Icarus最新文献

{"title":"Quantifying the force regime of pyrene adsorption on anatase","authors":"N. Kopacz ,&nbsp;H.E. King ,&nbsp;D. Campisi ,&nbsp;A. van Silfhout ,&nbsp;G. Delen ,&nbsp;I.L. ten Kate","doi":"10.1016/j.icarus.2025.116869","DOIUrl":"10.1016/j.icarus.2025.116869","url":null,"abstract":"<div><div>Polycyclic aromatic hydrocarbons (PAHs) are one type of meteoritic organic matter delivered to the surface of Mars. The further chemical evolution of meteoritic PAHs needs to be characterized in order to successfully differentiate between different possible sources of organic molecules detected by Mars rovers, including meteoritic, geological, and potential biological sources. In the ultraviolet regime of Mars, PAHs can be subject to metal-catalyzed degradation mechanisms in the presence of photocatalytic minerals. The efficacy of these mechanisms, however, will depend on the strength of the binding interaction between the PAH and the mineral surface. In this exploratory experimental study, we outline a protocol to characterize the force interactions between the PAH pyrene and an atomically flat mineral surface. The force regime of the adsorption was studied by functionalizing a probe and performing force curve measurements with an atomic force microscope (AFM). The distribution of pyrene on the functionalized probe was mapped with photo-induced force microscopy (PiFM). We produced atomically flat titanium dioxide pellets to obtain force information entirely attributable to the intentional modifications imposed on the probes. In addition we used density functional theory (DFT) to calculate the binding energies of pyrene and titanium dioxide to gain further insight into the nature of the chemical bonds formed in this system. Our method, though it could benefit from a more uniform distribution of pyrene at the surface of the AFM probe, revealed the binding energy between the pyrene molecules and the anatase surface in good agreement with that predicted by DFT calculations.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"446 ","pages":"Article 116869"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145448760","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Numerical simulation of impact cratering and induced seismic waves in sand targets","authors":"Kenji Kurosaki ,&nbsp;Masahiko Arakawa","doi":"10.1016/j.icarus.2025.116874","DOIUrl":"10.1016/j.icarus.2025.116874","url":null,"abstract":"<div><div>Impact cratering plays a crucial role in shaping the surfaces of small bodies, satellites, and planets, providing insights into their formation and the history of the Solar System. Small bodies are often covered with low-cohesion regolith. Using sand as a model of regolith, we constructed a numerical model for simulating impact on a sand target to investigate the mechanisms of crater formation and impact-induced seismic waves. Soda-lime glass and quartz sand targets were used for comparison. The developed sand model successfully reproduced the sound velocity measured in an experimental study. Using the new sand model, the crater formation was simulated using Smoothed Particle Hydrodynamics with a material strength parameter. The crater radius and <span><math><mi>π</mi></math></span>-scaling law derived from the numerical simulation were consistent with the experimental study. The vertical acceleration around the surface of the crater was consistent with the experimentally measured acceleration for the impact-induced seismic wave. The developed model can provide insight for predicting the size of craters on unknown small bodies.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"446 ","pages":"Article 116874"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145464746","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Asteroid phase curve modeling with empirical correction for shape and viewing geometry","authors":"Dagmara Oszkiewicz ,&nbsp;Przemysław Bartczak ,&nbsp;Milagros Colazo ,&nbsp;Antti Penttilä","doi":"10.1016/j.icarus.2025.116886","DOIUrl":"10.1016/j.icarus.2025.116886","url":null,"abstract":"<div><div>We present a novel empirical method for correcting asteroid phase curves for rotational and geometrical effects using precomputed spin-and-shape models. Our approach normalizes sparse photometric data to a pole-on geometry, enabling consistent phase-curve fitting across apparitions. We fit both the <span><math><mrow><mi>H</mi><mo>,</mo><mspace></mspace><msub><mrow><mi>G</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>,</mo><mspace></mspace><msub><mrow><mi>G</mi></mrow><mrow><mn>2</mn></mrow></msub></mrow></math></span> and <span><math><mrow><mi>H</mi><mo>,</mo><mspace></mspace><msub><mrow><mi>G</mi></mrow><mrow><mn>12</mn></mrow></msub></mrow></math></span> phase functions to the normalized data. We also numerically derive new constraints on parameter ranges that ensure physically meaningful solutions. These constraints are based on the requirement that the reduced magnitude must monotonically decrease with phase angle and remain within plausible slope bounds. Compared to earlier bounds, our new constraints are more permissive. We also compare derivative-based and derivative-free optimization methods, highlighting convergence issues with the <span><math><mrow><mi>H</mi><mo>,</mo><mspace></mspace><msub><mrow><mi>G</mi></mrow><mrow><mn>12</mn></mrow></msub></mrow></math></span> function and offering mitigation strategies. We applied our method to over 25,000 asteroids observed by the ATLAS survey, demonstrating its usability. The new method enables the selection of the preferred spin-and-shape solution based on either statistical phase-curve model selection criteria and/or physically motivated constraints on the phase-curve shape.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"446 ","pages":"Article 116886"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145621250","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Influence of albedo, radiation pressure, oblateness, and dust belt on the stability in the generalized elliptic restricted three-body problem","authors":"Bangaru Rama Prasadu,&nbsp;Rajib Mia","doi":"10.1016/j.icarus.2025.116885","DOIUrl":"10.1016/j.icarus.2025.116885","url":null,"abstract":"<div><div>In this paper, we investigate the motion of an infinitesimal body in the framework of the modified elliptic restricted three-body problem by taking into account additional forces due to albedo, radiation pressure, the oblateness of the primaries’ and the dust belt. We obtain semi-analytical solutions of locations for non-collinear equilibrium points. The positions of non-collinear equilibrium points are shown graphically for different values of perturbation parameters. To investigate the motion of the infinitesimal body, we have chosen three real astronomical systems: the Sun–Mars, Proxima Centauri, and Sun–Saturn. The effects of different perturbation parameters on the position of non-collinear equilibrium points are analysed. The linear stability analysis of equilibrium points is performed by computing the critical mass ratio. Our findings indicate that the stability and instability of non-collinear equilibrium points are influenced by the mass ratio and specific perturbation parameters associated with each system.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"446 ","pages":"Article 116885"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145577340","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A dual-branch automatic classification network for lunar simple crater degradation grades integrating image and morphological parameters","authors":"Shuai Shao,&nbsp;Meng Xiao,&nbsp;Zhizhong Kang,&nbsp;Teng Hu,&nbsp;Zhen Cao,&nbsp;Yingnan Zhang,&nbsp;Jinhao Cai,&nbsp;ZhongLu Lei,&nbsp;Haoxiang Hu","doi":"10.1016/j.icarus.2025.116863","DOIUrl":"10.1016/j.icarus.2025.116863","url":null,"abstract":"<div><div>Impact craters represent the most ubiquitous geomorphological feature on the lunar surface. Classifying these craters according to their degradation grades facilitates the analysis of the impact history and evolutionary processes within a given region. Traditional classification methods predominantly rely on manual interpretation, which is inherently limited in scalability for large-scale automation. To address this challenge, we propose a dual-branch automatic classification network for lunar simple crater degradation grades, named LSCDNet, which integrates both image data and morphological parameters. The network leverages DenseNet for feature extraction and employs a Transformer encoder to model the intricate relationships among the morphological parameters of the craters. Dynamic weighting fusion is applied to effectively combine these two feature types. During the training process, the MultiMarginLoss function is utilized to increase class score margins, thereby enhancing the overall classification performance. To evaluate the effectiveness of the proposed method, we construct the Lunar Simple Crater Degradation Grades (LSCD) dataset. Experimental results demonstrate that the proposed method achieves a classification accuracy of 83.12%, precision of 83.00%, recall of 82.36%, and an F1 score of 82.64% on the validation set, indicating strong performance. Moreover, through SHAP-based interpretability analysis, we identify the specific contributions of crater image features and morphological parameters in the model’s decision-making process. Notably, slope of the crater’s outer wall and depth-to-diameter ratio emerge as key factors in distinguishing among different degradation grades. Further analysis reveals that as the degradation grade of craters increases, the morphological parameters exhibit consistent trends, thereby offering deeper insights into the evolutionary process after crater formation. Finally, LSCDNet was applied to different geological unit areas to analyze the distribution of impact crater degradation degrades with variations in geological age, demonstrating that the degradation degree of impact craters has potential dating value.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116863"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145417807","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"How Enceladus’ plume depends on the crevasse wall temperature: An experimental perspective","authors":"Fabrizio Giordano ,&nbsp;Yaël R.A. Bourgeois ,&nbsp;Stéphanie M. Cazaux ,&nbsp;Ferdinand F.J. Schrijer","doi":"10.1016/j.icarus.2025.116842","DOIUrl":"10.1016/j.icarus.2025.116842","url":null,"abstract":"<div><div>In this study, plume experiments were conducted to mimic the thermodynamic conditions on Saturn’s moon, Enceladus. The icy moon’s subsurface ocean and cracks in the surface have been simulated using a liquid water reservoir and a narrow channel, while the low-pressure environment at Enceladus’ surface was achieved with a vacuum chamber. We aimed to examine how channel temperature affected the plume’s temperature, solid fraction and velocity, testing two models with differing wall temperatures: room temperature and near 0 °C. The colder setup better replicated Enceladus’ plume, producing a saturated flow in which nucleation of icy particles is possible. A conservative 1.5%–3% minimum solid fraction is estimated from measurements and modelling. Pitot-tube measurements indicated velocities around 400–500 m/s at the channel outlet. Flow temperature and velocity are closely correlated with wall temperature, indicating effective heat transfer. With a plume model based on the energy conservation law, we concluded that supersonic plume velocities observed on Enceladus cannot be achieved with straight channels, <em>i.e.</em> without requiring extreme expansion ratios. Additionally, the research provides evidence of the relationship between the crevasse’s expansion ratio and the temperatures of flow and crevasse walls.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116842"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145417802","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Characterising the efficiency of the hierarchical clustering method","authors":"Andrew Marshall-Lee ,&nbsp;Apostolos Christou ,&nbsp;Marco Delbo ,&nbsp;Alice Humpage ,&nbsp;Rogerio Deienno ,&nbsp;Kevin Walsh","doi":"10.1016/j.icarus.2025.116862","DOIUrl":"10.1016/j.icarus.2025.116862","url":null,"abstract":"<div><div>The Hierarchical Clustering Method (HCM) is the de-facto clustering algorithm in the search for groups of “family” asteroids that were formed due to the breakup of a larger parent body. In this work, we feed to the HCM a number of synthetic asteroid families at different positions in the main belt and of different dynamical ages. We then measure how effectively the algorithm can recover the family members, while minimising the inclusion of non-family members. The three metrics of “accuracy”, “precision”, and “recall” were used to characterise the HCM efficiency. The most important factor in the HCM’s ability to cluster families was found to be the relative number density between the family and the asteroid background it is situated in. We compared families to the background in a parameter space defined by proper orbital elements semi-major axis, eccentricity, and inclination (a, e, i), and for families approximately four times denser than the background <span><math><mo>∼</mo></math></span> 50% of the original family is recovered independently of age. However, to reach these relative densities for families older than 2 Gyr it was necessary to artificially reduce the synthetic background population. We conclude that older families would be all but undetectable in the real main belt, using the HCM.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116862"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145417803","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Liquid Vein networks as habitats in ice-cemented ground on Earth and Mars: Effects of soil geometry and salts","authors":"H.G. Sizemore ,&nbsp;M.T. Mellon ,&nbsp;A.W. Rempel ,&nbsp;C.P. McKay ,&nbsp;J.L. Heldmann ,&nbsp;C.R. Stoker ,&nbsp;M.R. Perry","doi":"10.1016/j.icarus.2025.116828","DOIUrl":"10.1016/j.icarus.2025.116828","url":null,"abstract":"&lt;div&gt;&lt;div&gt;We have carried out simulations of permafrost liquid fraction to investigate the historical habitability of Martian and Antarctic ground ice. These simulations are based on the development of new soil freezing curves (SFCs) for example Martian and Antarctic soils, and expand upon our previous investigation of the temperature history of shallow Martian ice (Mellon et al., 2024). We considered the effects of salt doping on both soil types, using magnesium perchlorate, Mg(ClO&lt;sub&gt;4&lt;/sub&gt;)&lt;sub&gt;2&lt;/sub&gt;, as an endmember low-eutectic-temperature solute representative of Mars, and NaCl as a high-eutectic-temperature endmember, approximately representative of solutes in the Dry Valleys of Antarctica. We applied our SFCs to calculate the total liquid fraction, &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt;, and maximum liquid vein diameter (or refugia diameter), &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt;, in the icy permafrost under relevant Martian and Antarctic environmental conditions, building on previous work that considered habitability limits in the context of temperature, &lt;em&gt;T&lt;/em&gt;, and water activity, &lt;em&gt;a&lt;/em&gt;&lt;sub&gt;&lt;em&gt;w&lt;/em&gt;&lt;/sub&gt;, only. We defined habitability thresholds of &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; ≥ 5 % and &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; ≥ 1 μm, then examined which of four habitability metrics (&lt;em&gt;T&lt;/em&gt;, &lt;em&gt;a&lt;/em&gt;&lt;sub&gt;&lt;em&gt;w&lt;/em&gt;&lt;/sub&gt;, &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt;, &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt;) presents the dominant limitation to shallow ice habitability in the Martian icy-permafrost environment and in the perennially sub-freezing environments of the Antarctic Dry Valleys. We also re-evaluated optimal landing site selection for Mars life and habitability exploration missions in this context.&lt;/div&gt;&lt;div&gt;We find that, without salts, neither of the examined soils produce habitable values of &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; or &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; below ∼ − 3 °C based on pore-confinement effects alone. The addition of 1 dry wt% NaCl extends the occurrence of habitable values of &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; and &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; to the eutectic temperature of −21 °C; the addition of 1 dry wt% Mg(ClO&lt;sub&gt;4&lt;/sub&gt;)&lt;sub&gt;2&lt;/sub&gt; extends the occurrence of habitable values of &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; and &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; to the magnesium perchlorate eutectic temperature of −64 °C, well below the previously defined extreme metabolic limit of &lt;em&gt;T&lt;/em&gt; = −40 °C. In both the Antarctic Dry Valley and Martian environments solute concentration is spatially variable and can occur locally at more or less than the 1 wt% scenarios we investigated. In the case of localized solute deficits, habitable &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; and &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; may not be achieved, even during summertime and high-obliquity temperature excursions. However, meeting the requirement of &lt;em&gt;d&lt;/em&gt;&lt;sub&gt;&lt;em&gt;r&lt;/em&gt;&lt;/sub&gt; &gt; 1 μm and &lt;em&gt;S&lt;/em&gt;&lt;sub&gt;&lt;em&gt;l&lt;/em&gt;&lt;/sub&gt; &gt; 5 % is surprisingly easy for silty to sandy soil","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116828"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462599","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A new method to improve the detection rate and astrometric accuracy of natural satellites located in the halo of Uranus","authors":"Z.Y. Wang ,&nbsp;H.Y. Zhang ,&nbsp;R.C. Qiao ,&nbsp;Y. Yu ,&nbsp;D. Yan ,&nbsp;K. Tang","doi":"10.1016/j.icarus.2025.116867","DOIUrl":"10.1016/j.icarus.2025.116867","url":null,"abstract":"<div><div>With the rapid development of deep-space exploration within the Solar System, the demand for precise ephemerides of planets and their natural satellites is growing steadily. Continuous updating of these ephemerides relies on long-term observational data, and ground-based observations play a vital role in improving ephemeris accuracy. However, the bright halos surrounding planets can reduce both the detection rate and the positional accuracy of their nearby satellites. To address this issue, we conducted a comparative study of two image-enhancement methods using 1030 CCD images of Uranus and its neighboring satellites obtained at Yunnan Observatory from 13 to 18 November 2020. The results demonstrate that a regularized Retinex algorithm effectively removes the halo and significantly improves the detection rate and positional accuracy of Uranian satellites. Stellar positions in this study are taken from Gaia DR3, Uranus positions from DE441, and the positions of Uranian satellites from Lainey et al. (2015).</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116867"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462556","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Electrostatic ion-cyclotron higher harmonic instability with latitudinal variation of magnetic field & inhomogeneous electric field in Jupiter’s magnetosphere","authors":"A.K. Dhaikar,&nbsp;R.S. Pandey","doi":"10.1016/j.icarus.2025.116858","DOIUrl":"10.1016/j.icarus.2025.116858","url":null,"abstract":"<div><div>This research explores kinetic approach for electrostatic ion-cyclotron instabilities related to higher harmonic modes (<span><math><mi>n</mi><mo>≥</mo><mn>1</mn></math></span>) in Jupiter's magnetosphere at radial distances of 10 and 15 Jupiter radii (R_J). We include the effects of Bessel functions of orders 1 and 2 for the fundamental (<em>n</em> = 1) and first higher harmonic (<em>n</em> = 2) modes. With a kinetic treatment and the method of characteristics solution, we obtain an altered dispersion relation that includes finite Larmor radius effects and latitude-variable magnetic field, described as <span><math><mi>B</mi><mo>=</mo><msub><mi>B</mi><mn>0</mn></msub><msqrt><mrow><mn>1</mn><mo>+</mo><mn>3</mn><msup><mi>sin</mi><mn>2</mn></msup><msub><mi>θ</mi><mi>mag</mi></msub></mrow></msqrt><mo>/</mo><msup><mi>cos</mi><mn>6</mn></msup><msub><mi>θ</mi><mi>mag</mi></msub></math></span>. We analyze the effects of various plasma parameters such as electric field inhomogeneity, velocity shear scale length, temperature anisotropy, magnitude of electric field, electron-to-ion temperature ratio, density gradient, and propagation angle on the dimensionless growth rate of these instabilities as a function of <span><math><msub><mi>k</mi><mo>⊥</mo></msub><msub><mi>ρ</mi><mi>i</mi></msub></math></span>. Numerical calculations, corroborated by the Galileo and Juno mission data, demonstrate disparate behaviors between the basic (<em>n</em> = 1) and higher harmonic (<em>n</em> = 2) modes. Higher growth rates are found for the fundamental modes, while the higher harmonics are more sensitive to smaller-scale structures. These results highlight the significance of kinetic effects in plasma transport, wave excitation, and auroral activity in Jupiter's fast-rotating, corotation-dominated magnetosphere.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"445 ","pages":"Article 116858"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145462682","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}