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1. Wireless optogenetic neural dust for deep brain stimulation

   https://doi.org/10.1109/HealthCom.2016.7749532  

   Wirdatmadja, Stefanus A.; Balasubramaniam, Sasitharan; Koucheryavy, Yevgeni; Jornet, Josep Miquel (September 2016, 2016 IEEE 18th International Conference on e-Health Networking, Applications and Services (Healthcom))
2. Supernova Dust Evolution Probed by Deep-sea ⁶⁰ Fe Time History

   https://doi.org/10.3847/1538-4357/acb699  

   Ertel, Adrienne F.; Fry, Brian J.; Fields, Brian D.; Ellis, John (April 2023, The Astrophysical Journal)

   Abstract There is a wealth of data on live, undecayed⁶⁰Fe (t_1/2= 2.6 Myr) in deep-sea deposits, the lunar regolith, cosmic rays, and Antarctic snow, which is interpreted as originating from the recent explosions of at least two near-Earth supernovae. We use the⁶⁰Fe profiles in deep-sea sediments to estimate the timescale of supernova debris deposition beginning ∼3 Myr ago. The available data admits a variety of different profile functions, but in all cases the best-fit⁶⁰Fe pulse durations are >1.6 Myr when all the data is combined. This timescale far exceeds the ≲0.1 Myr pulse that would be expected if⁶⁰Fe was entrained in the supernova blast wave plasma. We interpret the long signal duration as evidence that⁶⁰Fe arrives in the form of supernova dust, whose dynamics are separate from but coupled to the evolution of the blast plasma. In this framework, the >1.6 Myr is that for dust stopping due to drag forces. This scenario is consistent with the simulations in Fry et al. (2020), where the dust is magnetically trapped in supernova remnants and thereby confined around regions of the remnant dominated by supernova ejects, where magnetic fields are low. This picture fits naturally with models of cosmic-ray injection of refractory elements as sputtered supernova dust grains and implies that the recent⁶⁰Fe detections in cosmic rays complement the fragments of grains that survived to arrive on the Earth and Moon. Finally, we present possible tests for this scenario. 

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3. ILLUMINATING EQUATORIAL ENVIRONMENTS, CLIMATE, AND LIFE OF THE PERMIAN: THE DEEP DUST DRILLING PROJECT

   https://doi.org/10.1130/abs/2024AM-402502  

   Soreghan, Gerilyn S; Ramezani, Jahandar; Benison, Kathleen; Pfeifer, Lily; Noren, Anders; Hinnov, Linda (January 2024, Abstracts with programs Geological Society of America)
4. A Deep Learning Model for Detecting Dust in Earth's Atmosphere from Satellite Remote Sensing Data

   https://doi.org/10.1109/SMARTCOMP50058.2020.00045  

   Hou, Ping; Guo, Pei; Wu, Peng; Wang, Jianwu; Gangopadhyay, Aryya; Zhang, Zhibo (September 2020, 2020 IEEE International Conference on Smart Computing (SMARTCOMP))

   null (Ed.)
5. Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope

   https://doi.org/10.3847/1538-3881/ad67cb  

   Wolff, Schuyler G; Gáspár, András; Rieke, George H; Leisenring, Jarron M; Su, Kate; Wilner, David J; Matrà, Luca; Ygouf, Marie; Ballering, Nicholas P (November 2024, The Astronomical Journal)

   Abstract We present a provisory scattered-light detection of the Vega debris disk using deep Hubble Space Telescope (HST) coronagraphy (PID 16666). At only 7.7 pc, Vega is immensely important in debris disk studies both for its prominence and also because it allows the highest physical resolution among all debris systems relative to temperature zones around the star. We employ the STIS coronagraph’s widest wedge position and classical reference differential imaging to achieve among the lowest surface-brightness sensitivities to date ( $\sim 4\mu {\mathrm{Jy}\mathrm{arcsec}}^{-2}$) at wide separations using 32 orbits in Cycle 29. We detect a halo extending from the inner edge of our effective inner working angle at 10.″5 out to the photon noise floor at 30″ (80–230 au). The face-on orientation of the system and the lack of a perfectly color-matched point-spread function star have posed significant challenges to the reductions, particularly regarding artifacts from the imperfect color matching. However, we find that a halo of small dust grains provides the best explanation for the observed signal. Unlike Fomalhaut (a close twin to Vega in luminosity, distance, and age), there is no clear distinction in scattered light between the parent planetesimal belt observed with the Atacama Large Millimeter/submillimeter Array and the extended dust halo. These HST observations complement JWST GTO Cycle 1 observations of the system with NIRCam and MIRI. 

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