IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-12 DOI: 10.1016/j.icarus.2024.116299

A. Cousin , P.-Y. Meslin , O. Forni , O. Beyssac , E. Clavé , E. Hausrath , P. Beck , E. Dehouck , S. Schröder , T. Fouchet , C. Bedford , J. Johnson , P. Pilleri , J. Lasue , O. Gasnault , N. Martin , B. Chide , A. Udry , R. Sullivan , A. Vaughan , R.C. Wiens

{"title":"Soil diversity at Jezero crater and Comparison to Gale crater, Mars","authors":"A. Cousin , P.-Y. Meslin , O. Forni , O. Beyssac , E. Clavé , E. Hausrath , P. Beck , E. Dehouck , S. Schröder , T. Fouchet , C. Bedford , J. Johnson , P. Pilleri , J. Lasue , O. Gasnault , N. Martin , B. Chide , A. Udry , R. Sullivan , A. Vaughan , R.C. Wiens","doi":"10.1016/j.icarus.2024.116299","DOIUrl":"10.1016/j.icarus.2024.116299","url":null,"abstract":"<div><p>The martian soil is of particular interest as it can help us understand the different processes that have occurred on Mars by studying the chemistry and mineralogy of its constituents as a function of grain size. The fine-grained martian soil is thought to be homogeneous across the planet and thus to represent a global component. In this study we report on the soil targets analysed by the SuperCam instrument aboard the Perseverance rover, which is currently exploring Jezero crater. A total of 343 targets were analysed. Their grain size distribution confirms the sparsity of 250–900 Â<span><math><mrow><mi>μ</mi><mi>m</mi></mrow></math></span> particles in the martian soil, although both smaller and larger grains are present. We found that the local components, due to erosion of the local bedrock, are present not only in the very coarse grains or larger gravels of the soil, but also in the very fine ones (¡250 Â<span><math><mrow><mi>μ</mi><mi>m</mi></mrow></math></span>). We detected some very coarse grains enriched in olivine, pyroxene and carbonate in both the crater floor and the delta front locations, whereas phyllosilicate-rich grains have been encountered only in the delta front. We have compared the Jezero fine-grained soil targets with those of Gale crater using ChemCam data. We found that those at Jezero show no evidence of Mg sulfates, in contrast to the observation at Gale. In addition, the fine-grained soil at Jezero is more hydrated than that at Gale, probably due to its higher specific surface area.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116299"},"PeriodicalIF":2.5,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003592/pdfft?md5=fe395084f17bb0dbed650b8020c8a776&pid=1-s2.0-S0019103524003592-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142239428","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Preface: Ices in the Solar system; origin, evolution and distribution 前言太阳系的冰；起源、演变和分布

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-12 DOI: 10.1016/j.icarus.2024.116303

James B. Garvin , Richard J. Soare

引用次数: 0

The diurnal variation of dust and water ice aerosol optical depth at Jezero crater observed by MEDA/TIRS over a full Martian year MEDA/TIRS 观测到的杰泽罗陨石坑全年火星尘埃和水冰气溶胶光学深度的昼夜变化

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-12 DOI: 10.1016/j.icarus.2024.116313

Michael D. Smith , Germán M. Martínez , Eduardo Sebastián , Mark T. Lemmon , Samuel A. Atwood , Daniel Toledo , Daniel Viúdez-Moreiras , Aurélien Stcherbinine , Jose Antonio Rodriguez-Manfredi , Manuel de la Torre Juárez

{"title":"The diurnal variation of dust and water ice aerosol optical depth at Jezero crater observed by MEDA/TIRS over a full Martian year","authors":"Michael D. Smith , Germán M. Martínez , Eduardo Sebastián , Mark T. Lemmon , Samuel A. Atwood , Daniel Toledo , Daniel Viúdez-Moreiras , Aurélien Stcherbinine , Jose Antonio Rodriguez-Manfredi , Manuel de la Torre Juárez","doi":"10.1016/j.icarus.2024.116313","DOIUrl":"10.1016/j.icarus.2024.116313","url":null,"abstract":"<div><p>The Thermal InfraRed Sensor (TIRS) on the Perseverance rover has provided nearly two full Mars years of systematic monitoring of the total aerosol optical depth above Jezero Crater. These observations span a wide range of timescales, capturing seasonal patterns, diurnal variations, and minute-to-minute fluctuations in aerosol loading. By combining TIRS retrievals with orbital observations, the relative contributions of dust and water ice aerosols can be estimated, revealing their different seasonal and diurnal behaviors. The TIRS record shows distinct periods of dust storm activity, including strong regional storms during the perihelion season as well as short-lived but intense dust events outside the typical dust storm season. Water ice clouds exhibit pronounced seasonal and diurnal variability, with peak activity occurring during the aphelion season but with a presence throughout the year. The diurnal variation of clouds differs significantly between the aphelion and perihelion seasons, with clouds persisting throughout the night during the aphelion season, while largely absent outside of specific periods after sunrise and sunset during the perihelion season. These results provide new insights into the complex behavior of aerosols at Jezero Crater and their connections to atmospheric dynamics and the Martian dust and water cycles.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116313"},"PeriodicalIF":2.5,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142239426","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}

引用次数: 0

Global climate modelling of Saturn’s atmosphere, Part V: Large-scale vortices 土星大气层全球气候建模，第五部分：大尺度涡旋

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-07 DOI: 10.1016/j.icarus.2024.116302

Padraig T. Donnelly , Aymeric Spiga , Sandrine Guerlet , Matt K. James , Deborah Bardet

{"title":"Global climate modelling of Saturn’s atmosphere, Part V: Large-scale vortices","authors":"Padraig T. Donnelly , Aymeric Spiga , Sandrine Guerlet , Matt K. James , Deborah Bardet","doi":"10.1016/j.icarus.2024.116302","DOIUrl":"10.1016/j.icarus.2024.116302","url":null,"abstract":"<div><p>This paper presents an analysis of large-scale vortices in the atmospheres of gas giants, focusing on a detailed study conducted using the Saturn-DYNAMICO global climate model (GCM). Large-scale vortices, a prominent feature of gas giant atmospheres, play a critical role in their atmospheric dynamics. By employing three distinct methods – manual detection, machine learning via artificial neural networks (ANN), and dynamical detection using the Automated Eddy-Detection Algorithm (AMEDA) – we characterise the spatial, temporal, and dynamical properties of these vortices within the Saturn-DYNAMICO GCM. Our findings reveal a consistent production of vortices due to well-resolved eddy-to-mean flow interactions, exhibiting size and intensity distributions broadly in agreement with observational data. However, notable differences in vortex location, size, and concentration highlight the model’s limitations and suggest areas for further refinement. The analysis underscores the importance of zonal wind conditions in influencing vortex characteristics and suggests that more accurate modelling of giant planet vortices may require improved representation of moist convection and jet structure. This study not only provides insights into the dynamics of Saturn’s atmosphere as simulated by the GCM but also offers a framework for comparing vortex characteristics across observations and models of planetary atmospheres.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116302"},"PeriodicalIF":2.5,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003622/pdfft?md5=a06038aec5672d68278236e3e8477e07&pid=1-s2.0-S0019103524003622-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142230323","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Geometrical model of jets in cometary comae 彗星彗尾喷流的几何模型

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-05 DOI: 10.1016/j.icarus.2024.116300

Valerii Kleshchonok , Holger Sierks

{"title":"Geometrical model of jets in cometary comae","authors":"Valerii Kleshchonok , Holger Sierks","doi":"10.1016/j.icarus.2024.116300","DOIUrl":"10.1016/j.icarus.2024.116300","url":null,"abstract":"<div><p>Cometary comae frequently exhibit various formations such as jets, fans, and shells, which can provide crucial insights into the nuclear rotation parameters and the presence of active regions on cometary nuclei. To accurately interpret the visible shape of these jets, a geometric model has been developed. This model considers several factors, including the position of the comet nucleus’s axis of rotation, the location of active areas on the comet’s surface, the angular size of the emission cone, and the relative positions of the Earth, the Sun, and the comet. Utilizing this model, it is possible to track the evolution of the jets over extended periods, enhancing the precision of the model parameters estimation through its simplification. Application of the geometrical model is demonstrated in determining the rotational parameters of the nucleus of comet C/2017 K2 (PANSTARRS). The coordinates for the positive pole of the rotational axis of the comet’s nucleus are: right ascension <span><math><mrow><mi>α</mi><mo>=</mo><mn>70</mn><mo>°</mo><mo>±</mo><mn>15</mn><mo>°</mo></mrow></math></span>, declination <span><math><mrow><mi>δ</mi><mo>=</mo><mo>−</mo><mn>45</mn><mo>°</mo><mo>±</mo><mn>6</mn><mo>°</mo></mrow></math></span>, and the rotation period is 166.50 ± 0.02 h. The shape of the jet feature is consistent with an active area located at that latitude <span><math><mrow><mi>ϕ</mi><mo>=</mo><mo>+</mo><mn>45</mn><mo>°</mo><mo>±</mo><mn>6</mn><mo>°</mo></mrow></math></span>. The mean velocity of the dust particles is calculated to be 0.23 ± 0.03 km/s.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116300"},"PeriodicalIF":2.5,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142151777","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}

引用次数: 0

Corrigendum to “Polyphase tectonics on Mars: Insight from the Claritas Fossae” [Icarus 411 (15 March 2024) 115972] 火星上的多相构造：来自克拉里塔斯化石群的启示》更正[伊卡洛斯411（2024年3月15日）115972]

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-05 DOI: 10.1016/j.icarus.2024.116287

Evandro Balbi , Gabriele Ferretti , Silvano Tosi , Laura Crispini , Paola Cianfarra

引用次数: 0

Major brightening events in Jupiter’s sodium nebula during Juno era 朱诺时代木星钠星云的主要增亮事件

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-04 DOI: 10.1016/j.icarus.2024.116301

M. Yoneda , F. Tsuchiya , C. Schmidt , M. Kagitani , T. Sakanoi

{"title":"Major brightening events in Jupiter’s sodium nebula during Juno era","authors":"M. Yoneda , F. Tsuchiya , C. Schmidt , M. Kagitani , T. Sakanoi","doi":"10.1016/j.icarus.2024.116301","DOIUrl":"10.1016/j.icarus.2024.116301","url":null,"abstract":"<div><p>Successive observations of Jupiter’s sodium nebula have identified several brightening events, presumably due to variability in Io’s volcanic plumes. An event that began in the beginning of March 2018 has been already reported by Morgenthaler et al. (2019,2024a,2024b). In this work, we found that this event was followed by another one. By adding these observations, details of these events including one observed by Morgenthaler et al. (2019,2024a,2024b) are described herein. Especially, the event in 2018 seems to have been the strongest enhancement during Juno spacecraft’s orbital mission, at least before 2020. Also, our observations show that the D-line brightness of the sodium nebula was decreasing in early September, 2019. This tendency is consistent with Io’s volcanic plume activity observed by Atacama Large (sub)Millimeter Array (ALMA). The KCl gas observed in this plume with ALMA is a chemical analog of NaCl, which is believed to be the parent molecule that dissociates to form the sodium nebula. While these observations are not the direct evidence of plume supply to sodium nebula, they are suggestive of control of Io’s volcanic plumes on the brightness of Jupiter’s sodium nebula.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116301"},"PeriodicalIF":2.5,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003610/pdfft?md5=d160c29dbf39ac042be80f1a26f94066&pid=1-s2.0-S0019103524003610-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142169268","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Methane storm characteristics and evolution in simulations of Titan’s hydroclimate 土卫六水文气候模拟中的甲烷风暴特征和演变

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-03 DOI: 10.1016/j.icarus.2024.116290

Ethan Olim, Juan M. Lora, J. Michael Battalio

{"title":"Methane storm characteristics and evolution in simulations of Titan’s hydroclimate","authors":"Ethan Olim, Juan M. Lora, J. Michael Battalio","doi":"10.1016/j.icarus.2024.116290","DOIUrl":"10.1016/j.icarus.2024.116290","url":null,"abstract":"<div><p>Methane precipitation is a key component of the climate on Titan, and has been shown to impact surface features. Recent general circulation models (GCMs) have reproduced Titan’s hydroclimate, including precipitation, with increasing accuracy, yet characterization of their simulated precipitation events is lacking. We investigate the characteristics and evolution of methane storms simulated over 40 Titan years using the Titan Atmospheric Model, a validated GCM. Storms are identified and tracked using the density-based spatial clustering of applications with noise (DBSCAN) algorithm, allowing them to be followed through time and space. We find that storms follow seasonality expected from observations and prior modeling, occur preferentially in the summer hemisphere, and tend to start over high topography. The population of storms is bimodal in traits corresponding to intensity, area, and duration, with a large population of small, short-lived, and weakly precipitating storms and a smaller population of exceptionally large, long-lasting, and intense storms. These largest storms tend to evolve similarly over their lifetimes, peaking early in intensity and in the middle of their lives in area. We also find temporal clustering of storms, in alignment with observations and the proposed relaxation-oscillation model of Titan’s methane precipitation. These storm clusters emerge quasi-periodically following long dry spells during which evaporation of surface methane recharges atmospheric moisture. Approximately five clusters occur per Titan year, and their locations are strongly seasonal. Overall, our quantitative descriptions of storms and storm clusters over a long timescale provide additional insight into Titan’s methane cycle and surface features, and may assist in the planning of future missions such as <em>Dragonfly</em>.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116290"},"PeriodicalIF":2.5,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142151776","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}

引用次数: 0

Corrigendum to “The interaction of deep convection with the general circulation in Titan’s atmosphere, Part II: Impacts on the climate” "深层对流与土卫六大气总环流的相互作用，第二部分：对气候的影响 "的更正

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-09-02 DOI: 10.1016/j.icarus.2024.116264

J. Michael Battalio , Juan M. Lora , Scot Rafkin , Alejandro Soto

引用次数: 0

Rock thermal conductivity and thermal inertia measurements under martian atmospheric pressures 火星大气压力下的岩石导热性和热惯性测量

IF 2.5 2区物理与天体物理

Icarus Pub Date : 2024-08-30 DOI: 10.1016/j.icarus.2024.116272

A.A. Ahern , A.D. Rogers , R.J. Macke , S.A. Mertzman , K.R. Mertzman , B.J. Thomson , R.E. Kronyak , G.M. Peters , E.L. Carey , R.J. Hopkins

{"title":"Rock thermal conductivity and thermal inertia measurements under martian atmospheric pressures","authors":"A.A. Ahern , A.D. Rogers , R.J. Macke , S.A. Mertzman , K.R. Mertzman , B.J. Thomson , R.E. Kronyak , G.M. Peters , E.L. Carey , R.J. Hopkins","doi":"10.1016/j.icarus.2024.116272","DOIUrl":"10.1016/j.icarus.2024.116272","url":null,"abstract":"<div><p>The physical properties of rocks on planetary surfaces influence their bulk thermal conductivity (<em>k</em>) and thermal inertia (<em>TI</em>); however, there has been little work done to date to explore quantitative relationships between physical properties (bulk density, porosity, mechanical strength) and thermal properties (<em>k</em> and <em>TI</em>) at Mars-relevant pressures. We present the first <em>k</em> and <em>TI</em> measurements of a comprehensive suite of Mars-relevant igneous and sedimentary rocks under Mars atmospheric pressures. We used modified transient plane source (MTPS) and transient plane source (TPS) methods to measure <em>k</em> and <em>TI</em> values of 40 samples (3 monomineralic, 13 igneous, 24 sedimentary) at pressures between 1 and 10 mbar and at 1 bar, at ∼25 °C. The rock samples were characterized by bulk density, grain density, porosity, uniaxial compressive strength, mineralogy, and major and trace element abundances. We find that bulk density and porosity roughly correlate to <em>k</em> and <em>TI</em> values at Mars pressures by power law relationships. The relationships of the thermal properties with mechanical strength and chemical properties, however, are not straightforward. Many physical and chemical factors play a role in determining <em>k</em> and <em>TI</em> values; thus, it is not possible to relate a single physical or chemical property to <em>k</em> and <em>TI</em> directly based on these measurements. Rock <em>TI</em> values derived from rover surface temperature measurements on Mars agree with our results for similar rock types.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116272"},"PeriodicalIF":2.5,"publicationDate":"2024-08-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142162315","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}

引用次数: 0

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