We have learned a lot about freeze dried eggs in the last 5 years. I am doing a reboot on freeze dried eggs with all of the hints and tips we have learned since then to make the perfect freeze dried egg. We show how to rehydrate a freeze dried egg with the rehydration formula. We show how to make the best freeze dried egg powder with no clumping. Freeze dried eggs are eggs that have been processed through a freeze-drying process, which involves removing all the moisture from the eggs. This results in a powdered form of eggs that can be easily reconstituted by adding water. Freeze dried eggs are commonly used by backpackers and hikers due to their lightweight and long shelf life. They are also used by food manufacturers in various products like baking mixes, and by the military for emergency rations. The nutritional value of freeze dried eggs is almost the same as fresh eggs, and they can be used in any recipe that calls for eggs. To get the new hardcopy FREEZE DRYING COOKBOOK, follow this link: https://amzn.to/3hCWa1z Check out the NEW! Freeze Drying Cookbook at: http://www.freezedryingcookbook.com The freeze dryer accessories you see in this, or other videos can be found at: http://www.freezedryingsupplies.com If you are thinking of buying a freeze dryer, support the community & purchase through us! https://affiliates.harvestright.com/416.html It helps keep this YouTube content coming & allows us to do giveaways in our social media groups! If you are interested in purchasing an AVID ARMOR chamber vacuum sealer, check out their site through this link and enter the Coupon Code LIVELIFESIMPLE to get 10% off your purchase! https://www.avidarmor.com/?aff=43 For the Anova Sous Vide that I use: https://amzn.to/3WMGDLI ________________________________________________________________________________________________ The FLIR ONE Pro Thermal Camera I am using can be found at: https://amzn.to/3ErTa0B ________________________________________________________________________________________________ Join the FACEBOOK group (Retired at 40's Freeze Drying Group): https://www.facebook.com/groups/retiredat40livelifesimple ________________________________________________________________________________________________ Join our new MEWE freeze drying group: https://mewe.com/group/5faad29bc033146d6a0ec8ed ________________________________________________________________________________________________ For products I used on this video and love! http://www.amazon.com/shop/retiredat40 ________________________________________________________________________________________________ #freezedriedeggs #freezedriedeggpowder #freezedryingeggs #freezedryingcookbook #freezedryingrecipes

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Some of the most cataclysmic and mysterious events in the cosmos only reveal themselves by their gravitational waves. We’ve detected some of them with our ground-based detectors, but the size of these detectors is limited. The next step forward in gravitational wave (GW) astronomy is a space-based detector: LISA, the Laser Interferometer Space Antenna. When dense objects like black holes and neutron stars orbit each other and merge, they create gravitational waves. These ripples in space-time, which Einstein predicted in 1915, were observed for the first time in 2015 by LIGO (Laser Interferometer Gravitational-Wave Observatory). Now, we’ve observed dozens of them. Ground-based detectors like LIGO have two long “arms” at right angles to each other. A powerful laser beam is split into two identical beams that travel down each arm, or tunnel, that are several kilometres apart. The beams are reflected back and forth by mirrors at the ends of the arms, and when they combine, they interfere with each other. Whenever a GW passes through Earth, it warps spacetime. That makes one arm longer than the other, which changes the interference pattern in the beams. The Laser Interferometer Gravitational-Wave Observatory is made up of two detectors, this one in Livingston, La., and one near Hanford, Wash. The detectors use giant arms in the shape of an “L” to measure tiny ripples in the fabric of the universe. Credit: Caltech/MIT/LIGO Lab The length of the arms limits the sizes of the GWs LIGO can detect and also limits the type of mergers it can detect. It can only detect higher-frequency GWs from 10 to 1,000 Hertz, which come from merging pairs of black holes (BH), merging pairs of neutron stars (NS) and merging mixed pairs of BHs and NSs. LISA will be much different. It doesn’t have the same arm-length limitation. LISA will be the first dedicated space GW observatory, and it will consist of three separate spacecraft arranged in an equilateral triangle. Each spacecraft will be 2.5 million km apart, meaning LISA’s arms will be 2.5 million km long. An artist’s concept of how LISA will work to detect gravitational waves from orbit in space. Courtesy ESA. The ESA/NASA LISA mission is the next step in gravitational wave (GW) astronomy. With its much longer arms, LISA will detect low-frequency waves from 0.1 mHz to 1 Hz and expand our search for GWs and the events that create them. It’ll detect GWs from other sources, like supermassive black hole (SMBH) mergers, binary white dwarf systems, and Extreme Mass Ratio Inspirals (EMRIs). (EMRIs are systems where objects like a stellar-mass black hole or a white dwarf spiral into an SMBH.) Like LIGO, LISA will also be a laser interferometer. Any change in its laser interference pattern can be attributed to a GW. However, LISA will do more than just detect GWs. It can determine other characteristics in the complex GW waveforms, like black hole spin. NASA is busy working on the mission, which isn’t scheduled to launch until 2035. They’ve given us our first look at a full-scale prototype of the six cameras LISA will rely on. “Twin telescopes aboard each spacecraft will both transmit and receive infrared laser beams to track their companions, and NASA is supplying all six of them to the LISA mission,” said Ryan DeRosa, a researcher at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “The prototype, called the Engineering Development Unit Telescope, will guide us as we work toward building the flight hardware.” On May 20, the full-scale Engineering Development Unit Telescope for the LISA (Laser Interferometer Space Antenna) mission, still in its shipping frame, was moved within a clean room at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. They’re made of an amber-coloured glass ceramic called Zerodur that resists changes over a wide range of temperatures. The telescopes also feature a thin layer of gold on their surface. Image Credit: NASA/Dennis Henry The telescopes are made to be stable over a wide temperature range since precision is key to success. They need to detect changes as small as picometers, or trillionths of a meter, between each spacecraft. Unlike LIGO, the three spacecraft that make up the system cannot be kept at precise distances from one another. Over each year’s orbit, the distance between them changes significantly, and the system has to track the changes to guarantee precision. The thin layer of gold is highly reflective in the infrared range that LISA’s lasers will use. It also minimizes thermal absorption and provides consistent reflectivity over long periods of time. Gold also resists corrosion, protects the underlying layer from degradation, and is thermally stable. LISA has another trick up its sleeve: free-floating cubes or test masses. They reflect the lasers back and forth between the spacecraft and are a critical part of its detection system. They’re 46mm solid cubes made of gold-platinum alloy that weigh approximately 2 kg each. The cubes are extremely pure and will have a homogeneous material composition. They’ll float freely inside electrode housings within each spacecraft. The cubes serve as reference points for GW measurement. The ESA and NASA have already tested some of LISA’s components in space. In 2015, the ESA launched the LISA Pathfinder mission. It tested a much smaller version of one of LISA’s arms and also tested the cubes. It placed two test masses in a near-perfect gravitational free-fall and controlled and measured their motion with unprecedented accuracy. This image shows the interior layout of LISA Pathfinder’s science module. The test masses are visible in the centre of the image. Image Credit: ESA/ATG medialab. LICENCE: ESA Standard Licence We’ve come a long way since Einstein predicted gravitational waves. When the first one was detected in 2015, it opened a new window into the cosmos. LISA will throw that window wide open and reveal galaxy-defining events like supermassive black hole mergers. The post NASA is Building Telescopes for the LISA Mission appeared first on Universe Today.

Since the 1960s, astronomers have theorized that the Universe may be filled with a mysterious mass that only interacts with “normal matter” via gravity. This mass, nicknamed Dark Matter (DM), is essential to resolving issues between astronomical observations and General Relativity. In recent years, scientists have considered that DM may be composed of axions, a class of hypothetical elementary particles with low mass within a specific range. First proposed in the 1970s to resolve problems in the Standard Model of particle physics, these particles have emerged as a leading candidate for DM. In addition to growing evidence that this could be the case, researchers at CERN are developing a new telescope that could help the scientific community look for axions – the CERN Axion Solar Telescope (CAST). According to new research conducted by an international team of physicists, these hypothetical particles may occur in large clouds around neutron stars. These axions could be the long-awaited explanation for Dark Matter that cosmologists have spent decades searching for. What’s more, their research indicates that these axions may not be very difficult to observe from Earth. The team was led by Dion Noordhuis, a Ph.D. student with the GRavitational AstroParticle Physics Amsterdam (GRAPPA) Institute, the Institute for Theoretical Physics (ITP), and the Delta Institute for Theoretical Physics at the University of Amsterdam (UvA). He was joined by researchers from Princeton University’s Center for Theoretical Science (PCTS), the University of Barcelona, and the Rudolf Peierls Centre for Theoretical Physics at the University of Oxford. The paper that describes their findings was published on October 17th, 2024, in the journal Physical Review X. Like DM, the existence of axions was postulated to address gaps in our understanding of the behavior of another elementary particle—the neutron. However, also like DM, these hypothetical particles have not yet been detected after decades of investigation. This is understandable since, if such particles exist, they would be extremely light, making them very hard to detect through experiments or astronomical observations. This is why axions are considered a promising candidate to explain DM, which theoretically accounts for 85% of matter in our Universe. While DM is theorized to interact with visible matter via gravity, this does not necessarily mean that it has no other interactions that could be detectable. For example, axions are expected to convert into photons when exposed to electric and magnetic fields, which we can observe. However, the corresponding interaction strength and the amount of light produced should be very small. Therefore, they would likely go unnoticed unless there were an environment containing massive clouds of axions in a very strong electromagnetic field. This led Noordhuis and his team to consider neutron stars since they are the densest class of stars in the Universe and generate very powerful electromagnetic fields. In fact, neutron stars generate magnetic fields that are billions of times stronger than Earth’s magnetosphere. What’s more, astronomers have used supernovae and cooling neutron stars for some time to constrain the properties of axons, including their mass and interactions with other particles. Recent research also supports the idea that their powerful magnetic fields allow neutron stars to produce huge amounts of axions near their surfaces. In a previous study, Noordhuis and his colleagues investigated how axions could escape from a neutron star. This included computing the number of axions produced, which trajectories they would follow, and how their conversion into light could lead to an observable signal. In their latest work, the researchers focused on the axions theoretically captured by a neutron star’s gravity. Due to the very weak nature of their interactions, these particles will likely remain bound to their stars for millions of years. Artist’s impression of an axion cloud around a neutron star. Credit: UvA As they argue in their paper, they would gradually form a hazy cloud around the neutron star that could be visible to telescopes. The team also studied the formation, properties, and evolution of these axion clouds and found that (accounting for a wide range of axion properties) they would likely form around most, or even all, neutron stars. They also calculated that these clouds would be up to twenty orders of magnitude larger than local DM densities, producing powerful observational signatures. These could come in the form of a continuous signal emitted during much of a neutron star’s life or as a one-time burst of light at the end of its life. These signatures would be detectable by current radio telescopes and could be used to probe the interaction between axions and photons. While no axion clouds have been observed yet, the team’s study offers astronomers parameters on what to look for. In addition to searching for axion clouds, this research presents additional opportunities for further theoretical research. This includes follow-up work by one of the study’s co-authors on how the axion clouds can change the dynamics of neutron stars themselves. There’s also the possibility of exploring the numerical modeling of axion clouds to further constrain what and where astronomers should be looking. Finally, the present paper addresses single neutron stars, but there are also possibilities for binaries consisting of two neutron stars and a neutron star with a black hole companion. Taking advantage of next-generation instruments, in addition to current ones, these observations could be a step toward finding the elusive DM particle. These studies could also have applications in other fields of research, such as particle physics, astrophysics, plasma physics, and radio astronomy. In short, this latest study presents opportunities for cross-disciplinary research that could resolve some of the greatest mysteries in astronomy and cosmology today. Further Reading: University of Physics The post White Dwarf Stars May be Shrouded in Extremely Light Particles Called Axions appeared first on Universe Today.

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With the Cable Music Channel, Ted Turner tried to take on MTV and failed—but somehow still managed to win.

A legend. The post Led Zeppelin’s John Paul Jones names the only “perfect” bassist first appeared on Far Out Magazine.