The Sun Radio Interferometer Space Experiment (SunRISE) Ground Radio Lab (GRL) is a Science, Technology, Engineering, Arts, and Mathematics (STEAM) project aiming to engage and train the next generations of scholars. To achieve this, the project 1) recruited students to participate in the design, development, and testing of a simple antenna kit that were sent to high schools nationwide free of charge, 2) prepared online, self-paced training modules to educate students on topics including radio astronomy and space weather, and 3) recruited high schools to host antenna installations, participate in regular data collection and analysis campaigns, and engage in monthly webinars and Q&A sessions with space industry experts. GRL observation campaigns during the ongoing solar maximum have cataloged various solar radio bursts (SRB) types, defined as low-frequency radio emissions emanated by accelerated electrons associated with extreme solar activity, including solar flares and coronal mass ejections (CMEs). Our observations indicate that 1) Type III radio bursts closely follow solar flares, with their intensity often matching the flare’s strength, helping to further our understanding of electron acceleration and propagation dynamics, and 2) Type II radio bursts coincide with geomagnetic disturbances caused by Earth-bound CMEs, aligned with established literature. Our community of high school students and mentors will continue to maintain our publicly available catalog of SRBs in support of the science objectives of SunRISE mission.

We perform a statistical study of 3-s ultra-low frequency (ULF) waves using MMS observations in the Earth’s foreshock region. The average phase velocity in the plasma rest frame is determined to be anti-sunward, and the intrinsic polarization is right-handed. We further examine the linear instability conditions based on drift-bi-Maxwellian distribution functions according to observed plasma conditions. The resulting instability is a solution to the common dispersion equation of the ion/ion right-hand non-resonant and left-hand resonant instabilities. The predicted wave propagation is also predominantly anti-sunward. The cyclotron resonant conditions of the solar wind and backstreaming beam ions are evaluated, and we find that in some cases, the anti-sunward propagating waves can be resonant with beam ions, which was overlooked in previous studies. The result suggests that the dispersion equation provides the 3-s ULF waves a fundamental explanation that unifies a rich variety of resonant conditions. In the later stage, the 3s ULF waves could further develop into Short Large Amplitude Magnetic Structures, contributing to the turbulence in the foreshock region.

The occurrence of Jovian decametric emission (DAM) is sporadic as observed from ground-based instruments. When the timing intervals of observed occurrences of Jovian DAM are compared to all periods when Jupiter was observable, a set of Jovian DAM emission occurrence probabilities can be created. These probabilities are usefully plotted as a function of Jovian system III (magnetospheric) central meridian longitude (CML-III) and Io’s phase measured from superior geocentric conjunction (SGC), producing a CML-Io phase plane. It has been known since 1964 that Jovian DAM tends to have higher occurrence probabilities in different regions of the CML-Io phase plane, leading to the identification of different Io-related and non-Io-related DAM components. AJ4CO Observatory, located in High Springs, Florida, USA, has been observing Jupiter when it is within ~4.5 hours of transit since October, 2013. The primary instrument used for observing Jovian DAM is a swept-frequency (16 to 32 MHz) dual polarization spectrograph fed by an eight-element phased array of terminated folded dipoles. A high-speed digital spectrograph with a tunable 2 MHz bandwidth was also used from 2013 to 2016 to observe emission at higher time resolution. We analyze the dynamic spectra of Jovian DAM observed at AJ4CO Observatory from 2013 through 2020 to measure emission timing intervals and classify the emission into four types: L (for wideband L bursts), S (for wideband S bursts), N (for narrowband continuous emission), and T (for narrowband trains of S bursts). For this presentation, we show CML-Io phase plane probabilities categorized by radio frequency, polarization, emission type, and emission arc shape. We show how the various high-probability DAM regions within the phase plane change with each parameter and with various combinations of parameters. We present updated definitions of the DAM component phase plane boundaries and discuss how the DAM components appearing in various parts of the CML-Io phase plane may differ from one another.