Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628
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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Presentation to be presented during the Site-Directed Research and Development (SDRD) program FY 2021 review meeting (Webex), September 22–23, 2021.
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Case study of a DOE 2021 Housing Innovation Award winning custom home in a hot-humid climate that got a HERS -21 with PV, with 1,288 square feet, ENERGY STAR appliances, low-flow fixtures, low-e3 ENERGY STAR windows, LED lighting, six clerestory windows, and solar tubes.
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An overview of the history of cybersecurity at INL and how it has evolved with today's Critical Infrastructure, including the advancement of Electric Vehicles (EVs) and the EV charging infrastructure. Recent and future research efforts are included to demonstrate the current state of the art and where this technology might progress. With maybe a little Fear, Uncertainty, and Doubt (FUD) mixed in...
DESI observational data for the GD-1 and C-19 streams are compared to stream simulations in a common evolving multi-halo potential of a Milky Way-like galaxy based on a cosmological simulation. The goal is to find the best match of the stream velocity spread and the density power spectrum stream density to simulations having either CDM or WDM subhalos. The cocoon velocity width integrated over the length of the stream is independent of orbital blurring along the stream and the power spectrum integrates over the width of the stream, sidestepping the geometric details of the streams. Streams develop from star clusters inserted at $\simeq$1 Gyr after the Big Bang and evolved for 13 Gyr to their current orbital positions. Streams in a CDM subhalo population provide the best match to the velocity width, with streams younger than 10 Gyr ruled out as insufficiently hot. The progenitor star cluster masses, which determine the fraction of stars released at late times which comprise the stream core, are found to be $\simeq 8\times 10^4 M_\odot$ for GD-1 and $\simeq 4\times 10^4 M_\odot$ for C-19, although the mass depends on the star cluster half mass radius. Stream heating leads to stream lumpiness which is measurable for the relatively large and clean GD-1 dataset. The stream density power spectrum measured along the length of the DESI GD-1 sample is in good agreement with CDM simulations, with 1.7 to 1.9 times more power than WDM 7 keV and 5.5 keV simulations.
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