UMBC Goddard Planetary Heliophysics Institute (GPHI)
Permanent URI for this collectionhttp://hdl.handle.net/11603/10907
In May 2011, the NASA Goddard Space Flight Center (GSFC) awarded a Cooperative Agreement to the University of Maryland, Baltimore County, to create a science center for collaborative research in Solar-Planetary Sciences at NASA’s Goddard Space Flight Center, Greenbelt, MD. Through this arrangement, UMBC and its partners – University of Maryland College Park and American University – developed collaborative research programs in all areas of the Heliophysics sciences. This consortium between government and universities to create GPHI (Goddard Planetary Heliophysics Institute) not only provided a secure “home” for Heliophysics scientists, but also synergistically fostered new directions in research and technology.
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Recent Submissions
Item First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts(AAS, 2025-05) Krupar, Vratislav; Kontar, Eduard P.; Soucek, Jan; Wilson, Lynn B.; Szabo, Adam; Kruparova, Oksana; Reid, Hamish A. S.; Hajos, Mychajlo; Pisa, David; Santolik, Ondrej; Maksimovic, Milan; Pickett, Jolene S.We report the first detection of type III solar radio burst striae in the 30–80 kHz range, observed by the Cluster-4 spacecraft during an exceptionally quiet solar period. These low-frequency fine structures, which drift slowly in frequency and exhibit narrow bandwidths, provide a novel diagnostic of plasma processes in the inner heliosphere. The detected striae, interpreted as fundamental plasma emission, exhibit a frequency drift rate of 0.328 Hz s⁻¹ and a bandwidth of 1.3 kHz. By combining high-resolution radio observations with well-calibrated in situ electron velocity distribution function data from the Wind spacecraft, we characterized the plasma properties of the burst source region near 0.32 au. Our analysis estimates relative density fluctuations, at the effective turbulence scale length, as approximately 3.4% (inferred from striae bandwidths), 0.62% (from intensity fluctuations), and 3.5% (from a heliocentric distance-based empirical model). These findings offer critical insights into small-scale density inhomogeneities and turbulence that affect electron beam propagation. This study underscores the potential of combining well-calibrated in situ electron data with radio burst measurements to probe the physical conditions of the solar wind and to refine our understanding of solar radio bursts across a broad frequency range.Item Evidence of Interaction between Ion-Scale Waves and Ion Velocity Distributions in the Solar Wind(2025-05-05) Yogesh; Ofman, Leon; Boardsen, Scott; Klein, Kristopher; Martinovic, Mihailo; Sadykov, Viacheslav M.; Verniero, Jaye; Shankarappa, Niranjana; Jian, Lan K.; Mostafavi, Parisa; Huang, Jia; Paulson, K. W.Recent in situ observations from Parker Solar Probe (PSP) near perihelia reveal ion beams, temperature anisotropies, and kinetic wave activity. These features are likely linked to solar wind heating and acceleration. During PSP Encounter 17 (at 11.4Rₛ) on Sep-26-2023, the PSP/FIELDS instrument detected enhanced ion-scale wave activity associated with deviations from local thermodynamic equilibrium in ion velocity distribution functions (VDFs) observed by the PSP/Solar Probe Analyzers-Ion (SPAN-I). Dense beams (secondary populations) were present in the proton VDFs during this wave activity. Using bi-Maxwellian fits to the proton VDFs, we found that the density of the proton beam population increased during the wave activity and, unexpectedly, surpassed the core population at certain intervals. Interestingly, the wave power was reduced during the intervals when the beam population density exceeded the core density. The drift velocity of the beams decreases from 0.9 to 0.7 of the e Alfvén speed and the proton core shows a higher temperature anisotropy (T ⊥* / T ∥* > 2.5) during these intervals. We conclude that the observations during these intervals are consistent with a reconnection event during a heliospheric current sheet crossing. During this event, α particle parameters (density, velocity, and temperature anisotropy) remained nearly constant. Using linear analysis, we examined how the proton beam drives instability or wave dissipation. Furthermore, We investigated the nonlinear evolution of ion kinetic instabilities using hybrid kinetic simulations. This study provides direct clues about energy transfer between particles and waves in the young solar wind. * = symbol is in subscriptItem Tracing the Heliospheric Magnetic Field via Anisotropic Radio-Wave Scattering(2025-03-28) Clarkson, Daniel L.; Kontar, Eduard P.; Chrysaphi, Nicolina; Emslie, A. Gordon; Jeffrey, Natasha L. S.; Krupar, Vratislav; Vecchio, AntonioAstrophysical radio sources are embedded in turbulent magnetised environments. In the 1 MHz sky, solar radio bursts are the brightest sources, produced by electrons travelling along magnetic field lines from the Sun through the heliosphere. We demonstrate that the magnetic field not only guides the emitting electrons, but also directs radio waves via anisotropic scattering from density irregularities in the magnetised plasma. Using multi-vantage-point type III solar radio burst observations and anisotropic radio wave propagation simulations, we show that the interplanetary field structure is encoded in the observed radio emission directivity, and that large-scale turbulent channelling of radio waves is present over large distances, even for relatively weak anisotropy in the embedded density fluctuations. Tracing the radio emission at many frequencies (distances), the effects of anisotropic scattering can be disentangled from the electron motion along the interplanetary magnetic field, and the emission source locations are unveiled. Our analysis suggests that magnetic field structures within turbulent media could be reconstructed using radio observations and is found consistent with the Parker field, offering a novel method for remotely diagnosing the large-scale field structure in the heliosphere and other astrophysical plasmas.Item Temporal and Spatial Dynamics of Nitric Oxide Production at High Latitudes Caused by an ICME-Driven Storm onDec. 14, 2006(AGU, 2025) Delano, Kevin; Zesta, Eftyhia; Oliveira, Denny; Martínez Ledesma, Miguel; Mutschler, ShaylahGeomagnetic storms release large amounts of energy on Earth's upper atmosphere at high latitudes that result in the heating and upward expansion of the neutral gas. During geomagnetic storms driven by interplanetary coronal mass ejections (ICMEs), neutral mass density heating and cooling times are shorter for stronger storms and longer for weaker storms. The start time influx of energy into Earth's upper atmosphere allows for the enhanced production of nitric oxide (NO) at high latitudes, which in turn cools the thermosphere by radiating away excess energy. As a result, greater NO production results in quicker thermospheric cooling. While the production of NO on a global scale has been linked to the storm cycle, the spatiotemporal evolution of NO with respect to the storm onset and storm strength must also be understood to improve predictions of the storm evolution cycle and their impact on low-Earth orbit satellites. In this study, we investigate the effects of a particular ICME-driven storm on the production of NO at high latitudes and associated local time asymmetries. We compare NO measurements from the Thermosphere, Ionosphere, Mesosphere Dynamics (TIMED) spacecraft to neutral mass density measurements from the Challenging Minisatellite Payload spacecraft and find that the impact of the shock prior to the storm, in addition to the onset of the storm itself, is responsible for an increase in NO production. We also observe a dawn-dusk asymmetry in high-latitude NO production and identify solar wind geometry and internal processes as potential drivers for this asymmetry.Item Pushing the Frontier of Solar & Space Physics: Exploration of the Heliosphere and the Very Local Interstellar Medium by an Interstellar Probe(American Astronomical Society, 2023-07-31) Brandt, Pontus; Alterman, Benjamin; Alvarez, Erika; Baker, Daniel; Bale, Stuart; Baliukin, Igor; Barabash, Stas; Beichman, Charles; Bergman, Jan; Bertaux, Jean-Loup; Bladek, Piotr; Blanc, Michel; Christian, Eric; Clarke, John; Cocoros, Alice; Cooper, John; Decker, Robert; DeMajistre, Robert; Desai, Mihir; Dialynas, Kostas; Dodd, Suzanne; Eriksson, Stefan; Fedorov, Andrei; Fields, Brian; Fisk, Lennard; Fountain, Glen; Friedman, Louis; Frisch, Priscilla; Fujimoto, Masaki; Funsten, Herbert; Galli, Andre; Gavilian, Lisseth; Gkioulidou, Matina; Gladstone, Randy; Gloeckler, George; Gruntman, Mike; Gurvits, Leonid; Harman, Sonny; Hill, Matthew; Ho, George; Holler, Bryan; Horanyi, Mihaly; Horbury, Timothy; Hunziker, Silvan; Iess, Luciano; Katushkina, Olga; Kempf, Sascha; Kha, Kathy; Kinnison, James; Kornbleuth, Marc; Korreck, Kelly; Krimigis, Tom; Kucharek, Harald; Kurth, William; Lallement, Rosine; Lavraud, Benoit; Liewer, Paulett; Linsky, Jeffrey; Lisse, Casey; Livi, Stefano; Magnes, Werner; Mandt, Kathleen; Mayyasi, Majd; McNutt, Ralph; Mewaldt, Richard; Miller, Jesse; Mitchell, Donald; Moebius, Eberhard; Mostafavi, Parisa; Nicolaou, Georgios; Nikoukar, Romina; Opher, Merav; Owino, Stephen; Park, Jeewoo; Paschalidis, Nikolaos; Paul, Michael; Paxton, Larry; Plaschke, Ferdinand; Plumaris, Michael; Pogorelov, Nikolai; Poppe, Andrew; Provornikova, Elena; Ratkiewicz, Romana; Redfield, Seth; Reisenfeld, Daniel; Retherford, Kurt; Richardson, John; Roelof, Edmond; Runyon, Kirby; Rymer, Abigail; Santos-Costa, Daniel; Schwadron, Nathan; Sigurdsson, Steinn; Slavin, Jonathan; Smith, Todd; Sokol, Justyna; Sorriso-Valvo, Luca; Spilker, Linda; Spitzer, Sarah; Stapelfeldt, Karl; Sterken, Veerle; Stern, Alan; Stough, Robert; Swaczyna, Pawel; Szabo, Adam; Szalay, Jamey; Turner, Drew; Vertesi, Janet; Wahlund, Jan-Erik; Wang, Chi; Westlake, Joseph; Wicks, Robert; Wimmer-Schweingruber, Robert; Wood, Brian; Wurz, Peter; Zarka, Philippe; Zemcov, Michael; Zirnstein, Eric; Zong, QiugangThe interaction of our protective heliosphere and the Very Local Interstellar Medium (VLISM) is the least explored and most rewarding frontier of space physics. New evidence amplifies the central role of the heliosphere in the evolution of the solar system along its 4.6- billion-year journey around the galaxy. In addition to the dense clouds of plasma, gas and dust seeding the early proto solar nebula, recent supernovae have left the entire solar system exposed to extreme fluxes of interstellar material and cosmic radiation with far-reaching implications. Our current knowledge lacks the direct measurements necessary to understand how our star upholds its vast heliosphere and its potentially game-changing role in the evolution of our galactic home. Interstellar Probe provides new, required measurements over more than a solar cycle to uncover the physical processes starting near the Sun responsible for creating our dynamic heliosphere. In April 2022, the pragmatic Interstellar Probe Mission Concept Study was completed after four years, detailing a Large Strategic heliophysics mission that would transect the heliosphere from 1 au to the VLISM. Its journey provides rich science for generations across heliophysics and presents an opportunity to push the frontier of space exploration farther than ever done before. Modest crossdivisional investments enable high-value planetary science and astrophysics, deepening our understanding of the emergence of our habitable planetary system. A trajectory through the forward hemisphere of the heliosphere would be accomplished by a launch in the 2036-2042 timeframe using conventional chemical propulsion and a heavy-lift launch vehicle, such as the Space Launch System (SLS). A Jupiter Gravity Assist could propel an 860-kg spacecraft with an 87-kg payload of ten instruments delivering a unified view of the global heliosphere, reaching the VLISM after 16 years. The spacecraft is designed to a 50-year nominal lifetime using modern-day technology based on successful missions like New Horizons. Two next-generation Radioisotope Thermal Generators (RTGs) would ensure 300 We at end of nominal mission at 375 au and could enable exploration even beyond 500 au.Item The first analysis of the outward H fluxes measured by IBEX-Lo in 20–50 Rᴇ geocentric distances(Frontiers, 2025-03-13) Park, Jeewoo; Connor, Hyunju K.In this study, we analyze the energetic neutral atom (ENA) observations measured in the lowest energy channel (10–21 eV) of the IBEX-Lo instrument on Interstellar Boundary Explorer (IBEX) during two spring seasons, day of year (DOY) 101–146, 2009, and DOY 88–178, 2013, confirming the existence of outward hydrogen (H) fluxes at 15 eV. The outward H flux decreases slightly with distance, showing an intensity of approximately 10⁶ cm⁻² s⁻¹ sr⁻¹ keV⁻¹. Results also suggest that the outward H fluxes are not influenced by solar radio flux. We compute the expected H ENA fluxes at 15 eV using ion flux measurements from the Helium, Oxygen, Proton, and Electron (HOPE) mass spectrometer aboard the Radiation Belt Storm Probes (RBSP) during the corresponding period of the 2013 spring season, combined with a simple exospheric density model (nʜ=nʜ₀(r₀/r)³, where r₀=10 Rᴇ). The expected ENA fluxes similarly show a decrease in the intensity with increasing geocentric distance, which is on the order of 10⁵–10⁶ cm⁻² s⁻¹ sr⁻¹ keV⁻¹. These consistent features suggest that the outward H fluxes observed by IBEX-Lo are closely related to escaping H ENAs produced within the inner exosphere (<4 Rᴇ).Item Field Aligned Currents and Aurora During the Terrestrial Alfven Wing State(2025-03-11) Burkholder, Brandon; Chen, Li-Jen; Sorathia, Kareem; Lin, Dong; Vines, Sarah; Bowers, Charles F.When sub-Alfv´enic (Alfv´en Mach number MA < 1) plasmas impact Earth, the magnetosphere develops Alfv´en wings. A Multiscale Atmosphere Geospace Environment (MAGE) global simulation of the April 2023 geomagnetic storm, validated against Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE), reveals the mechanism of field-aligned current (FAC) generation and auroral precipitation for the terrestrial Alfv´en wings. Simulation and observations show northern hemisphere planetward flowing auroral electrons (negative FAC) are predominantly at magnetic local times (MLTs) 8-12. Just before the wings formed, solar wind conditions were similar and MA ∼ 1.4, yet the same FAC system extended from 9-18 MLT. Flow vorticity drives FACs at the boundary of the Alfv´en wings and unshocked solar wind. The Alfv´en wing shape presents a different obstacle to the solar wind compared to typical lobe fluxes, producing the unique FAC and auroral patterns. New insights about Alfv´en wing FACs will help to understand auroral features for exoplanets inside their host star’s Alfv´en zoneItem Mach Number Scaling of Foreshock Magnetic Fluctuations at Quasi-parallel Bow Shocks and Their Role in Magnetospheric Driving Throughout the Solar System(AAS, 2025-01-30) Burkholder, Brandon; Chen, Li-Jen; Nykyri, Katariina; Romanelli, Norberto; Sarantos, Menelaos; Sibeck, Dave; Verniero, Jaye; DiBraccio, Gina A.; Gershman, Daniel; Lindberg, Martin; Kincade, ErinUpstream of quasi-parallel bow shocks, reflected ions generate ion–ion instabilities. The resulting magnetic fluctuations can advect through the shock and interact with planetary magnetospheres. The amplitude of magnetic fluctuations depends on the strength of the shock, quantified by the Alfvén Mach number (MA), which is the ratio of solar wind velocity to the local Alfvén velocity. With increasing heliocentric distance, the solar wind MA generally increases, such that Mercury typically experiences a lower MA ~ 5 compared to Earth (MA ~ 8), and Mars a slightly higher MA ~ 9. Farther out in the solar system, Saturn has even higher MA (~10). However, the solar wind flow is highly irregular, and on top of solar cycle variations these values for average MA at each planet do not capture extreme events. Statistical analysis of OMNIWeb observations from 2015 to 2023 shows that sustained (30 minutes or more) high MA (30–100) occurs at Earth about once a month. Using a selection of events in the ion foreshock regions of Mercury, Earth, Mars, and Saturn, a linear scaling is calculated for the maximum magnetic fluctuation amplitude as a function of MA. The resulting slope is ~0.2. Based on the dominant fluctuation frequency for the largest-amplitude events at each planet, it is found that Mars exists in a special regime where the wave period of the magnetic fluctuations can be similar to or longer than the magnetospheric convection timescale, making Mars more susceptible to space weather effects associated with foreshock fluctuations.Item Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe(AAS, 2025-01-14) Kruparova, Oksana; Szabo, Adam; Jian, Lan K.; Němec, František; Šafránková, Jana; Němeček, Zdeněk ; Pasanen, Jacob; Narock, Ayris; Krupar, VratislavWe present a comprehensive analysis of 66 interplanetary shocks observed by the Parker Solar Probe between 2018 November and 2024 January. Among these, 33 events fulfilled the Rankine–Hugoniot (R-H) conditions, ensuring reliable asymptotic plasma parameter solutions. The remaining 33 events could not be confirmed by the standard R-H approach—potentially including wave-like structures—yet were analyzed via averaging and mixed-data methods to obtain robust shock parameters. Utilizing our ShOck Detection Algorithm database, the shocks are categorized into fast-forward, fast-reverse, slow-forward, and slow-reverse types. We investigate the statistical properties of these shocks, focusing on correlations between key parameters—magnetic field compression, density compression, shock normal angle, and change in velocity—and heliocentric distance. Significant positive correlations are identified between heliocentric distance and both magnetic field compression and density compression, suggesting that shocks strengthen as they propagate away from the Sun, largely due to the high local magnetosonic speeds closer to the Sun that can suppress shock formation except in extremely fast events. These findings provide new insights into the dynamic processes governing shock evolution in the inner heliosphere, including scenarios where the near-radial magnetic field geometry may lead to predominantly quasi-parallel shock configurations and thus affect near-Sun particle acceleration efficiency. We also provide strong evidence for the existence of slow-mode shocks near the Sun, contributing to the understanding of shock formation and evolution in the inner heliosphere.Item Connecting energetic electrons at the Sun and in the heliosphere through X-ray and radio diagnostics(A&A, 2025-02-07) Paipa-Leon, David; Vilmer, Nicole; Maksimovic, Milan; Krupar, Vratislav; Vecchio, AntonioSolar flares release huge amounts of energy, a considerable part of which is channeled into particle acceleration in the lower corona. Hard X-ray (HXR) emissions are used to diagnose the accelerated electrons that bombard the chromosphere, while type III radio bursts result from energetic electron beams propagating through the corona and into interplanetary space. The Solar Orbiter mission, launched in 2020, aims to link solar flare remote observations with heliospheric events, thus producing useful observations for our understanding of particle acceleration and propagation from the Sun to the heliosphere. While both hard X-Ray and radio emissions result from flare-accelerated electrons, their relationship is not straightforward. By comparing the evolution of the X-ray emitting sites and the timing of type III bursts, our aim is to determine the conditions for associations between X-ray flares and interplanetary (IP) type III bursts. We analyzed 15 interplanetary type III bursts that are associated with HXR bursts in the first available period for simultaneous X-ray/radio observations of type III bursts from Solar Orbiter (using the RPW and STIX instruments). X-ray imaging was performed around the onset of the type III bursts, complemented by EUI 174 A images to assess the magnetic configuration of the corona. All 15 X-ray flares originated from the same active region on the west limb as observed by Solar Orbiter. In each of the events, a change in X-ray source morphology occurred shortly (<6 minutes) before the onset of type III radio bursts, indicating a change in the electron acceleration region preceding the radio emission. Considering the delays observed between the two emissions, these findings describe complex scenarios with multiple reconnection episodes, some of which may allow accelerated electrons to escape into IP space when open magnetic field lines are involved (interchange reconnection). In some cases, X-ray source elongations toward open field lines in the UV were observed, reinforcing this idea.Item The Solar and Geomagnetic Storms in 2024 May: A Flash Data Report(AAS, 2025-01-16) Hayakawa, Hisashi; Ebihara, Yusuke; Mishev, Alexander; Koldobskiy, Sergey; Kusano, Kanya; Bechet, Sabrina; Yashiro, Seiji; Iwai, Kazumasa; Shinbori, Atsuki; Mursula, Kalevi; Miyake, Fusa; Shiota, Daikou; Silveira, Marcos V. D.; Stuart, Robert; Oliveira, Denny; Akiyama, Sachiko; Ohnishi, Kouji; Ledvina, Vincent; Miyoshi, YoshizumiIn 2024 May, the scientific community observed intense solar eruptions that resulted in a great geomagnetic storm and auroral extensions, highlighting the need to document and quantify these events. This study mainly focuses on their quantification. The source active region (AR; NOAA Active Region 13664) evolved from 113 to 2761 millionths of the solar hemisphere between May 4 and 14. NOAA AR 13664’s magnetic free energy surpassed 10³³ erg on May 7, triggering 12 X-class flares on May 8–15. Multiple interplanetary coronal mass ejections (ICMEs) were produced from this AR, accelerating solar energetic particles toward Earth. According to satellite and interplanetary scintillation data, at least four ICMEs erupted from AR 13664, eventually overcoming and combining each other. The shock arrival at 17:05 UT on May 10 significantly compressed the magnetosphere down to ≈5.04 Rₑ and triggered a deep Forbush Decrease. GOES satellite data and ground-based neutron monitors confirmed a ground-level enhancement from 2 UT to 10 UT on 2024 May 11. The ICMEs induced exceptional geomagnetic storms, peaking at a provisional Dst index of −412 nT at 2 UT on May 11, marking the sixth-largest storm since 1957. The AE and AL indices showed great auroral extensions that located the AE/AL stations into the polar cap. We gathered auroral records at that time and reconstructed the equatorward boundary of the visual auroral oval to 29.°8 invariant latitude. We compared naked-eye and camera auroral visibility, providing critical caveats on their difference. We also confirmed global disturbances of the storm-enhanced density of the ionosphere.Item Detection asymmetry in solar energetic particle events(2024-11-12) Dalla, S.; Hutchinson, Adam; Hyndman, R. A.; Kihara, K.; Nitta, N.; Rodriguez-Garcia, L.; Laitinen, T.; Waterfall, C. O. G.; Brown, D. S.Context. Solar energetic particles (SEPs) are detected in interplanetary space in association with flares and coronal mass ejections (CMEs) at the Sun. The magnetic connection between the observing spacecraft and the solar active region (AR) source of the event is a key parameter in determining whether SEPs are observed and the properties of the particle event. Aims. We investigate whether an east-west asymmetry in the detection of SEP events is present in observations and discuss its possible link to corotation of magnetic flux tubes with the Sun. Methods. We used a published dataset of 239 CMEs recorded between 2006 and 2017 and having source regions both on the front side and far side of the Sun as seen from Earth. We produced distributions of occurrence of in-situ SEP intensity enhancements associated with the CME events, versus \Delta \phi, the separation in longitude between the source active region and the magnetic footpoint of the observing spacecraft based on the nominal Parker spiral. We focused on protons of energy >10 MeV measured by the STEREO A, STEREO B and GOES spacecraft at 1 au. We also considered the occurrence of 71-112 keV electron events detected by MESSENGER between 0.31 and 0.47 au. Results. We find an east-west asymmetry in the detection of >10 MeV proton events and of 71-112 keV electron events. For protons, observers for which the source AR is on the east side of the spacecraft footpoint and not well connected (-180 < \Delta \phi < -40) are 93% more likely to detect an SEP event compared to observers with +40 < \Delta \phi < +180. The asymmetry may be a signature of corotation of magnetic flux tubes with the Sun, given that for events with \Delta \phi < 0 corotation sweeps the particle-filled flux tubes towards the observing spacecraft, while for \Delta \phi > 0 it takes them away from it.Item Additions to Space Physics Data Facility and pysatNASA: Increasing Mars Global Surveyor and Mars Atmosphere and Volatile EvolutioN Dataset Utility(MDPI, 2024-11-08) Esman, Teresa; Halford, Alexa J.; Klenzing, Jeff; Burrell, Angeline G.The Space Physics Data Facility (SPDF) is a digital archive of space physics data and is useful for the storage, analysis, and dissemination of data. We discuss the process used to create an amended dataset and store it on the SPDF. The operational software to generate the archival data software uses the open-source Python package pysat, and an end-user module has been added to the pysatNASA module. The result is the addition of data products to the Mars Global Surveyor (MGS) magnetometer (MAG) dataset, its archival location on SPDF, and pysat compatibility. The primary and metadata format increases the convenience and efficiency for users of the MGS MAG data. The storage of planetary and heliophysics data in one location supports the use of data throughout the solar system for comparison, while pysat compatibility enables loading data in an identical format for ease of processing. We encourage the use of the outlined process for past, present, and future space science missions of all sizes and funding levels. This includes balloons to Flagship-class missions.Item The 10 October 2024 geomagnetic storm may have caused the premature reentry of a Starlink satellite(2024-11-03) Oliveira, Denny; Zesta, Eftyhia; Nandy, DibyenduIn this short communication, we qualitatively analyze possible effects of the 10 October 2024 geomagnetic storm on accelerating the reentry of a Starlink satellite from low-Earth orbit (LEO). The storm took place near the maximum of solar cycle (SC) 25, which has shown to be more intense than SC24. Based on preliminary geomagnetic indices, the 10 October 2024, along with the 10 May 2024, were the most intense events since the well-known Halloween storms of October/November 2003. By looking at a preliminary version of the Dst index and two-line element (TLE) altitude data of the Starlink-1089 (SL1089) satellite, we observe a possible connection between storm main phase onset and a sharp decay of SL1089. The satellite was scheduled to reenter on 22 October, but it reentered on 12 October, 10 days before schedule. The sharp altitude decay of SL1089 revealed by TLE data coincides with the storm main phase onset. Therefore, we call for future research to establish the eventual causal relationship between storm occurrence and satellite orbital decay. As predicted by previous works, SC25 is already producing extreme geomagnetic storms with unprecedented satellite orbital drag effects and consequences for current megaconstellations in LEO.Item Observation of O+ Characteristics During the Terrestrial Alfvén Wing State Induced by the April 2023 Coronal Mass Ejection(2024-10-28) Liang, Haoming; Chen, Li-Jen; Fuselier, Stephen A.; Gomez, Roman G.; Burkholder, Brandon; Bessho, Naoki; Gurram, Harsha; Rice, Rachel C.; Shuster, Jason; Ardakani, Akhtar S.We report Magnetospheric Multiscale observations of oxygen ions (O+) during a coronal mass ejection in April 2023 when the solar wind was sub-Alfvénic and Alfvén wings formed. For the first time, O+ characteristics are studied at the contact region between the unshocked solar wind and the magnetosphere. The O+ ions show energies between 100s eV and ~30 keV. The possible sources are the ring current, the warm plasma cloak, and the ionosphere. The O+ ions exhibit bi-directional streaming along newly-formed closed field lines (CFLs), and dominantly anti-parallel on earlier-formed CFLs. Escaping O+ ions in the unshocked solar wind are observed. During the recovery phase, the O+ pitch-angle distribution associated with flux tubes shows dispersion, indicating potential loss to the solar wind. Our results show escaping as well as trapped O+ ions in the region where a magnetic cloud, an Alfvén wing, and magnetospheric field lines are mixed.Item A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations(IOP, 2024-10-25) Lario, D.; Balmaceda, L. A.; Gómez-Herrero, R.; Mason, G. M.; Krupar, Vratislav; Cormack, C. Mac; Kouloumvakos, A.; Cernuda, I.; Collier, H.; Richardson, I. G.; Kumar, P.; Krucker, S.; Carcaboso, F.; Wijsen, N.; Strauss, R. D.; Dresing, N.; Warmuth, A.; Rodríguez-Pacheco, J.; Rodríguez-García, L.; Jebaraj, I. C.; Ho, G. C.; Buĉík, R.; Pacheco, D.; Lara, F. Espinosa; Hutchinson, Adam; Horbury, T. S.; Rodríguez, L.; Janitzek, N. P.; Zhukov, A. N.; Aran, A.; Nitta, N. V.A series of solar energetic electron (SEE) events was observed from 2022 November 9 to November 15 by Solar Orbiter, STEREO-A, and near-Earth spacecraft. At least 32 SEE intensity enhancements at energies >10 keV were clearly distinguishable in Solar Orbiter particle data, with 13 of them occurring on November 11. Several of these events were accompanied by ≲10 MeV proton and ≲2 MeV nucleon⁻¹ heavy-ion intensity enhancements. By combining remote-sensing and in situ data from the three viewpoints (Solar Orbiter and STEREO-A were ∼20° and ∼15° east of Earth, respectively), we determine that the origin of this rapid succession of events was a series of brightenings and jetlike eruptions detected in extreme ultraviolet (EUV) observations from the vicinity of two active regions. We find a close association between these EUV phenomena, the occurrence of hard X-ray flares, type III radio bursts, and the release of SEEs. For the most intense events, usually associated with extended EUV jets, the distance between the site of these solar eruptions and the estimated magnetic connectivity regions of each spacecraft with the Sun did not prevent the arrival of electrons at the three locations. The capability of jets to drive coronal fronts does not necessarily imply the observation of an SEE event. Two peculiar SEE events on November 9 and 14, observed only at electron energies ≲50 keV but rich in ≲1 MeV nucleon⁻¹ heavy ions, originated from slow-rising confined EUV emissions, for which the process resulting in energetic particle release to interplanetary space is unclear.Item MARBLE: How to make an open science global magnetosphere code?(2023-10-09) Bard, Christopher; Dorelli, John; da Silva, Daniel; Khazanov, George; Sur, DibyenduThe Magnetosphere-Aurora Boundary Layer Explorer (MARBLE) is a currently-under-development global magnetosphere code which will solve the "kinetic Hall MHD" equations. Although NASA now requires all newly funded scientific software to be open source, this is in sharp contrast to the traditionally closed-development ecosystem of global magnetosphere codes. MARBLE, currently being built from the ground up, presents a unique opportunity to develop a large-scale, production code right from the outset with open science principles at its core. While MARBLE's primary objective is to simulate magnetospheric impacts on auroral physics, our stretch goal is to provide a platform for the development of a community, open-source global magnetosphere code. Such a code, in order to be useful, needs to be powerful, accessible, understandable, and seamlessly fit into existing scientific analysis workflows. To achieve this vision, we have chosen to write MARBLE in Python. This provides several advantages, including more rapid development and compatibility with community open source libraries such as Kamodo, SunPy, SpacePy, and others in the PyHC ecosystem. Although pure Python itself is slow, we take advantage of helper libraries such as Numba and CuPy to accelerate low-level arithmetic calculations. The use of Python also enables us to adopt a modular approach to model development. This modularity streamlines addition, substitution, and development of desired features, resulting in a flexible and adaptable resource for the community. We envision this kind of open-source community model as a teaching code, a testbed for prototype development, and a means to more easily ingest and make accessible advanced features from privately developed global codes.Item Enabling Unprecedented Exploration of Kinetic Plasma Phenomena: Utilizing and Reaching Beyond the MMS FPI Breakthrough(AAS, 2023-07-31) Shuster, Jason; Gershman, Daniel; Bessho, Naoki; Wang, Shan; Uritsky, Vadim; Chen, Li-Jen; Gurram, Harsha; Sharma, A. Surjalal; Dorelli, John; Burch, James; Webster, James; Schwartz, Steven; Denton, Richard; Cassak, Paul; Stawarz, Julia; Ng, Jonathan; Paterson, William; Schiff, Conrad; Viñas, Adolfo; Avanov, Levon; Liu, Yi-Hsin; Li, Tak Chu; Argall, Matthew; Torbert, Roy; Afshari, Arya; Payne, Dominic; Farrugia, Charles; Genestreti, Kevin; Verniero, Jaye; Wilder, Frederick; da Silva, Daniel; Haggerty, ColbyThe spectrometer suites onboard NASA’s Magnetospheric Multiscale (MMS) mission offered us an unexpected breakthrough in measurement capability that no spacecraft or laboratory experiment has achieved previously: the ingeniously engineered FPI dual ion and electron spectrometers enable direct measurement of terms in the Vlasov equation for the first time in the history of plasma physics research.Item Research to Operations Visualization for WSA Coronal and Solar Wind Predictions(2023-10-09) Landeros, Jaime A.; da Silva, Daniel; Arge, C. Nick; Jones, Shaela I.The Wang-Sheeley-Arge (WSA) Model has served both the research and operational communities with ambient solar wind forecasts for over a decade, but it has lacked an interactive, centralized, and publicly accessible method for visualizing its empirical and physics-based corona and solar wind predictions. A browser-based dashboard has been developed to fill this gap by providing forecasters with the ability to juxtapose recent in situ and remotely sensed satellite observations and model predictions to assess model performance. It will also serve a complementary purpose of science-enablement through investigation of the model’s detailed ensemble predictions from various satellite perspectives and comparison with observations. Visualized data include time series plots of solar wind speed and interplanetary magnetic field (IMF) polarity, as well as projected maps of derived coronal holes overlayed on EUV coronal hole and filament observations, the heliospheric current sheet location at 5 solar radii, and probabilistic predictions of satellite-footpoint connectivity. Predictions are available for satellites dispersed throughout the Heliospheric System Observatory, including ACE, STEREO-A, PSP, and SolO. The project has been developed with maintainability and ease of deployment in mind with the Plotly Dash framework in Python, targeted JS functions to reduce latency, Git version control, and Docker containerization.Item Helionauts: A Cross-Organization Heliophysics Forum(2023-10-05) Attie, Raphael; Kirk, Michael; Bard, Christopher; Thompson, Barbara; da Silva, Daniel; Narock, Ayris; Mason, Emily; Pesnell, Dean; Zarro, Dominic; Addison, Kevin; Thomas, BrianThe COVID-19 pandemic highlighted the need for a lasting community-wide discussion platform in the field of Heliophysics, supplementing in-person interactions at conferences and within local departments. To address this, instant messaging apps like Slack and Teams were hastily adopted, but their constant online presence requirements posed problems: overlapping content and information sprawl across various chat workspaces, confusion about where discussions should take place. To provide a more coherent landscape for written communication, NASA is backing Helionauts.org, a permanent platform for heliophysicists. It features topic-based and searchable discussions, smart notifications for asynchronous conversations, and supports technical conversations with Markdowns, LaTeX, and code syntax highlighting. The platform fosters inclusivity, connecting experts, postdocs, and students to promote knowledge-sharing and collaboration in our heliophysics community.