Lifeboat Foundation

NASA is working with private industry partners and small businesses under Artemis to produce scalable, affordable, and advanced laser communications systems that could enable greater exploration and discovery beyond Earth for the benefit of all.

Laser, or optical, communications provide missions with increased data rates – meaning that missions using laser technology can send and receive more information in a single transmission compared with those using traditional radio waves. When a spacecraft uses laser communications to send information, infrared light packs the data into tighter waves so ground stations on Earth can receive more data at once. Laser communications systems can provide 10 to 100 times higher data rates than the radio systems used by space missions today.

As science instruments evolve to capture high-definition data, missions will need expedited ways to transmit information to Earth. It would take roughly nine weeks to transmit a complete map of Mars back to Earth with current radio frequency systems. With lasers, it would only take about nine days.

A research team at Osaka Metropolitan University has fabricated a gallium nitride (GaN) transistor using diamond, which of all natural materials has the highest thermal conductivity on earth, as a substrate, and they succeeded in increasing heat dissipation by more than 2X compared with conventional transistors. The transistor is expected to be useful not only in the fields of 5G communication base stations, weather radar, and satellite communications, but also in microwave heating and plasma processing.

Researchers at Osaka Metropolitan University are proving that diamonds are so much more than just a ‘girl’s best friend.’ Their groundbreaking research focuses on gallium nitride (GaN) transistors, which are high-power, high-frequency semiconductor devices used in mobile data and satellite communication systems.

With the increasing miniaturization of semiconductor devices, problems arise such as increases in power density and heat generation that can affect the performance, reliability, and lifetime of these devices.

HIVE begins testing in deep space.

• Los microrobots de la misión de la UNAM encendieron correctamente, informó Gustavo Medina Tanco • La misión tiene un nivel de éxito mayor al 50 por ciento y se espera que en las próximas horas-y durante la madrugada-se efectúen pruebas que puedan llevar a un 75 por ciento de éxito.

WASHINGTON — The U.S. Space Force has inked a $19.8 million deal with Microsoft to develop a virtual and mixed-reality training environment. This agreement positions the tech giant in the burgeoning military simulation market and expands its Azure cloud’s reach into space applications.

The one-year contract announced Jan. 5 is to continue work on an augmented reality space simulation tool that Microsoft started developing last year for the Space Systems Command in Los Angeles.

Dubbed the Integrated, Immersive, Intelligent Environment (I3E), the system features Microsoft’s HoloLens headsets, Azure cloud platform, and a mesh framework for building shared AR experiences. Together, these technologies enable an interactive model of space with accurately scaled orbital objects that users can manipulate in real time.

A new study published in The Astrophysical Journal reveals new evidence for standard gravity breaking down in an idiosyncratic manner at low acceleration. This new study reinforces the evidence for modified gravity that was previously reported in 2023 from an analysis of the orbital motions of gravitationally bound, widely separated (or long-period) binary stars, known as wide binaries.

The new study was carried out by Kyu-Hyun Chae, a professor of physics and astronomy at Sejong University in Seoul, South Korea, with wide binaries observed by European Space Agency’s Gaia space telescope.

Gravitational anomalies reported in 2023 by Chae’s study of wide binaries have the unique feature that orbital motions in binaries experience larger accelerations than Newtonian predictions when the mutual gravitational acceleration is weaker than about 1 nanometer per second squared and the acceleration boost factor becomes about 1.4 at accelerations lower than about 0.1 nanometer per second squared.

The biggest buzz in ground-based astronomy these days is the soon to be completed Rubin Observatory and its forthcoming wide field Large Synoptic Sky Survey.

When the widefield optical Rubin Observatory comes online later this year, it will not only revolutionize astronomy, but the art of science data management as well.

The Space Force announced Friday that it has given Microsoft a contract to continue work on a simulated environment where guardians can train, test new capabilities and interact with digital copies of objects in orbit.

Under the $19.8 million, one-year contract from Space Systems Command (SSC), Microsoft will develop the Integrated, Immersive, Intelligent Environment (I3E) — an augmented reality space simulation powered by the company’s HoloLens headsets. The training tool is a successor to the service’s Immersive Digital Facility (IDF) prototype developed in 2023, according to a press release.

The contract period began Dec. 1, and the deal includes a reserved scope for an additional three years of work, per the release.

“The misperception of Neptune’s color, as well as the unusual color changes of Uranus, have bedeviled us for decades. This comprehensive study should finally put both issues to rest,” said Dr. Heidi Hammel.

In space, not everything is how it seems, and this might be the case with Uranus and Neptune, as a study scheduled to be published in February 2024 in the Monthly Notices of the Royal Astronomical Society examines how the colors of the two gas giants might be more similar that what NASA’s Voyager 2 spacecraft imaged in 1986 and 1989, respectively, as it flew past the gas giants during its mission. Originally, Voyager 2 imaged Uranus to exhibit a greenish-type color while Neptune appeared to be a strong blue, and this new study holds the potential to help scientists better understand how to estimate the true colors of planets throughout the cosmos.

“Although the familiar Voyager 2 images of Uranus were published in a form closer to ‘true’ color, those of Neptune were, in fact, stretched and enhanced, and therefore made artificially too blue,” said Dr. Patrick Irwin, who is a Professor of Planetary Physics at the University of Oxford and lead author of the study. “Even though the artificially-saturated color was known at the time amongst planetary scientists – and the images were released with captions explaining it – that distinction had become lost over time.”

Continue reading “Revealing the True Colors of Neptune and Uranus: A Breakthrough Study” »

First, we halved the deep methane abundance (model A), since we know the polar regions are methane-depleted, but found that although such a change produces changes in (I/F)₀ and k that reasonably approximate the shape of observed differences between the polar and equatorial regions in Fig. 12, the amplitude is not sufficiently large and is close to zero at blue wavelengths. Secondly, we tried halving the methane abundance and increasing the opacity of the Aerosol-2 layer, τ₂, by 1.0 (model B), from 4.6 to 5.6. Note that all opacities quoted here are at a reference wavelength of 800 nm. Here, we see an increase in the (I/F)₀ and k difference at green wavelengths, but a decrease at blue wavelengths. The reason for this is that the Aerosol-2 particles are retrieved to have increased imaginary refractive index at blue wavelengths (Irwin et al. 2022), which lowers the single-scattering albedo here. Hence, increasing the Aerosol-2 opacity reduces the reflectivity at blue wavelengths, rather than increasing it. How then can we match the observed differences between the polar and equatorial spectra of the 2002 HST/STIS data? In the study of James et al. (2023), noted earlier, it was found that the optimal solution was to not only increase the opacity of the particles in the Aerosol-2 layer, but also make them more reflective at wavelengths longer than 500 nm. We could have similarly adjusted the imaginary refractive index spectra, n_imag, of the Aerosol-2 particles (lower n_imag values increase the single-scattering albedo), but in a parallel analysis of VLT/MUSE observations of Neptune, Irwin et al. (2023b) found that the observed spectra of deep bright spots could be well approximated by adding a component of bright particles to the existing Aerosol-1 layer at ∼5 bar. We wondered whether a similar approach might be applicable here. Changes in the Aerosol-1 layer cannot account for the observed HST/STIS pole–equator differences, since this layer is only detectable in narrow wavelength bands of very low methane absorption, but in Fig. 12 it can be seen that if we add a unit opacity of conservatively scattering particles to the Aerosol-2 layer at 1–2 bar (with the same Gamma size distribution as the Aerosol-2 particles, with mean radius 0.6 μm and variance σ = 0.3) the (I/F)₀ and k difference increases at all wavelengths longer than ∼ 480 nm (model X), although not as much as the difference between polar and equatorial latitudes. However, if we add this additional opacity and simultaneously halve the methane abundance (Model C1) we find that the differences in the (I/F)₀ and k spectra agree moderately well with the observed pole–equator difference spectra at most wavelengths. What might be responsible for this extra component of bright particles in the Aerosol-2 layer will be discussed further, but it could indicate that more methane ice particles are present in the haze/methane-ice layer, or that more methane ice is condensed onto the haze Cloud Condensation Nuclei (CCN). Whatever the cause, it is clear that the spectral difference between the polar and equatorial regions seen by HST/STIS in 2002 is consistent with a reduction in methane abundance coupled with an increase in the reflectivity of the particles in the Aerosol-2 layer that could be caused by the addition of a conservatively scattering component.

Having surveyed the possible interpretations of the HST/STIS polar and equatorial spectra, we then tested these models against the seasonal photometric magnitude data. While the Lowell Observatory magnitude data accurately preserve the quantities that were measured, they are a less intuitive measure for interpreting the changes in Uranus’s reflectivity spectrum with atmospheric models. Hence, we converted the magnitudes to the mean disc-averaged reflectivities of Uranus, which also corrects out the solid-angle variations of Uranus’s disc size, noted earlier. This conversion was done using the procedures outlined in Appendix B. The resulting seasonal variations in disc-averaged reflectivity at the blue and green wavelengths of the Strömgren b and y filters are shown in Fig. 13. Here, it can be seen that the disc-averaged green reflectivity of Uranus changes from ∼0.47 to ∼0.