05 $mu$m spectral feature seen in JWST transmission spectra [Rustamkulov et al.(submitted), Alderson et al.(submitted)] and leads to observable features at ultraviolet and thermal infrared wavelengths not available from the current observations. The sensitivity of the SO$_2$ feature to the enrichment of heavy elements in the atmosphere ("metallicity") suggests that it can be used as a powerful tracer of atmospheric properties, with our results implying a metallicity of $sim$10$times$ solar for WASP-39b. Through providing improved constraints on bulk metallicity and sulphur abundance, the detection of SO$_2$ opens a new avenue for the investigation of giant-planet formation. Our work demonstrates that sulphur photochemistry may be readily observable for exoplanets with super-solar metallicity and equilibrium temperatures $gtrsim$750 K. The confirmation of photochemistry through the agreement between theoretical predictions and observational data is pivotal for further atmospheric characterisation studies. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10490v1

Direct Evidence of Photochemistry in an Exoplanet Atmosphere by Shang-Min Tsai et al. on Monday 21 November Photochemistry is a fundamental process of planetary atmospheres that is integral to habitability, atmospheric composition and stability, and aerosol formation. However, no unambiguous photochemical products have been detected in exoplanet atmospheres to date. Here we show that photochemically produced sulphur dioxide (SO$_2$) is present in the atmosphere of the hot, giant exoplanet WASP-39b, as constrained by data from the JWST Transiting Exoplanet Early Release Science Program and informed by a suite of photochemical models. We find that SO$_2$ is produced by successive oxidation of sulphur radicals freed when hydrogen sulphide (H$_2$S) is destroyed. The SO$_2$ distribution computed by the photochemical models robustly explains the 4.05 $mu$m spectral feature seen in JWST transmission spectra [Rustamkulov et al.(submitted), Alderson et al.(submitted)] and leads to observable features at ultraviolet and thermal infrared wavelengths not available from the current observations. The sensitivity of the SO$_2$ feature to the enrichment of heavy elements in the atmosphere ("metallicity") suggests that it can be used as a powerful tracer of atmospheric properties, with our results implying a metallicity of $sim$10$times$ solar for WASP-39b. Through providing improved constraints on bulk metallicity and sulphur abundance, the detection of SO$_2$ opens a new avenue for the investigation of giant-planet formation. Our work demonstrates that sulphur photochemistry may be readily observable for exoplanets with super-solar metallicity and equilibrium temperatures $gtrsim$750 K. The confirmation of photochemistry through the agreement between theoretical predictions and observational data is pivotal for further atmospheric characterisation studies. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10490v1

If you're not familiar with some of the terms used in this discussion – some key ones are described here for your reference:Bio-inorganic chemistry – the study of the role of metals in biological processes. This includes naturally occurring molecules and artificially introduced proteins.Metal center (active site) – the active metal in a larger molecule that reacts in (or catalyzes) a reactionCatalysis – increasing the rate of a reaction by introducing a substance to the reaction know as a catalyst. Catalysts are not consumed in the reaction.Functionalization of Carbon-Hydrogen bonds – converting a (Carbon-Hydrogen) C-H bond to a C-R bond. R represents a functional group that enables the final molecule to perform a specific reaction.Activation of Carbon-Hydrogen bonds – Reading (or breaking) the C-H bond so that the desired functional group can replace the Hydrogen.Enzyme – An organic catalyst, often found in nature and active in living cells. Enzymes are typically protein molecules.Organic molecule/organic substrate – A compound containing Carbon.Hydrogen bonding – An electrostatic force of interaction between a Hydrogen atom and another electronegative atom. The most common Hydrogen bonds occur between Hydrogen and either Nitrogen, Oxygen, or Fluorine.Reoxidize (oxidize) – during a reaction, a catalyst may accept electrons from the primary reactants or otherwise become reduced. Removing those electrons, or otherwise oxidizing the catalyst enables it to once more catalyze the reaction.Stoichiometric amount – Calculating the number of molecules (usually in moles) required for a given reaction.Photochemistry – Chemical reactions which are influenced by the presence or absence of light, often at specific wavelengths. Photochemistry is used to closely control reactions – i.e. the reaction will not take place if the correct light isn't present.Motif – A specific part of a molecule – often found in a number of molecules. Prof Maiti is contactable on social media, and you can find him on LinkedIn at https://www.linkedin.com/in/debabrata-maiti-54ab622a/ Our theme music is "Wholesome" by Kevin MacLeod (https://incompetech.com)Music from https://filmmusic.ioLicense: CC BY (http://creativecommons.org/licenses/by/4.0/) Connect with me (Paul) at https://www.linkedin.com/in/paulorange/H.E.L. group can be found at www.helgroup.com online,on LinkedIn at https://www.linkedin.com/company/hel-group/ on Twitter, we're @hel_group, https://twitter.com/hel_groupor search for us on Facebook 

Photochemistry and Heating Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations by Jeong-Gyu Kim et al. on Monday 17 October We present an efficient heating/cooling method coupled with chemistry and ultraviolet (UV) radiative transfer, which can be applied to numerical simulations of the interstellar medium (ISM). We follow the time-dependent evolution of hydrogen species (H$_2$, H, H$^+$), assume carbon/oxygen species (C, C$^+$, CO, O, and O$^+$) are in formation-destruction balance given the non-steady hydrogen abundances, and include essential heating/cooling processes needed to capture thermodynamics of all ISM phases. UV radiation from discrete point sources and the diffuse background is followed through adaptive ray tracing and a six-ray approximation, respectively, allowing for H$_2$ self-shielding; cosmic ray (CR) heating and ionization are also included. To validate our methods and demonstrate their application for a range of density, metallicity, and radiation field, we conduct a series of tests, including the equilibrium curves of thermal pressure vs. density, the chemical and thermal structure in photo-dissociation regions, H I-to-H$_2$ transitions, and the expansion of H II regions and radiative supernova remnants. Careful treatment of photochemistry and CR ionization is essential for many aspects of ISM physics, including identifying the thermal pressure at which cold and warm neutral phases co-exist. We caution that many current heating and cooling treatments used in galaxy formation simulations do not reproduce the correct thermal pressure and ionization fraction in the neutral ISM. Our new model is implemented in the MHD code Athena and incorporated in the TIGRESS simulation framework, for use in studying the star-forming ISM in a wide range of environments. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08024v1

ABOUT TODAY's EPISODE Following up from last week's episode on the hair cuticle, today's episode focuses on all we can do to preserve the cuticle. If you want to see inches, and you have not been paying attention to the hair cuticle, then this episode is for you. I discuss why the cuticle is important, what is causes damage and steps we can take to preserve it, as long as possible. Cuticle damage will lead to exposure of the hair cortex, leading to split ends and we do not want that! Enjoy and make sure you apply the knowledge. SUPPORT! Thank you SO much for your constant support. It means the world to me. If you are wondering how you can support, please see below Share share share to the ends of the world: You can share this podcast to as many people as you know and love. You does not love a fun podcast about hair and skin? See links for that here https://linktr.ee/ChiomaAgha Support financially: https://anchor.fm/chioma-agha Download: Do you know that you can download any episode? Take me (well my voice, LOL) anywhere you are. Just click on download, and voila! Listen: Errmmm listen listen and listen again. You can listen one zillion uncountable billion times. LOL. Listen to the Ads ooooooo. T for Tenks REFERENCES 1. Takahashi, Mamada, Kiwaza et al. "Age dependent damage for hair cuticle: contribution of S100A3 protein and its citrullination". Journal of cosmetic dermatology. 2015 2. BIRBECK, M S, and E H MERCER. “The electron microscopy of the human hair follicle. II. The hair cuticle.” The Journal of biophysical and biochemical cytology vol. 3,2 (1957): 215-22. doi:10.1083/jcb.3.2.215 3. M. Richena, C.A. Rezende. "Morphological degradation of human hair cuticle due to simulated sunlight irradiation and washing". Journal of Photochemistry and Photobiology B: Biology, Volume 161, 2016, Pages 430-440, ISSN 1011-1344. 4. Robbins, C.R. (2012) Chemical and Physical Behavior of Human Hair. 5th Edition. Disclaimer The information provided on this podcast, including but not limited to, text, graphics, are for informational purposes only and does not serve as a diagnosis, treatment or substitute for medical advice. Always seek the advice of a qualified health care professional for any medical condition you may be experiencing. --- This episode is sponsored by · Anchor: The easiest way to make a podcast. https://anchor.fm/app Support this podcast: https://anchor.fm/chioma-agha/support

On today's ID the Future, Miracle of Man author and biologist Michael Denton continues his conversation with host Eric Anderson. Here Denton does a rapid flyover of several more anthropic “coincidences” in chemistry, biochemistry, and Earth science that are fine tuned to allow air-breathing, bipedal, technology-developing terrestrial creatures like ourselves to exist and thrive. The fine tuning, what Denton calls anthropic prior fitness, would seem to require foresight and planning on literally a cosmic scale. The wide-ranging conversation, the final one in a four-part series, gives a flavor for the breadth—if not the depth and richness—of Denton's new book from Discovery Institute Press, available here. Source

Welcome back! Todays ep:Catch ups so long it's basically the whole podSober Bonnie and Averill butchering the pronunciation of several wordsA lil jellyfish ✨background✨ and life cycle Immortal jellyfish?Do jellies sleepGreen fluorescent protein!!Sources for the nerds:Life cyclesRebecca Helm Lab Blog -https://jellybiologist.comImmortalityL. Martell, S. Piraino, C. Gravili & F. Boero (2016) Life cycle, morphology and medusa ontogenesis of Turritopsis dohrnii (Cnidaria: Hydrozoa), Italian Journal of Zoology, 83:3, 390-399SleepNath, R. D., Bedbrook, C. N., Abrams, M. J., Basinger, T., Bois, J. S., Prober, D. A., Sternberg, P. W., Gradinaru, V., & Goentoro, L. (2017). The jellyfish cassiopea exhibits a sleep-like state. Current Biology, 27(19), 2984-2990GFPChalfie, M. (1995), GREEN FLUORESCENT PROTEIN. Photochemistry and Photobiology, 62: 651-656.As always, we welcome any and all thoughts:Instagram: @soundsscientificTwitter: @soundscientific*views are our own and not the opinions of our employers or institutionWe are a tiny podcast so do your act of kindness for the day and click those like/subscribe/follow/share buttons *views are our own and not the opinions of our employers or institution*

Laws of photochemistry, luminescence,radiative transition

Laws of photochemistry, luminescence,radiative transition

Why does light cause tattoos to fade? John Swierk, Asst. Professor of Chemistry at Binghampton University is currently investigating the composition of commercial tattoo inks as well as the underlying photochemistry to understand how light causes tattoos to change and what underlying risks to human health those changes might generate.  Information about commercial tattoo ink compositions can be found at www.whatsinmyink.com. * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * Watch on www.ReinventingTheTattoo.com or join us on our FREE mobile app. Android: https://www.youtube.com/redirect?event=video_description&redir_token=QUFFLUhqbk5sY2dXQmpPdVh3NWp0Tl93UzM0TVJhYWFqZ3xBQ3Jtc0ttLTc0SmRPUVNKQURRdnN5QUJUSW03VmctaW4tOFdyNGZQendPOHd3RDJta1RJdllNaFRXMmU2X3FYZjlGbzRQUWpBRWticDhhWWVjTS1qNTVIR193a0ZLR1NGV3NjZ3Fua1RkaDA4Ykk5dm5ndl8yRQ&q=https%3A%2F%2Frb.gy%2Fid9ppf (https://rb.gy/id9ppf)​ IOS: https://www.youtube.com/redirect?event=video_description&redir_token=QUFFLUhqbHZhVXlFbkZhSllyQnpzcDdYMnVPQjJqd0E4UXxBQ3Jtc0ttVC1jaHMxR21RM2x6aUhMdXVFWmlyRTVvRnpDc0UzdGZrSF9qYzhmNERuWm1oM3Z5ZkYybmNVS2FtQmJKQzdPMG96Mjh1aV9GTkRNMHU1bmUyQUk1Z2NoTGNLOE9TWW1leG9WNDNKLU9WaEFmcGp6VQ&q=https%3A%2F%2Frb.gy%2Fkz9uvs%C2%A0 (https://rb.gy/kz9uvs )​

Referencer1)Hamblin, 2018, Photochemistry and photobiology2)Gendron et Hamblin, 2019, Photobiomodulation, photomedicine and laser surgery3)Da Silva et al, 2018, Lasers in medical science4)De Paica et al, 2016, Lasers in medical science5)De Marchi et al, 2017, Lasers in medical science6)Pinto et al, 2016, Journal of strength and conditioning research,7)Dornelles et al, 2019, Lasers in medical science8)Tomazoni et al, 2019, Oxidative Medicine and Cellular Longevity9)Larkin-Kaiser et al, 2015, Journal of athletic training10) Malta et al, 2019, Frontiers in physiology11) Vanin et al, 2016, Photomedicine and laser surgery12) Vanin et al, 2016, Lasers in medical science13) Miranda et al, 2018, Lasers in medical science14) Langella et al, 2018, Lasers in medical science15) Baltzer et al, 2016, Lasers in surgery and medicine16) Gomes et al, 2018, Lasers in surgery and medicine17) Vassao et al 2019, Lasers in medical therapy

Mary Niedrauer is a new PhD from Purdue University. She does her research in Synthetic Organic Chemistry, Medicinal Chemistry, Photochemistry, and Peptide Synthesis. She also obtain her MBA during her time at Purdue. A US Army vet and Jiu Jitsu practitioner. --- This episode is sponsored by · Anchor: The easiest way to make a podcast. https://anchor.fm/app Support this podcast: https://anchor.fm/idris-sunmola/support

Mr. Darius Dinshah, author of Let There Be Light joins Dr. Elaina George for this week’s episode of Living in the Solution to discuss Spectro-Chrome Color Therapy, a modality that has been present since 1897. It uses the electromagnetic energy from visible light to restore cellular balance and support health. Spectro-Chrome and light therapies are garnering renewed interest as potentially beneficial in treating patients with COVID-19. As such, one  study recently published in the Journal of Photochemistry and Photobiology on May 1, 2020 highlights this potentiality and is available for review on the National Center for Biotechnology Information under the heading, “Light as a potential treatment for pandemic coronavirus infections: A perspective.” Dinshah Health Society – Spectro-Chrome System, is the preeminent spectrum-based health system. Spectro-Chrome therapy is a safe, natural, inexpensive home-use medical system that does not rely on any drugs or chemicals, with their uncertain side effects. This system has been in use since 1920, and was used in a major medical center in Philadelphia, PA for many years.This system utilizes safe, specific colored light for particular problems with a simple, low-powered lamp and color filters. [Dinshah Health Society Website]

The photochemical activities of phycoerythrocyanin α-subunits from Mastigocladus laminosus separated by isoelectric focusing were tested by irradiating at 500, 550, 577 and 600 nm. Two types of photoreversible photochromic responses have been characterized by absorption and absorption difference spectroscopy. Type I is the well-known absorption shift from 571 to 506 nm. Type II is a new response characterized by a line-broadening of the 570 nm absorption.

Tue, 1 Jan 1991 12:00:00 +0100 http://epub.ub.uni-muenchen.de/2346/ http://epub.ub.uni-muenchen.de/2346/1/2346.pdf Scheer, Hugo Scheer, Hugo (1991): Photochemistry and photophysics of biliprotein chromophores. A case of molecular ecology. In: Riklis, Emanuel (Hrsg.), Photobiology. The science and its applications. Plenum Press: New York u.a., pp. 491-495. Biologie

Mon, 1 Jan 1990 12:00:00 +0100 http://epub.ub.uni-muenchen.de/2327/ http://epub.ub.uni-muenchen.de/2327/1/2327.pdf Siebzehnrübl, S.; Lipp, G.; Fischer, R.; Scheer, Hugo Siebzehnrübl, S.; Lipp, G.; Fischer, R. und Scheer, Hugo (1990): The reversible photochemistry of phycorythrocyanin. In: Baltschewsky, M. (Hrsg.), Current research in photosynthesis. Bd. 4, Kluwer: Dordrecht u.a., pp. 421-424. Biologie

Wed, 1 Feb 1989 12:00:00 +0100 http://epub.ub.uni-muenchen.de/2303/ http://epub.ub.uni-muenchen.de/2303/1/160.pdf Scheer, Hugo Scheer, Hugo (Februar 1989): How does the electron get to the other side? The 1988 Nobel prize in Chemistry. In: Journal of Photochemistry and Photobiology B: Biology, Vol. 3, Nr. 1: v-vii. Biologie

Native PEC from the cyanobacterium, Mastigocladus laminosus, and its isolated α-subunit show photoreversibly photochromic reactions with difference-maxima around 502 and 570 nm in the spectral region of the α-84 phycoviolobilin chromophore. (b) Native PEC and its β-subunit show little if any reversible photochemistry in the 600–620 nm region, where the phycocyanobilin chromophores on the β-subunit absorb maximally, (c) Reversible photochemistry is retained in ureadenatured PEC at pH = 7.0 or pH ≤ 3. The difference maxima are shifted to 510 and 600 nm, and the amplitudes are decreased. An irreversible absorbance increase occurs around 670 nm (pH ≤ 3). (d) The amplitude of the reversible photoreaction difference spectrum is maximum in the presence of 4–5 M urea or 1 M KSCN, conditions known to dissociate phycobiliprotein aggregates into monomers. At the same time, the phycocyanobilin chromophore(s) are bleached irreversibly, (e) The amplitude becomes very small in high aggregates, e.g. in phycobilisomes. (f) In a reciprocal manner, the phototransformation of native PEC leads to a reversible shift of its aggregation equilibrium between trimer and monomer. The latter is favored by orange, the former by green light, (g) It is concluded that the phycoviolobilin chromophore of PEC is responsible for reversible photochemistry in PEC, and that there is not only an influence of aggregation state on photochemistry, but also vice versa an effect of the status of the chromophore on aggregation state. This could constitute a primary signal in the putative function as sensory pigment, either directly, or indirectly via the release of other polypeptides, via photodynamic effects, or the like.

Highly frequency selective photochemistry at cryogenic temperatures is used to gain information on the excited state dynamics of large biomolecular aggregates, the phycobilisomes from the blue–green alga (cyanobacterium) Masticogladus laminosus. In particular, we show that in spite of the well organized structure of these aggregates disorder on a microscopic level dominates the optical spectra. The hole burning reaction in the resonantly excited chromophores is most probably due to a conformational change in the neighborhood of the chromophore. From the widths of the holes energy transfer times between different pigments on the order of 16 ps are determined. These transfer times are independent of the excitation energy. The Journal of Chemical Physics is copyrighted by The American Institute of Physics.

Thu, 1 Jan 1987 12:00:00 +0100 http://epub.ub.uni-muenchen.de/2222/ http://epub.ub.uni-muenchen.de/2222/1/2222.pdf Scheer, Hugo Biggins, J. (Hrsg.) (1987): Photochemistry and photophysics of C-phycocyanin. VIIth International Congress on Photosynthesis, 10. - 15. August 1986, Providence, Rhode Island, USA. Biologie

Sat, 1 Jan 1983 12:00:00 +0100 http://epub.ub.uni-muenchen.de/2907/ http://epub.ub.uni-muenchen.de/2907/1/2907.pdf Lubitz, Wolfgang; Lendzian, F.; Scheer, Hugo; Plato, M.; Möbius, K. Zewail, A. H. (Hrsg.) (1983): Electron-nuclear multiple resonance studies on primary products of bacterial photosynthesis. International Conference on Photochemistry and Photobiology , Jan. 5 - 10, 1983, Alexandria.