@proceedings{Lamy2026-PREX-4607,
        title = "{Planetary, Solar and Heliospheric Radio Emissions X}",
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
         year = 2026,
       editor = {{Lamy}, L. and {Louis}, C.~K. and {Fischer}, G. and {Morosan}, D. and {Zarka}, P.},
        doi = {10.25935/PREX-4607},
        publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris},
       abstract = {The ``10th International Workshop on Planetary, Solar and Heliospheric Radio Emissions" was held in June 2025 in Marseille, France, in continuation of an established tradition following previous successful international workshops held in Austria, in 1984, 1987, 1991, 1996, 2001, 2005, 2010, 2016 and Dublin, in 2022. The proceedings of this workshop are now available as the book ``Planetary, Solar and Heliospheric Radio Emissions 10 (PRE X)". All contributions were double peer-reviewed under the guidance of the five scientific editors L. Lamy, C. K. Louis, G. Fischer, D. Morosan, P. Zarka. The conference was hosted, funded, and logistically supported by Aix-Marseille Université (AMU) and OSU Pythéas, which also provide technical assistance for the dissemination of the proceedings on the HAL platform. The electronic version of the proceedings is published by Observatoire de Paris.}
}

@inproceedings{bria2026-PREX-JDZY,
    author = {{Briand}, C. and {Peccoux}, T. and {Zarka}, P. and {Grie{\ss{}}meier}, J. and {Cecconi}, B. and {Girard}, J.},
    title = {{Decameter solar spikes for coronal diagnostics}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-JDZY},
    abstract = {{The study aims to give some clues on the relationship between solar activity, plasma dynamics, and the occurrence of spikes. A total of one thousand spikes, recorded with high temporal and spectral resolution by the NenuFAR radio instrument, were analyzed. These spikes occur concurrently to Type III storms or Type II. The strong circular polarization observed suggests that emissions are in the fundamental mode. Electron beam velocities deduced from spike time-frequency drifts are at least ten times lower than those driving Type III bursts. The spike's duration shows a dependence with the type of solar activity and scales with frequency as approximately f^-0.73. The coronal temperature decreases with altitude, ranging from about 1 MK to 0.5 MK. Finally, fitting the distributions of duration and bandwidth with a Gamma function indicates that, in contrast to the striae of Type IIIb emissions, spikes are significantly more sensitive to stochastic plasma phenomena.}}
}

@inproceedings{cecc2026-PREX-BFI6,
    author = {{Cecconi}, B. and {Girard}, J. N. and {Dumez-Viou}, C. and {Mauduit}, E. and {Aicardi}, S. and {Nammour}, F. and {nones}, E. Q. and {Xandri-Zaragoza}, B. and {Molina-Gim{\'{e}}nez}, E. and {Martin{\'{e}}z}, O. and {Barcelona-Pons}, D. and {Hadad}, E. and {Bondonneau}, L. and {Landeau}, V. and {Bellucci}, A. and {Penas}, I.},
    title = {{EXTRACT/TASKA: TOWARDS A DIGITAL COMPUTING PLATFORM FOR MODERN RADIO ASTRONOMY}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-BFI6},
    abstract = {{The EXTRACT project (<https://extract-project.eu/>) aims to design a distributed data-mining software platform that can efficiently and smoothly orchestrate tasks across a continuum of computing resources, including edge devices, cloud systems, and high-performance computing centres. One use-case of EXTRACT is TASKA (Transient Astrophysics with an SKA Pathfinder), in which this  platform will be used to process massive astronomy datasets, particularly those generated by the NenuFAR instrument, a SKA Pathfinder developed in Nançay, France. NenuFAR has the potential to produce up to 109 PB of raw data annually, necessitating on-site processing using carefully designed pipelines to reduce the dataset to approximately 1 PB per year.

The TASKA project is structured into four distinct use cases:
(a) Real-time detection of high-resolution events within beamformer data streams, seamlessly integrated with artificial intelligence algorithms.
(b) The development of a modular and adaptable radio imaging pipeline, capable of operating on local, cloud, or high-performance computing resources.
(c) The design of a novel dynamic radio imager, employing video reconstruction techniques and artificial intelligence, as an integral component of the radio imaging pipeline.
(d) The creation of a spatial-temporal-spectral feature-matching tool, facilitating the integration of detected events with images generated by the imaging pipeline.

The current status and results of TASKA activities demonstrate their application to NenuFAR data processing and their relevance for the SKA Regional Centre network.}}
}

@inproceedings{coll2026-PREX-TR41,
    author = {{Collet}, B. and {Lamy}, L. and {Kurth}, W. S. and {Wu}, S. and {Allegrini}, F. and {Connerney}, J. E. P.},
    title = {{Detection of Jovian kilometric and hectometric auroral radio harmonics with Juno/Waves in situ measurements}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    doi = {10.25935/PREX-TR41},
    abstract = {{Auroral radio emissions from Earth, Saturn, and Jupiter are now known to all be generated by the cyclotron maser instability near the electron cyclotron fundamental frequency f_ce. This common generation mechanism results in similar wave properties in terms of beaming and polarization. However, while harmonics at 2 × f_ce and 3 × f_ce have been identified in the terrestrial and kronian cases, none of the components of Jupiter's auroral radio spectrum had been associated with harmonics. In this study, we confirm the existence of first harmonic emissions for the Jovian broadband-kilometric (bKOM) and hectometric (HOM) components (200-700 kHz) in 6 cases using in situ data from Juno/Waves observations close to the source. Among these cases, 2 second harmonics were also identified. These harmonics are three orders of magnitude weaker than the associated fundamental and were identified in regions where the f_pe/f_ce(f_pe the electron plasma frequency) ratio is of the order of 10^-2. This discovery confirms the universality of the CMI and suggests that harmonics in the decametric range could exist.}},
    pages = {}
}

@inproceedings{fisc2026-PREX-YYTU,
    author = {{Fischer}, G. and {Taubenschuss}, U. and {Wu}, S. and {Píša}, D. and {Jost}, D.},
    title = {{Partial polarization and propagation of Saturn kilometric radiation at low and very low frequencies}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-YYTU},
    abstract = {{Saturn kilometric radiation (SKR) is known to be generated by the Cyclotron Maser Instability (CMI) mechanism by which it is largely generated in the right-hand extraordinary mode (R-X), but also left-hand ordinary mode (L-O) is possible. R-X mode SKR shows right-hand circular polarization when coming from the northern aurora and left-hand circular polarization from the southern aurora. Due to its short coherence length, SKR usually experiences incoherent superposition when it originates from various sources, and for this process the Stokes vectors need to be added. In case of two SKR sources with opposite circular polarization, the resultant superposed SKR gets depolarized leading to a partially polarized radio emission. In this paper we discuss the different ways how SKR can be depolarized and the influence of the Enceladus plasma torus on the polarization and propagation of SKR. We look at low and very low SKR frequencies below 100 kHz, and ray-tracing studies suggest that SKR is refracted in and around the meridian plane by the plasma torus. However, direction finding of SKR could not confirm this, since radio waves of low polarization degree show large errors for the incoming radio wave direction.}}
}

@inproceedings{garn2026-PREX-K1KH,
    author = {{Garnier}, P. and {Lamy}, L. and {Jácome}, H. R. P.},
    title = {{Statistical analysis of Jovian decametric radio emissions occurrence drivers}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-K1KH},
    abstract = {{The Jovian decametric (DAM) radio emissions are long-known emissions whose origin is attributed to the cyclotron maser instability, which are produced above the magnetic polar regions of Jupiter.
These emissions are anisotropically beamed, so that the emissions' observation depends on the position of the observer. We revisit here the work by Jácome et al. (2024) who studied the statistical effect of various drivers on the detection occurrence of Jovian DAM emissions, collected since 1990 with the Routine receiver connected to the Nançay Decameter Array. We analyze here the ranking of several drivers (magnetic declination, declination, distance, elongation) based on the DAM emissions occurrence dataset for Io-DAM and non Io-DAM emissions, using statistical approaches dedicated to ranking and disentangling drivers in complex systems.}}
}

@inproceedings{gira2026-PREX-HJJZ,
    author = {{Girard}, J. N. and {Louis}, C. K. and {Zhang}, X. and {Lamy}, L. and {Loh}, A. and {Zarka}, P. and {Santos-Costa}, D. and {N{\'{e}}non}, Q.},
    title = {{Detecting the Jovian Synchrotron Emission at Very Low Frequencies Using NenuFAR}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-HJJZ},
    abstract = {{Jupiter the strongest source of planetary radio emissions in the solar system, it also features a moderate continuum radio emission associated with the radiation of relativistic electrons trapped between 1 and 4 Jovian radii. Above ∼1 GHz, a typical synchrotron spectrum describes the emission, however, due to the fast rotation of the magnetic field and the varying relative position of Earth, short-term, long-term and spatial variability are observed. Below ∼1 GHz, a spectral turnover reduces the intensity of the emission while the associated emitting electron populations also change at a larger radial distance from Jupiter. At decameter wavelengths, the lower part of the synchrotron spectrum can be detected down to 50 MHz with LOFAR (Girard_2016), but it has yet to be validated with a sensitive instrument such as NenuFAR. Below 40 MHz, the decametric emission associated with the cyclotron-MASER instability (CMI) mechanism dominates all other radio emissions at Jupiter during visibility windows. We will study the feasibility of unambiguously detecting the lowest part of the synchrotron emission down to 40 MHz when the CMI emissions are off with tentative NenuFAR imaging of the (unresolved) total intensity of the emission. Data analysis required specific processing for planets and could potentially reveal detection in the Stokes I, Q and U. Detection will give insight into the electron population that undergoes inward diffusion toward the belts and generates synchrotron emission in lower B regions.}}
}

@inproceedings{imai2026-PREX-MZ59,
    author = {{Imai}, M. and {Ono}, T. and {Imai}, K.},
    title = {{Compact Low-Frequency Radio Observatory LWA-Niyodo in Japan}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    doi = {10.25935/PREX-MZ59},
    abstract = {{The low-frequency radio observatories at frequencies below 100 MHz are widely distributed around the world, and some of them operate daily observations of natural radio emissions from the Sun and Jupiter. Continuously monitoring low-frequency radio emissions from these sources requires three separated observatories around the world. Although most of the low-frequency radio observatories are located in Europe and the United States, there are fewer of the observatories in Asia and Oceania. We have built a new compact low-frequency radio observatory in Niyodogawa-cho, Kochi, Japan. The observatory called LWA-Niyodo consists of eight bow-tie antennas (originally designed for the Long Wavelength Array station One in New Mexico, the United States), in which each antenna receives two perpendicular linearly polarized powers. Currently, these signals are combined into two channels using two 8-to-1 analog combiners. With two independent receivers of the Software Defined Radios and Raspberry Pi systems, we have operated the daily observations since March 2024. This receiver is based on Jupiter's radio receiver onboard the KOSEN-1 CubeSat. In this paper, we report the detailed specifications of LWA-Niyodo and highlight some early observations. The LWA-Niyodo data will be shared via the das2 platform (<https://das2.org>) as well as our website at the Institute of Atmospheric Physics of the Czech Academy of Sciences.}},
    pages = {}
}

@inproceedings{kurt2026-PREX-MP08,
    author = {{Kurth}, W. S.},
    title = {{Jupiter Radio Emissions from Juno and Support Observations}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    doi = {10.25935/PREX-MP08},
    abstract = {{Juno has provided the first opportunities to directly sample sources of Jovian auroral radio emissions. In addition to measuring the radio emissions, the supporting plasma observations from the Juno plasma instrument, JADE, have enabled the identification of free energy sources including loss cones, electron conics, and shell distributions. Although studies at Earth have shown these to be unstable to the cyclotron maser instability, they had only been conjectured for Jovian emissions. The Juno observations have also shown the distribution of radio source locations, such as on the equatorward edge of the auroral oval. Juno's polar orbit has also advanced our knowledge of the beaming characteristics of the emissions.  Earth-based observations have also been used to supplement our understanding of the beaming properties.}},
    pages = {}
}

@inproceedings{lamy2026-PREX-MMIF,
    author = {{Lamy}, L. and {Pit}, C. and {Bonfond}, B. and {Tao}, C. and {Benmahi}, B. and {Prang{\'{e}}}, R. and {Gustin}, J.},
    title = {{Mapping the energy of Jovian auroral electrons with HST/STIS from the brightness and color ratios}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-MMIF},
    abstract = {{Far-UV (FUV) spectroscopic observations of the giant planet's aurorae form a rich proxy of their magnetosphere. In this exploratory work, we first compare H_2UV synthetic spectra to check conversion factors used in the literature to infer the total unabsorbed auroral brightness radiated in the H_2 bands. We then process FUV spectroscopic observations of Jupiter from the Space Telescope Imaging Spectrograph (STIS) abord the Hubble Space Telescope (HST) slewing its auroral regions to construct 2D maps of both the H_2 and H-Lyα auroral brightnesses, and in turn of the Brightness Ratio (BR) and of the Color Ratio (CR). BR measures the H-Lyα/H_2 relative emission, and CR the differential emission absorption by hydrocarbons in two H_2 bands. The BR and CR observables are sensitive to electron energies below and beyond a few 10s keV, respectively. They are used to derive complementary maps of the full electron energy spectrum over the entire Jovian auroral region. Such maps are a powerful constraint to the acceleration mechanisms underlying the aurorae.}}
}

@inproceedings{loui2026-PREX-BPTH,
    author = {{Louis}, C. K. and {Marques}, M. S. and {Loh}, A. and {Zarka}, P. and {Mauduit}, E. and {Lamy}, L. and {Girard}, J. N. and {Cecconi}, B.},
    title = {{Lomb–Scargle Analysis of 30 years of Data from the Nançay Decameter Array: Evolution of the Periodicity of Jovian Decametric Emissions}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-BPTH},
    abstract = {{We investigate the long-term evolution of the periodicity of Jupiter's decametric radio emissions over the 1990–2020 period, using data from the Nançay Decameter Array and an extended version of the Marques et al. (2017a)'s catalogue. We apply a Lomb-Scargle analysis to characterize temporal variations in the radio signal's periodicity. The results show that the radio periodicity of Jovian auroral and Io-induced emissions has been stable over 30 years, with variations on an annual scale.}}
}

@inproceedings{loui2026-PREX-VWFQ,
    author = {{Louis}, C. K. and {Boudouma}, A. and {Prang{\'{e}}}, R. and {Girard}, J. N. and {Zarka}, P. and {Lamy}, L. and {Collet}, B. and {Waters}, J. and {Cecconi}, B.},
    title = {{Search for the influence of the Galilean moons on Jovian kilometric and decametric radio emissions over 7 years of Juno data}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-VWFQ},
    abstract = {{The radio emissions generated at Jupiter by the Cyclotron Maser Instability (CMI) are categorized based on their frequency –kilometric, hectometric, or decametric; hectometric and decametric components are relatively continuous, see, e.g., Zarka et al. (2021)– and their origin, whether auroral or induced by the Galilean moons. Regarding the latter category, the moons Io, Europa, and Ganymede are known to influence Jupiter's decametric radio spectrum. Emissions induced by Io have long been observed from Earth in the decametric range and were later confirmed down to the hectometric range by space missions. By contrast, radio signatures from Europa and Ganymede in the hectometric and decametric ranges have only been confirmed recently, through both ground–based and spacecraft observations. However, no clear evidence has yet been found of their influence in the kilometric range. In this study, we present an extended search for radio emissions induced by Europa, Ganymede, and Callisto, using seven years of Juno spacecraft observations. Io's influence on the decametric radio emission is presented for the first time across the full [3.5–40] MHz range and from all latitudes. In the kilometric range, potential influence by the four different Galilean moons is observed for Io (in both hemispheres), Europa (Southern hemisphere), Ganymede (both hemispheres) and Callisto (both hemispheres).}}
}

@inproceedings{litv2026-PREX-ZF77,
    author = {{Litvinenko}, G. and {Ryabov}, V. and {Zakharenko}, V. and {Konovalenko}, A. and {Rothkaehl}, H. and {Ulyanov}, O.},
    title = {{Unusual spectral features in multi-scale spectra of Jovian decameter emission}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    doi = {10.25935/PREX-ZF77},
    abstract = {{We report the detection of intricate fine time-frequency structures and their complex temporal evolution in Jovian sporadic decametric emission (DAM). These patterns are identified in several wideband (WB), narrowband (NB), and mixed WB–NB components observed in high-resolution spectrograms. Their detailed characterization provides new insights into plasma processes in Jupiter's magnetospheric environment, enabling refinement of key plasma parameters and proper selection of models for DAM wave generation. The analyzed waveform data were acquired with the Ukrainian T-shape Radio Telescope (UTR-2) using a baseband digital receiver during an intense Jovian DAM storm on 26^th of November 2009. Spectral images were produced with custom software optimized for multiscale analysis and incorporating various digital filtering techniques to suppress narrowband radio-frequency interference. The resulting WB and NB patterns exhibit complex fine and superfine internal organization, whose principal characteristics are discussed; several features are described here for the first time.}},
    pages = {}
}

@inproceedings{shev2026-PREX-4ZIM,
    author = {{Shevchuk}, M. and {Bubnov}, I. and {Dorovskyy}, V. and {Yerin}, S. and {Konovalenko}, A. and {Reznichenko}, A. and {Stanislavsky}, A. and {Stanislavsky}, L. and {Ulyanov}, O. and {Zakharenko}, V. and {Selin}, V. and {Belov}, A. and {Shevchenko}, V. and {Tokarsky}, P. and {Khristenko}, A. and {Sidorchuk}, M.},
    title = {{Usage of the Solar Energy for the Solar Radio Observations with Mobile Antenna Array}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-4ZIM},
    abstract = {{The first results of solar radio observations with broadband (meter-decameter range) compact mobile quickly-deployable antenna array which can operate autonomously in field conditions, i.e. away of stationary alternating current power network, being powered only by solar energy are presented in the paper. We show that within a relatively short period of time nearly all major types of solar radio bursts (including fine structured ones) were detected proving that 25 element mobile PAA possesses sufficient sensitivity for routine solar observations. The main characteristics of the antenna and the solar power station are also given.}}
}

@inproceedings{stan2026-PREX-77FV,
    author = {{Stanislavsky}, A. A. and {Bubnov}, I. N. and {Stanislavsky}, L. A. and {Zarka}, P. and {Loh}, A. and {Viou}, C. and {Konovalenko}, A. A. and {Vashchishyn}, R. V.},
    title = {{NenuFAR Observations of Scintillation During High Solar Activity}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-77FV},
    abstract = {{We present a reproducible diagnostic framework for detecting interplanetary scintillation (IPS) in low-frequency radio observations of compact sources with the New Extension in Nançay upgrading LOFAR (NenuFAR). Power spectral densities were estimated using Welch's method and partitioned into ionospheric (<0.05 Hz) and interplanetary (0.05–1.0 Hz) bands, with IPS ratios defined as the fraction of power in the latter. Bootstrap resampling provided empirical confidence intervals, while Gaussian fits to autocorrelation functions yielded scintillation timescales via full width at half maximum (FWHM). Applying this chain to multi-channel observations of Cassiopeia A and Cygnus A, we find systematically higher IPS ratios and narrower FWHM for Cas A, with statistically significant separation confirmed by both two-sample t-tests (p = 0.0006) and non-overlapping bootstrap confidence intervals. These results demonstrate that IPS dominates the fast fluctuations in Cas A, while Cyg A serves as a control for ionospheric scintillation. In agreement with Fallows et al. (2020), we acknowledge possible D-region contributions at low frequencies, but our multi-source comparison rules out ionospheric contamination as the sole explanation. The methodology provides a transparent, transferable standard for IPS detection, applicable to other compact sources and coordinated multi-station campaigns.}}
}

@inproceedings{taub2026-PREX-6LGD,
    author = {{Taubenschuss}, U. and {Píša}, D. and {Fischer}, G. and {Imai}, M.},
    title = {{Cassini Direction-Finding
and an application to
Saturn Drifting Bursts}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-6LGD},
    abstract = {{The first part of this study is a review of the basic direction-finding equations on a three-axis stabilized spacecraft, followed by outlining a solution by direct inversion. In the second part, we present first results of direction-finding when applied to Saturn Drifting Burst (SDB) emissions as observed by the Cassini spacecraft at Saturn. This confirms that SDBs have their source locations inside the Enceladus plasma torus, which favors linear or nonlinear mode conversion as a possible generation mechanism, similar to Saturn's narrowband emissions which often occur within the same frequency range.}}
}

@inproceedings{kita2026-PREX-XBQ4,
    author = {{Kita}, H. and {Misawa}, H. and {Tsuchiya}, F. and {Kondo}, T. and {Iwai}, K. and {Takefuji}, K.},
    title = {{Low-frequency VLBI observation with Iitate, Zao, and Toyokawa observatory}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-XBQ4},
    abstract = {{The study demonstrates the first low-frequency VLBI using a compact, disk-based K5/VSSP system with offline FX-type correlation for high-resolution radio astronomy. Using three stations in Japan (Iitate, Zao, and Toyokawa) equipped with K5/VSSP recorders, the team observed the bright calibrator source 3C147 at 327 MHz to test system stability and fringe detection. Successful detection of strong fringes across all baselines confirmed coherent signal synchronization and robust frequency stability, despite ionospheric and radio interference challenges. The use of an offline FX-type software correlator on a general-purpose workstation proved effective for low-frequency data analysis. These results validate the technical readiness of compact, affordable VLBI systems for sub-GHz observations. The experiment lays essential groundwork for future global low-frequency VLBI networks, including collaboration with facilities such as GMRT, to spatially separate stellar and planetary radio emissions and to search for auroral radio bursts from exoplanets.}}
}

@inproceedings{pena2026-PREX-LLH6,
    author = {{Pe\~{n}a-Mo\~{n}ino}, L. P. and {P{\'{e}}rez-Torres}, M.},
    title = {{Exploring Magnetic Star-Planet Interactions in CARMENES targets Using Radio Observations}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-LLH6},
    abstract = {{Magnetic star–planet interaction (SPI) in the sub-Alfvénic regime can channel Poynting flux back to the host star and potentially power highly circularly polarised, time-variable electron–cyclotron maser (ECM) emission. Here we present multi-epoch uGMRT Band 4 observations aimed at searching for SPI-driven emission from nearby CARMENES systems (GJ 806, GJ 436, and CD Cet). Our preliminary results show non-detections for all of these CARMENES systems. We then revisit GJ 486 using the latest public release of our SIRIO code, extending our published uGMRT analysis by (i) exploring a large range of efficiencies in the conversion of Poynting flux into radio emission, β, and stellar mass-loss rates; and (ii) incorporating additional interaction prescriptions and wind/magnetic geometries. The resulting exclusion maps directly show how uGMRT non-detections constrain the allowed combinations of stellar mass-loss rate and β,  and highlight which modelling assumptions dominate the inference.}}
}

@inproceedings{vecc2026-PREX-Z3DL,
    author = {{Vecchio}, A. and {Cecconi}, B. and {Kasaba}, Y. and {Grosset}, L. and {Yasuda}, R. and {Louis}, C. K. and {Tsuchiya}, F. and {Misawa}, H. and {Waters}, J. and {Lamy}, L. and {Wahlund}, J. and {Bergman}, J. E. S. and {Puccio}, W.},
    title = {{JUICE RPWI high-frequency calibration by using solar Type III radio bursts}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-Z3DL},
    abstract = {{The Radio and Plasma Wave Investigation (RPWI) aboard the ESA JUpiter ICy moons Explorer (JUICE) spacecraft is currently en route to Jupiter. This paper exhibits part of the calibration of the high frequency (HF) receiver for RPWI based on observations of solar Type III radio bursts during the August 2024 Lunar-Earth Gravity Assist, using measurements from Wind and PSP missions. In addition, we estimate the instrument sensitivity to Auroral Kilometric Radiation (AKR) for the Earth flybys planned in 2026 and 2029.}}
}

@inproceedings{walk2026-PREX-ZTZA,
    author = {{Walker}, S. and {Jackman}, C. and {Fogg}, A. and {Waters}, J. E.},
    title = {{Technique for treating discrete received power in radio measurements from the RAD1 receiver on board WIND}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-ZTZA},
    abstract = {{The radio instruments within the WIND WAVES suite are widely used to observe terrestrial radio emissions, such as Auroral Kilometric Radiation (AKR), and solar radio bursts. However, instruments like radio receiver band 1 (RAD1) cannot observe multiple frequency channels simultaneously. Common observational modes sweep only a subset of available channels, and even full sweeps leave gaps between channels, resulting in ≈255 kHz of unsampled frequency space. Consequently, visualising and analysing received power as a continuous function of time and frequency requires methods to address these gaps.

We present a simple approach that reconstructs missing frequency information by exploiting the instrument's native sampling cadence (≈ 3 s). Previous studies typically average the received power over a full frequency sweep (≈ 183 s), whereas our method retains variability on timescales constrained by the minimum interval between successive observations of the same frequency channel (≈ 44 s).

We apply this method to one solar Type III radio burst and two AKR events, comparing results with traditional approaches. Our method suggests previously unresolved substructures in AKR, consistent with a potentially bursty extension of the source region along magnetic field lines, and enables clearer separation of partially overlapping solar radio bursts. Integrated power analysis across selected frequency ranges indicates increased temporal variability and improved peak timing, demonstrating the method's advantages beyond visualisation.}}
}