Space Science Reviews最新文献

{"title":"Geodetic Investigations of the Europa Clipper Mission.","authors":"G Steinbrügge, R S Park, J H Roberts, M Bland, S Brooks, J Castillo-Rogez, G Cascioli, A Genova, T Greathouse, H Hussmann, R Kirk, A Magnanini, E Mazarico, F Nimmo, M S Park, F Petricca, K Retherford, D M Schroeder, K M Soderlund, P Tortora, M Zannoni","doi":"10.1007/s11214-025-01250-x","DOIUrl":"10.1007/s11214-025-01250-x","url":null,"abstract":"<p><p>The Europa Clipper mission will investigate the geophysical properties of Europa, one of Jupiter's Galilean moons, to assess its habitability. Geodetic measurements will play a critical role in determining Europa's internal structure, including the thickness of the ice shell, the presence and extent of a subsurface ocean, and the distribution of mass in the deeper interior. To build the necessary geodetic data set, the Geodesy Focus Group (GFG) coordinates cross-instrument efforts to measure Europa's global shape, rotational parameters, gravity field, and degree-2 tidal Love numbers ( <math><msub><mi>k</mi> <mn>2</mn></msub> </math> and <math><msub><mi>h</mi> <mn>2</mn></msub> </math> ). Here we summarize how data from the Gravity/Radio Science (G/RS) investigation, Europa Imaging System (EIS), Radar for Europa Assessment and Sounding (REASON), and Europa Ultraviolet Spectrograph (Europa-UVS) will be used to infer geodetic constraints on the interior structure and to establish a precise cartographic reference system for geophysical and geological interpretation. Together, the resulting geodetic information will contribute to a deeper understanding of Europa's internal dynamics and the potential habitability of its ocean.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 1","pages":"17"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC12868062/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146126423","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":"Direct Samples of Interstellar and Interplanetary Material with IMAP.","authors":"J R Szalay, E Provornikova, E Ayari, M Bzowski, E R Christian, H O Funsten, A Galli, M Gkioulidou, M Horányi, S Livi, D J McComas, E Möbius, K Ogasawara, F Rahmanifard, J S Rankin, D B Reisenfeld, N A Schwadron, Z Sternovsky, P Swaczyna, D Turner, G P Zank, E J Zirnstein","doi":"10.1007/s11214-026-01291-w","DOIUrl":"10.1007/s11214-026-01291-w","url":null,"abstract":"<p><p>The Interstellar Mapping and Acceleration (IMAP) mission probes the interaction between our heliosphere and the interstellar medium (ISM) in unprecedented detail. The broad science that IMAP addresses has been organized into three distinct science themes: A) Acceleration and the broader context of the solar wind and space weather; B) Exploring the outer heliosphere through energetic neutral atoms, and C) Sampling of the interstellar and interplanetary material. This paper summarizes the scientific goals of the latter theme and identifies the key scientific opportunities for IMAP available due to its unique ability to directly sample the interstellar and interplanetary material from 1 au. It is organized into three broad scientific questions that directly relate to IMAP's science objectives: 1) What is the state of the pristine upstream LISM and how does it relate to its origins and evolution? 2) How does the VLISM interact with the heliosphere? 3) How does interstellar material, as well as interplanetary dust, affect the near-Sun environment?</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 3","pages":"36"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13046683/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147623929","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":"Euhabitability: A New Term to Aid in the Search for Life in Addition to the Habitable Zone Framework.","authors":"Donald M Glaser, Stephanie Olson, Svetlana Berdyugina, Paul Byrne, Peter Cawood, Manasvi Lingam, Jacob Lustig-Yaeger, Tilman Spohn","doi":"10.1007/s11214-026-01315-5","DOIUrl":"10.1007/s11214-026-01315-5","url":null,"abstract":"<p><p>The search for life on exoplanets is difficult due to observational limitations stemming from vast separating distances. The Habitable Zone (HZ) is a simplifying framework for identifying exoplanets that may be suitable for life, given our observational limitations. The HZ framework is built on many simplifying assumptions and only attempts to bound the circumstellar regions where surface oceans are not precluded. In other words, HZ exoplanets are where surface oceans are possible, not necessarily where life is possible. Water is essential for life as we know it, however, life requires additional factors such as nutrients and a magnetosphere. Therefore, the criteria of the HZ framework is one step removed from assessing the suitability for life. This nuance is easily lost in translation and has caused confusion among researchers and the general public; as the term \"Habitable Zone\" implies that planets in the HZ are habitable and those outside are uninhabitable. Here we define a new term, euhabitable (suitable for life), that addresses this confusion. In brief, a euhabitable exoplanet can exist outside the HZ (e.g., a Europa-like planet), and an uninhabitable exoplanet can exist within the HZ (e.g., a desiccated planet). The \"euhabitable\" term can be used to discuss these cases explicitly, avoiding confusion between an exoplanet's suitability for life and it's position relative to the HZ. The euhabitable framework is informed by the advancements in astrobiology over the past three decades, and primes exoplanet science for the future by moving the habitability discussion beyond \"follow the water.\"</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 5","pages":"63"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13447492/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148689900","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":"Super-Critical Accretion onto Stellar Mass Black Holes and Neutron Stars: A Short Review.","authors":"M Middleton, G Lipunova, K Ohsuga, M Abramowicz","doi":"10.1007/s11214-026-01318-2","DOIUrl":"10.1007/s11214-026-01318-2","url":null,"abstract":"<p><p>Super-critical accretion is of both theoretical and observational importance. Theoretically first established by Shakura & Sunyaev in 1973, studies of this accretion regime has since evolved to encompass vital aspects such as advection, surface effects (neutron stars) and the interplay between the plasma, magnetic fields and radiation in full numerical GR-(R)MHD. In this short review of the subject, we present the underlying analytical theory, observational predictions and the role of numerical simulations, with a focus on super-Eddington accretion onto stellar mass black holes and neutron stars. We then discuss observational progress and tensions, and suggestions for how the field might progress in the coming years.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 6","pages":"71"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13558364/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148930909","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":"Water Versus Land on Temperate Rocky Planets.","authors":"Claire Marie Guimond, Tilman Spohn, Svetlana Berdyugina, Paul K Byrne, Nicolas Coltice, Donald M Glaser, Manasvi Lingam, Charles H Lineweaver, Peter A Cawood","doi":"10.1007/s11214-025-01264-5","DOIUrl":"10.1007/s11214-025-01264-5","url":null,"abstract":"<p><p>Water and land surfaces on a planet interact in particular ways with gases in the atmosphere and with radiation from the star. These interactions define the environments that prevail on the planet, some of which may be more amenable to prebiotic chemistry, some to the evolution of more complex life. This review article covers (i) the physical conditions that determine the ratio of land to sea on a rocky planet, (ii) how this ratio would affect climatic and biologic processes, and (iii) whether future astronomical observations might constrain this ratio on exoplanets. Water can be delivered in multiple ways to a growing rocky planet - and although we may not agree on the contribution of different mechanism(s) to Earth's bulk water, hydrated building blocks and nebular ingassing could at least in principle supply several oceans' worth. The water that planets can sequester over eons in their solid deep mantles is limited by the water concentration at water saturation of nominally anhydrous mantle minerals, being in sum likely less than 2000 ppm of the planet mass. Water is cycled between mantle and surface through outgassing and ingassing mechanisms that, while tightly linked to tectonics, do not necessarily require plate tectonics in every case. The actual water/land ratio at a given time then emerges from the balance between the volume of surface water on the one hand, and on the other hand, the shape of the planet (its ocean basin volume) that is carved out by dynamic topography, the petrologic evolution of continents, impact cratering, and other surface-sculpting processes. By leveraging the contrast in reflectance properties of water and land surfaces, spatially resolved 2D maps of Earth-as-an-exoplanet have been retrieved from models using real Earth observations, demonstrating that water/land ratios of rocky exoplanets may be determined from data delivered by large-aperture, high-contrast imaging telescopes in the future.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 1","pages":"8"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC12783251/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145953082","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":"Properties of Magnetic Switchbacks in the Near-Sun Solar Wind.","authors":"Samuel T Badman, Naïs Fargette, Lorenzo Matteini, Oleksiy V Agapitov, Mojtaba Akhavan-Tafti, Stuart D Bale, Srijan Bharati Das, Nina Bizien, Trevor A Bowen, Thierry Dudok de Wit, Clara Froment, Timothy Horbury, Jia Huang, Vamsee Krishna Jagarlamudi, Andrea Larosa, Maria S Madjarska, Olga Panasenco, Etienne Pariat, Nour E Raouafi, Alexis P Rouillard, David Ruffolo, Nikos Sioulas, Shirsh Lata Soni, Luca Sorriso-Valvo, Gabriel Ho Hin Suen, Marco Velli, Jaye Verniero","doi":"10.1007/s11214-026-01267-w","DOIUrl":"10.1007/s11214-026-01267-w","url":null,"abstract":"<p><p>Magnetic switchbacks are fluctuations in the solar wind in which the interplanetary magnetic field sharply deflects away from its background direction so as to create folds in magnetic field lines while remaining of roughly constant magnitude. The magnetic field and velocity fluctuations are extremely well correlated in a way corresponding to Alfvénic fluctuations propagating away from the Sun. For a background field which is nearly radial this causes an outwardly propagating jet to form. Switchbacks and their characteristic velocity jets have recently been observed to be nearly ubiquitous by Parker Solar Probe with <i>in situ</i> measurements in the inner heliosphere within 0.3 AU. Their prevalence, substantial energy content, and potentially fundamental role in the dynamics of the outer corona and solar wind motivate the significant research efforts into their understanding. Here we review the <i>in situ</i> measurements of these structures (primarily by Parker Solar Probe). We discuss how they are identified and measured, and present an overview of the primary observational properties of these structures, both in terms of individual switchbacks and their collective arrangement into \"patches\". We identify both properties for which there is a strong consensus and those that have limited or qualified support and require further investigation. We identify and collate several open questions and recommendations for future studies.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 1","pages":"14"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC12847248/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146086854","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":"Upper Atmosphere Dynamics and Drivers of Volatiles Loss from Terrestrial-Type (Exo)Planets.","authors":"Daria Kubyshkina, M J Way, Iannis Dandouras, Helmut Lammer, Antonino Francesco Lanza, Manasvi Lingam, Rumi Nakamura, Moa Persson, Manuel Scherf, Kanako Seki","doi":"10.1007/s11214-026-01283-w","DOIUrl":"10.1007/s11214-026-01283-w","url":null,"abstract":"<p><p>Volatile loss from exoplanetary atmospheres and its possible implications for the longevity of habitable surface conditions is a topic of vigorous debate currently. The vast majority of the habitable zone terrestrial-like exoplanets known to date orbit low-mass M- and K-dwarf stars and are subject to the conditions drastically different to those of terrestrial planets in the Solar System. In particular, they orbit far closer to their host stars than similar planets around G-dwarfs similar to the Sun. Therefore they receive higher X-ray and UV fluxes, even though luminosities of M- and K-dwarfs are lower than those of heavier stars. Furthermore, due to their slower evolution, M-dwarfs retain high activity on the gigayear timescales. The combination of these two effects has led to claims that most terrestrial planets orbiting M-dwarfs may have their atmospheres stripped from the higher X-ray and UV fluxes of their host stars. Opposing this are researchers who point out that volatile inventories for terrestrial exoplanets are ill-constrained, and hence, they may be able to \"weather the storm\" of these higher X-ray and UV fluxes. In this article, we focus on exploring volatile loss in the upper atmospheres of terrestrial planets in our solar system and applications to those in exoplanetary systems around stars of different types.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 3","pages":"28"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC12999714/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147499956","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":"Accreting White Dwarfs: An Unreview.","authors":"Simone Scaringi, Christian Knigge, Domitilla de Martino","doi":"10.1007/s11214-026-01290-x","DOIUrl":"10.1007/s11214-026-01290-x","url":null,"abstract":"<p><p>Accreting white dwarfs (AWDs) are among the best natural laboratories for understanding disk accretion. Their proximity, brightness, and purely classical nature make them ideal systems in which to probe the fundamental physics that governs the transport of angular momentum, the generation of outflows, and the coupling between disks, magnetospheres, and accretors. Yet despite decades of study, many critical questions remain unresolved. In this \"unreview\", we therefore focus not on what is known, but on what is unknown. What drives viscosity and sustains accretion in largely neutral disks? How are powerful winds launched, and how do they feed back on the disk and binary evolution? Why do so many systems show persistent retrograde precession, and what drives bursts in magnetic AWDs? By identifying these open problems - and suggesting ways to resolve them - we aim to motivate new observational, numerical, and theoretical efforts that will advance our understanding of accretion physics across all mass scales, from white dwarfs to black holes.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 3","pages":"32"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13013232/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147521935","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":"Variability of the Martian Homopause: Insights from Global Climate Modelling and Empirical Estimates.","authors":"Juan Alday, Francisco González-Galindo, Denis A Belyaev, Miguel Ángel López-Valverde, Daria Kossova, Edward M B Thiemann, J Scott Evans, Anna A Fedorova, Sonal Jain, James A Holmes, Manish R Patel, François Forget","doi":"10.1007/s11214-026-01309-3","DOIUrl":"10.1007/s11214-026-01309-3","url":null,"abstract":"<p><p>The homopause marks the transition in a planetary atmosphere from turbulent mixing, which maintains a well-mixed composition, to molecular diffusion, which causes the diffusive separation of chemical species, impacting how these are distributed in the upper atmosphere and potentially escape to space. Here, we analyse simulations from the Mars Planetary Climate Model (Mars PCM) to investigate the variability of the Martian homopause in diurnal, seasonal and interannual timescales. The simulations reveal strong seasonal and latitudinal trends, with homopause altitudes peaking in the summer polar regions (∼120-130 km) and showing minimum values during the winter southern polar region (∼60-90 km). The simulations predict diurnal variations in the homopause altitude typically within 5-15 km and suggest that dust events can raise the value of the homopause altitude by 10-20 km, depending on the intensity of the event. When comparing the Mars PCM results with empirical estimates of the homopause altitude and density derived from Martian atmospheric data, we find that the model captures the overall magnitude and seasonal/latitudinal variability of the homopause, but appear to underestimate the strength of the diurnal cycle. Finally, we use the Mars PCM data to constrain the variability of the eddy diffusion coefficient, which can vary by one or two orders of magnitude across latitude and season. The derived parameterisation and variability of the eddy diffusion coefficient is suitable for use in one-dimensional models devoted to understanding seasonal difference in atmospheric photochemistry and escape.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 5","pages":"57"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13375689/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148580119","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":"Observations of Exocomets.","authors":"Judith Korth, Azib Norazman, Raphaël Bendahan-West, Grant Kennedy, Cristina Madurga Favieres, Daniela Iglesias, Olena Shubina, Siyi Xu, Nathan X Roth","doi":"10.1007/s11214-026-01300-y","DOIUrl":"10.1007/s11214-026-01300-y","url":null,"abstract":"<p><p>Active small bodies in extrasolar systems, the extrasolar analogues of Solar System comets, provide insights into the orbital evolution and physical processes shaping planetary systems. Since the discovery of exocomets around <math><mi>β</mi></math>  Pictoris, these small, icy bodies have shown the potential to become key probes for understanding planetary formation and migration. This review presents an overview of current observational techniques used to detect exocomets, focusing on individual systems and large-scale searches. We discuss photometric methods that identify exocomet transits through asymmetric light curves and spectroscopic techniques revealing cometary gases via time-variable absorption lines. Despite progress, significant open questions remain regarding the physical properties, occurrence rates, and similarities between exocomets and their Solar System counterparts. This review explores future opportunities in observational exocomet research, highlighting advancements required to further our understanding of these active small bodies and their role in the context of planetary system evolution.</p>","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":"222 4","pages":"41"},"PeriodicalIF":9.8,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC13128715/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147820953","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}