Icarus最新文献

{"title":"Dynamical evolution of the Uranian satellite system I.","authors":"Sérgio R.A. Gomes ,&nbsp;Alexandre C.M. Correia","doi":"10.1016/j.icarus.2024.116282","DOIUrl":"10.1016/j.icarus.2024.116282","url":null,"abstract":"<div><p>Mutual gravitational interactions between the five major Uranian satellites raise small quasi-periodic fluctuations on their orbital elements. At the same time, tidal interactions between the satellites and the planet induce a slow outward drift of the orbits, while damping the eccentricities and the inclinations. In this paper, we revisit the current and near past evolution of this system using a <span><math><mrow><mi>N</mi><mo>−</mo></mrow></math></span>body integrator, including spin evolution and tidal dissipation with the weak friction model. We update the secular eigenmodes of the system and show that it is unlikely that any of the main satellites were recently captured into a high obliquity Cassini state. We rather expect that the Uranian satellites are in a low obliquity Cassini state and compute their values. We also estimate the current variations in the eccentricities and inclinations, and show that they are not fully damped. We constrain the modified quality factor of Uranus to be <span><math><mrow><msubsup><mrow><mi>Q</mi></mrow><mrow><mi>U</mi></mrow><mrow><mo>′</mo></mrow></msubsup><mo>=</mo><mrow><mo>(</mo><mn>1</mn><mo>.</mo><mn>2</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>4</mn><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>5</mn></mrow></msup></mrow></math></span>, and that of Ariel to be <span><math><mrow><msubsup><mrow><mi>Q</mi></mrow><mrow><mi>A</mi></mrow><mrow><mo>′</mo></mrow></msubsup><mo>=</mo><mrow><mo>(</mo><mn>7</mn><mo>±</mo><mn>3</mn><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>4</mn></mrow></msup></mrow></math></span>. We find that the system most likely encountered the 5/3 mean motion resonance between Ariel and Umbriel in the past, at about <span><math><mrow><mo>(</mo><mn>0</mn><mo>.</mo><mn>7</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>2</mn><mo>)</mo></mrow></math></span> Gyr ago. We additionally determine the eccentricities and inclinations of all satellites just after the resonance passage that comply with the current system. We finally show that, from the crossing of the 5/3 MMR to the present, the evolution of the system is mostly peaceful and dominated by tides raised on Uranus by the satellites.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116282"},"PeriodicalIF":2.5,"publicationDate":"2024-08-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003427/pdfft?md5=67d5833993d4db688b503b98b01d594d&pid=1-s2.0-S0019103524003427-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142152016","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}

{"title":"New gravity field of comet 67P/C-G based on Rosetta’s Doppler and optical data","authors":"Julien Laurent-Varin ,&nbsp;Théo James ,&nbsp;Jean-Charles Marty ,&nbsp;Laurent Jorda ,&nbsp;Sebastien Le Maistre ,&nbsp;Robert Gaskell","doi":"10.1016/j.icarus.2024.116284","DOIUrl":"10.1016/j.icarus.2024.116284","url":null,"abstract":"<div><p>The gravity field of a celestial body gives valuable insights into its fundamental properties such as its density and internal structure. The Doppler data collected by the Radio-Science Investigation (RSI) experiment of the Rosetta mission were previously used to determine the gravity field of comet 67P/Churyumov–Gerasimenko up to degree 2 (Pätzold et al., 2016). In the present study we re-estimate the gravity field of 67P/C-G using not only RSI data as before, but also images data from Rosetta’s OSIRIS camera. These data, converted into “landmark” observations, are complementary to RSI data. Therefore, the analysis of combined Doppler and optical data results in a significant improvement in the restitution of Rosetta’s orbit and the determination of the comet gravity field with respect to previous work. Some coefficients of the comet’s gravity field are now resolved up to degree 4. The mass and low degrees estimates are in fairly good agreement with those previously published, but the improvement in their accuracy (i.e. lower sigmas) as well as the better resolution (i.e. maximum degree) of the new gravity field suggests that the distribution of mass in the nucleus may not be uniform, contrary to what was previously thought. Moreover, we estimate a change in the mass of the comet attributed to ice sublimation at its orbital perihelion that is almost three times greater than that previously published. The new estimated mass loss is <span><math><mrow><mi>Δ</mi><mi>M</mi><mo>=</mo><mn>28</mn><mo>.</mo><mn>0</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>29</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>9</mn></mrow></msup><mspace></mspace><mi>kg</mi></mrow></math></span>, corresponding to 0.28% of the total mass of the comet. Thanks to a precise determination of the degree-1 gravity coefficients, we observe for the first time a motion of the center of mass of the comet by <span><math><mrow><mo>∼</mo><mn>35</mn><mspace></mspace><mi>m</mi></mrow></math></span> northward that could be explained by a more pronounced outgassing activity in the south of the comet due to the orientation of its spin axis relative to the Sun. The temporal evolution (before versus after perihelion) of the other estimated gravity coefficients and in particular degree-2 is more modest (0.8% for <span><math><msub><mrow><mi>C</mi></mrow><mrow><mn>20</mn></mrow></msub></math></span> and 2% for <span><math><msub><mrow><mi>C</mi></mrow><mrow><mn>22</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>S</mi></mrow><mrow><mn>22</mn></mrow></msub></math></span>).</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116284"},"PeriodicalIF":2.5,"publicationDate":"2024-08-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142151909","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":"Evidence of a Martian spatter cone south of Pavonis Mons","authors":"Ian T.W. Flynn ,&nbsp;Erika Rader","doi":"10.1016/j.icarus.2024.116286","DOIUrl":"10.1016/j.icarus.2024.116286","url":null,"abstract":"<div><p>Spatter cones are a common mafic explosive volcanic feature observed on Earth associated with Hawaiian and Strombolian-style lava fountaining. Across Mars there are numerous explosive volcanic features assessed to be accumulations of cold pyroclasts (e.g., scoria cones, tuff rings) but identification of welded and fused explosive deposits (i.e., spatter) has only recently been investigated. We present evidence indicating the presence of a Martian spatter cone south of Pavonis Mons and a comparison to a spatter cone formed during the 2021 Fagradalsfjall eruption, Iceland. The morphology and morphometry of the possible Martian spatter cone are more consistent with agglutinated rock like the spatter cone formed during the Fagradalsfjall eruption than poorly consolidated tephra, characteristic of scoria cones. In addition, the size of the two spatter cones falls within anticipated dimensions based on a simple ballistic trajectory model. Evidence for spatter included high angled slopes, knobby yet layered surface textures, rounded boulder talus, and thermophysical properties consistent with material that is more indicative of rock than scoria. The evidence indicates that the volcanic feature South of Pavonis Mons should be classified as a spatter cone. Identification of a Martian spatter cone has implications for eruption dynamics, magmatic volatile content, and environmental conditions.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116286"},"PeriodicalIF":2.5,"publicationDate":"2024-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003464/pdfft?md5=75d7e7702bddf8ff8a471d18abbbc5fe&pid=1-s2.0-S0019103524003464-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142095070","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}

{"title":"Identification and preliminary characterisation of signals recorded by instrument for lunar seismic activity at the Chandrayaan 3 landing site","authors":"J. John,&nbsp;V. Thamarai,&nbsp;Teena Choudhary,&nbsp;M.N. Srinivasa,&nbsp;Ashwini Jambhalikar,&nbsp;M.S. Giridhar,&nbsp;Madan Mohan Mehra,&nbsp;Mayank Garg,&nbsp;K.V. Shila,&nbsp;Krishna Kummari,&nbsp;S.P. Karantha,&nbsp;Kalpana Arvind,&nbsp;K.V. Sriram","doi":"10.1016/j.icarus.2024.116285","DOIUrl":"10.1016/j.icarus.2024.116285","url":null,"abstract":"<div><p>The science objective of the Instrument for Lunar Seismic Activity (ILSA) is to study the seismicity at the landing site of the Indian lunar mission, the Chandrayaan 3. It also aimed at demonstrating the capability of devices based on silicon micromachining technology to survive and operate in planetary missions and environments. The Chandrayaan 3 mission had a lander and a rover together carrying five different scientific instruments. ILSA was placed on the lunar surface and had six accelerometers in it. It was operated during the lunar day from 24 August 2023 to 4 September 2023. This paper presents the summary of observations made on 190 h of data recorded by ILSA. We have identified more than 250 distinct signals of which about 200 signals are correlated to known activities involving the physical movements of the rover or the operation of science instruments. This paper presents our approach in the preliminary characterisation and cataloguing of the events based on their temporal properties and spectral contents. It will also act a guide for the future researchers to search, identify and analyse the records made by ILSA.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116285"},"PeriodicalIF":2.5,"publicationDate":"2024-08-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142122404","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":"Moisture cycles in Jezero crater, Mars","authors":"Hannu Savijärvi ,&nbsp;Jouni Polkko ,&nbsp;Maria Hieta ,&nbsp;German Martinez ,&nbsp;Maria-Paz Zorzano ,&nbsp;Leslie Tamppari ,&nbsp;Ari-Matti Harri","doi":"10.1016/j.icarus.2024.116283","DOIUrl":"10.1016/j.icarus.2024.116283","url":null,"abstract":"<div><p>Diurnal and annual water cycles are studied during the first year of Perseverance rover in Jezero, using observations from the Mars Environmental Dynamics Analyzer (MEDA) and column modeling. Areal values for the ground thermal inertia (TI) and albedo are first found at one site by fitting model temperatures to the observed air temperatures. Areal soil porosity and the initial water vapor volume mixing ratios (vmr) are next found via model-vmr fits to the observation-based vmr. The meteorology and physics of the modeled air and subsurface diurnal moisture cycle at the site is then discussed in detail. The process of fit to observations is finally extended to fourteen sites along the Perseverance track, resulting in estimates for areal TI, albedo and porosity at these sites, and in MEDA-based initial estimates for the annual and diurnal moisture cycles at Jezero during MY36.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"423 ","pages":"Article 116283"},"PeriodicalIF":2.5,"publicationDate":"2024-08-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142097791","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":"Site selection for the second Flyeye telescope: A simulation study for optimizing near-earth object discovery","authors":"D. Föhring ,&nbsp;L. Conversi ,&nbsp;M. Micheli ,&nbsp;E. Dölling ,&nbsp;P. Ramirez Moreta","doi":"10.1016/j.icarus.2024.116281","DOIUrl":"10.1016/j.icarus.2024.116281","url":null,"abstract":"<div><p>The European Space Agency (ESA) is developing a network of wide-field survey telescopes, named Flyeye, to improve the discovery of Near-Earth Objects (NEOs). The first telescope in the network will be located in the Northern Hemisphere on Mount Mufara (Italy), and a second Flyeye telescope, featuring increased detection capabilities, has just started the critical design phase.</p><p>The potential location for the second Flyeye telescope is investigated by performing simulations of NEOs on impacting trajectories. Approximately 3000 impacting asteroids of two absolute magnitudes (H = 25 and H = 28) were propagated and tested for detectability by major existing surveys (Catalina, Pan-STARRS, ATLAS), the upcoming Vera Rubin Observatory (LSST), and possible Flyeye locations. Chile, South Africa, and a second facility in the Northern Hemisphere were considered. For each observatory, their past or planned pointing strategies were taken into account in the simulation.</p><p>Before LSST deployment, a single Flyeye in the Southern Hemisphere performs similarly to a telescope in the Northern Hemisphere. When combined, having one telescope in the north and one in the south maximizes detections and number of unique objects detected. After LSST, southern and northern Flyeye telescopes remain complementary. Overall, simulations show that a second Flyeye in the south complements a Flyeye telescope in the north both before and after LSST. A Flyeye located at La Silla would take advantage of the excellent atmospheric conditions, while allowing a balance of assets across hemispheres.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116281"},"PeriodicalIF":2.5,"publicationDate":"2024-08-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142151940","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":"Albedo analysis of dust devil-induced slope streaks and tracks on Mars","authors":"T. Heyer ,&nbsp;J. Raack ,&nbsp;W. Iqbal ,&nbsp;H. Hiesinger ,&nbsp;A. Oetting","doi":"10.1016/j.icarus.2024.116270","DOIUrl":"10.1016/j.icarus.2024.116270","url":null,"abstract":"<div><p>Despite frequent observations of slope streaks and dust devil tracks on the same slopes in various regions on Mars, only a few instances in Arabia Terra have documented slope streaks directly triggered by dust devils. Here we present new observations of dust devil-induced slope streaks in Elysium Planitia and Amazonis Planitia. These observations represent a rare opportunity to study the erosional effects of both dust devils and slope streaks on the martian surface. Since dust devil tracks and the triggered streaks are formed basically simultaneously and are therefore subject to similar alteration processes, e.g., settling dust from the atmosphere, the relative albedo of these features can be determined using high-resolution orbital images. Our relative albedo analyses of twelve dust devil-induced slope streaks revealed that slope streaks appear substantially darker than the respective dust devil tracks. These observations might indicate a stronger erosion of fine-grained material by slope streaks compared to dust devils.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"423 ","pages":"Article 116270"},"PeriodicalIF":2.5,"publicationDate":"2024-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003300/pdfft?md5=5c507fa8df7b22ab7621525c0c43cbc8&pid=1-s2.0-S0019103524003300-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142049713","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}

{"title":"Characterization of the M1 and M2 layers in the undisturbed Martian ionosphere at a variety of solar conditions with MAVEN ROSE","authors":"Jennifer Segale ,&nbsp;Marianna Felici ,&nbsp;Paul Withers ,&nbsp;Shannon Curry","doi":"10.1016/j.icarus.2024.116251","DOIUrl":"10.1016/j.icarus.2024.116251","url":null,"abstract":"<div><p>We utilize data from the MAVEN Radio Occultation Science Experiment (<span><span>Withers et al., 2020</span></span>) - with unprecedented coverage in solar zenith angle - to isolate the effects that local time and season induce on the photochemical ionosphere of Mars around solar minimum, leading to solar maximum. 185 out of the 1228 electron density profiles of the Martian undisturbed ionosphere collected by MAVEN ROSE between July 2016 and December 2022 show a distinct M1 layer below the M2 layer. We define undisturbed here as conditions when there are no solar events or dust storms to influence the ionosphere. This allowed us to study the behavior of both the M2 and M1 peak densities and altitudes as a function of solar zenith angle, and, for the first time, to be able to separate these trends by dusk and dawn local time, as well as by southern spring and summer versus southern fall and winter. We find that the M1 layer at small SZA can occur at altitudes lower than 100 km; that the peak altitudes and densities of both the M2 and M1 layers at dawn change more with season than they do at dusk; and that the M2 peak density decreases at a faster rate than the M1 with SZA.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116251"},"PeriodicalIF":2.5,"publicationDate":"2024-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003117/pdfft?md5=43b2136dc5bf268f254936412ec9c2b5&pid=1-s2.0-S0019103524003117-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142162314","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}

{"title":"Unexpected mineral impact on organic evolution during simulated aqueous alteration in asteroids","authors":"Coline Serra ,&nbsp;Vassilissa Vinogradoff ,&nbsp;Grégoire Danger ,&nbsp;Marie-Vanessa Coulet ,&nbsp;Fabrice Duvernay","doi":"10.1016/j.icarus.2024.116273","DOIUrl":"10.1016/j.icarus.2024.116273","url":null,"abstract":"<div><p>The presence of organic matter in carbonaceous chondrites provides valuable information about the early composition of the Solar System. Although they are considered primitive, the majority of these chondrites have undergone secondary processes subsequent to their formation. These processes, such as aqueous alteration, have altered their composition. The effect of aqueous alteration on minerals is well known, but the effect on organic matter and/or on an organo-mineral system have been little studied. Here, we report experimental results devoted to investigate the chemical evolution of a hypothetical initial chondritic material subjected to hydrothermal alteration under reducing conditions at low-temperature. The mixtures consist of different anhydrous minerals (peridot, feldspar, troilite) together with hexamethylenetetramine (HMT) chosen as a model molecule inherited from the interstellar grains. After different times at 80 °C, the large molecular diversity formed is highly influenced by the presence and the nature of the minerals, as highlighted in particular by the evolution of the amide produced. The presence of minerals in the mixture appears to influence the reactivity of the system more through the formation of salts and chelates than through surface adsorption mechanisms. The most pronounced effect is observed in the presence of troilite, both in the degradation of HMT and in the abundance of amides formed. The study of the mutual influence of minerals and organic matter, and their intrinsic transformations in the media during the processes, could help to understand about the origin of organic molecules observed in carbonaceous chondrites.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"423 ","pages":"Article 116273"},"PeriodicalIF":2.5,"publicationDate":"2024-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142049714","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":"Dyke swarms of Onenhste and adjacent coronae in Parga Chasmata, SE of Atla Regio, Venus: Detailed mapping, swarm interactions and geological history","authors":"Mohamed Ben Marzoug ,&nbsp;Hafida El Bilali ,&nbsp;Richard E. Ernst ,&nbsp;Kenneth L. Buchan ,&nbsp;James W. Head ,&nbsp;Naima Hannour","doi":"10.1016/j.icarus.2024.116269","DOIUrl":"10.1016/j.icarus.2024.116269","url":null,"abstract":"<div><p>Parga Chasmata is a 10,000 km long rift system on Venus with abundant coronae (enigmatic circular tectonomagmatic features). In order to further investigate the rift-corona relationship, detailed 1:500,000 geological mapping was focused on Onenhste Corona and the surrounding region (16°-24° S, 145°-131° W). More than 46,000 extensional lineaments were mapped and grouped into 50 sets, comprising 17 radiating, 28 circumferential and 5 linear sets (interpreted to overlie mafic dyke swarms). Radiating and circumferential swarms are linked with Onenhste Corona (OC), Momu Coronae (MC), Ulgen-ekhe Coronae (UEC), Rzhanitsa Corona (RzC, centred just outside the study area) and 5 Unnamed Coronae (UC1–5), as well as Malibran Patera (MP) and Fedchenko Patera (FP). Linear swarms are provisionally linked with magmatic centres outside the study area. Crosscutting relationships between the graben sets (dyke swarms) were used to identify the relative ages of magmatic centres. We applied an additional approach to recognize coeval centres, the swinging or deflection of radiating and circumferential dyke swarms to reveal the stress interaction between different coeval centres. The relative ages (oldest to youngest) of the magmatic centres are UC2 &gt; RzC &gt; MC ≥ OC = UC1 = UEC ≥ MP &gt; UC5, and FP &gt; UC3. These new detailed data provide significant information on coronae timing, evolution and relation to rift zones that will serve as a basis for future quantitative studies of lithospheric and mantle evolution and the combined cause and effect of rifting and mantle diapiric upwelling.</p><p>Several centres, RzC, UC2, MC, UC3 and FP, ordered from NW to SE, are aligned along a trend parallel to Parga Chasmata but offset about 900 km to the south from the main zone of rifting. It is inferred that this alignment is related to a zone of weakness associated with the rift extension. Along this trend the centres do not show an age progression.</p><p>Coronae MC, OC, UC1 and UEC are aligned along the NNE trending P13 Linea, orthogonal to the main Parga Chasmata rift. The main centre, Onenhste, is coeval with UC1, which in turn is coeval with UEC. Additional age relationships indicate that the late stage of OC was active at the same time as MP, MC and the UC2–9 centre of UC2. Linea P13 is older than Chondi Chasma. This study, and continuing, detailed geological mapping and analysis are increasing our understanding of the relationships between the formation of the main WNW trending Parga Chasmata rift zone, the orthogonal trends of rifting and the numerous magmatic centres (mainly coronae) distributed along both trends.</p></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"424 ","pages":"Article 116269"},"PeriodicalIF":2.5,"publicationDate":"2024-08-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0019103524003294/pdfft?md5=91dee2a1412e238618cf7d74a972f653&pid=1-s2.0-S0019103524003294-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142117676","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}