Gsus4

cross-posted from: https://lemmy.world/post/34272214

A California-based biotechnology startup has officially launched the world's first commercially available butter made entirely from carbon dioxide, hydrogen, and oxygen, eliminating the need for traditional agriculture or animal farming. Savor, backed by Microsoft co-founder Bill Gates through his Breakthrough Energy Ventures fund, announced the commercial release of its animal- and plant-free butter after three years of development.

The revolutionary product uses a proprietary thermochemical process that transforms carbon dioxide captured from the air, hydrogen from water, and methane into fat molecules chemically identical to those found in dairy butter. According to the company, the process creates fatty acids by heating these gases under controlled temperature and pressure conditions, then combining them with glycerol to form triglycerides.

I've found so many variations e.g.

soak for 6 hours (minimize fermentation), soak for 3 days (to maximize available nutrients and purge phytic acid);

scrub to remove skins, or don't;

change water...or don't;

blend, boil, strain;

blend, strain, boil;

boil, blend, no straining;

Boil no more than 15 minutes or it will taste like miso paste Vs 20 minutes...Vs longer because beans take a long time to cook

extra condiments or thickeners Vs just sugar.

Sooo...has anyone tried a few of these to tell me which differences to expect?

I was leaning towards soak 24h, scrub skins, boil 15m, blend (my blender is not that strong, so that's why I'm boiling first, add sugar (no straining).

Is there a configuration that is less bitter or closer to nut milk? I'm trying to understand why I am doing things, so that I can control it, otherwise I'm just following random recipes and tweaking with no idea what's happening :P

PS: https://m.youtube.com/watch?v=GWoP0lc-KqY&amp%3Bpp=ygUIc295IG1pbGs%3D added this recipe with the "burnt pan" trick.

https://feddit.nl/comment/2555047

We are familiar with the social "id" through mob dynamics, crowd control. But is there anything akin to the ego and superego for society or groups? Maybe the media act as a bit of a superego on societies...but maybe the concept just does not extend that easily.

Abstract: Large earthquakes occurring worldwide have long been recognized to be non Poisson distributed, so involving some large scale correlation mechanism, which could be internal or external to the Earth. Till now, no statistically significant correlation of the global seismicity with one of the possible mechanisms has been demonstrated yet. In this paper, we analyze 20 years of proton density and velocity data, as recorded by the SOHO satellite, and the worldwide seismicity in the corresponding period, as reported by the ISC-GEM catalogue. We found clear correlation between proton density and the occurrence of large earthquakes (M > 5.6), with a time shift of one day. The significance of such correlation is very high, with probability to be wrong lower than 10–5. The correlation increases with the magnitude threshold of the seismic catalogue. A tentative model explaining such a correlation is also proposed, in terms of the reverse piezoelectric effect induced by the applied electric field related to the proton density. This result opens new perspectives in seismological interpretations, as well as in earthquake forecast.

Abstract: Investigating the early-stage evolution of an erupting flux rope from the Sun is important to understand the mechanisms of how it looses its stability and its space weather impacts. Our aim is to develop an efficient scheme for tracking the early dynamics of erupting solar flux ropes and use the algorithm to analyse its early-stage properties. The algorithm is tested on a data-driven simulation of an eruption that took place in active region AR12473. We investigate the modelled flux rope's footpoint movement and magnetic flux evolution and compare with observational data from the Solar Dynamics Observatory's Atmospheric Imaging Assembly in the 211 Å and 1600 Å channels. To carry out our analysis, we use the time-dependent data-driven magnetofrictional model (TMFM). We also perform another modelling run, where we stop the driving of the TMFM midway through the flux rope's rise through the simulation domain and evolve it instead with a zero-beta magnetohydrodynamic (MHD) approach. The developed algorithm successfully extracts a flux rope and its ascend through the simulation domain. We find that the movement of the modelled flux rope footpoints showcases similar trends in both TMFM and relaxation MHD run: they recede from their respective central location as the eruption progresses and the positive polarity footpoint region exhibits a more dynamic behaviour. The ultraviolet brightenings and extreme ultraviolet dimmings agree well with the models in terms of their dynamics. According to our modelling results, the toroidal magnetic flux in the flux rope first rises and then decreases. In our observational analysis, we capture the descending phase of toroidal flux. In conclusion, the extraction algorithm enables us to effectively study the flux rope's early dynamics and derive some of its key properties such as footpoint movement and toroidal magnetic flux.

Abstract: The solar atmosphere is known to contain many different types of wavelike oscillation. Waves and other fluctuations (e.g., turbulent eddies) are believed to be responsible for at least some of the energy transport and dissipation that heats the corona and accelerates the solar wind. Thus, it is important to understand the behavior of magnetohydrodynamic (MHD) waves as they propagate and evolve in different regions of the Sun’s atmosphere. In this paper, we investigate how MHD waves can affect the overall plasma state when they reflect and refract at sharp, planar interfaces in density. First, we correct an error in a foundational paper (Stein 1971) that affects the calculation of wave energy-flux conservation. Second, we apply this model to reflection-driven MHD turbulence in the solar wind, where the presence of density fluctuations can enhance the generation of inward-propagating Alfven waves. This model reproduces the time-averaged Elsasser imbalance fraction (i.e., ratio of inward to outward Alfvenic power) from several published numerical simulations. Lastly, we model how the complex magnetic field threading the transition region between the chromosphere and corona helps convert a fraction of upward-propagating Alfven waves into fast-mode and slow-mode MHD waves. These magnetosonic waves dissipate in a narrow region around the transition region and produce a sharp peak in the heating rate. This newly found source of heating sometimes exceeds the expected heating rate from Alfvenic turbulence by an order of magnitude. It may explain why some earlier models seemed to require an additional ad-hoc heat source at this location.

Turns out schools of fish hang out around sharks to use their skin as an exfoliator 🤣 and to tag along and save energy.