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Journal articles on the topic 'Inner Solar System'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Slater, Tim. "Inner solar system concepts." Physics Teacher 38, no. 5 (2000): 264–65. http://dx.doi.org/10.1119/1.880527.

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2

Greenstreet, Sarah. "Asteroids in the inner solar system." Physics Today 74, no. 7 (2021): 42–47. http://dx.doi.org/10.1063/pt.3.4794.

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3

Sylvan, Richard, Narayanan M. Komerath, Kirk Woellert, Mark Homnick, and Joseph E. Palaia. "The Emerging Inner Solar System Economy." World Futures Review 1, no. 2 (2009): 23–38. http://dx.doi.org/10.1177/194675670900100206.

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4

Donahue, T. M., T. I. Gombosi, and B. R. Sandel. "Cometesimals in the inner Solar System." Nature 330, no. 6148 (1987): 548–50. http://dx.doi.org/10.1038/330548a0.

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5

Mann, Ingrid, Edmond Murad, and Andrzej Czechowski. "Nanoparticles in the inner solar system." Planetary and Space Science 55, no. 9 (2007): 1000–1009. http://dx.doi.org/10.1016/j.pss.2006.11.015.

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6

Alexander, Conel M. O'D. "The origin of inner Solar System water." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2094 (2017): 20150384. http://dx.doi.org/10.1098/rsta.2015.0384.

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Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model)

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7

Trinquier, Anne, Jean‐Louis Birck, and Claude J. Allegre. "Widespread54Cr Heterogeneity in the Inner Solar System." Astrophysical Journal 655, no. 2 (2007): 1179–85. http://dx.doi.org/10.1086/510360.

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8

Hall, D. T., and D. E. Shemansky. "No cometesimals in the inner Solar System." Nature 335, no. 6189 (1988): 417–19. http://dx.doi.org/10.1038/335417a0.

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9

Milgrom, Mordehai. "MOND effects in the inner Solar system." Monthly Notices of the Royal Astronomical Society 399, no. 1 (2009): 474–86. http://dx.doi.org/10.1111/j.1365-2966.2009.15302.x.

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10

Chambers, John E. "Planetary accretion in the inner Solar System." Earth and Planetary Science Letters 223, no. 3-4 (2004): 241–52. http://dx.doi.org/10.1016/j.epsl.2004.04.031.

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11

Elkins-Tanton, Linda T. "Magma Oceans in the Inner Solar System." Annual Review of Earth and Planetary Sciences 40, no. 1 (2012): 113–39. http://dx.doi.org/10.1146/annurev-earth-042711-105503.

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12

Resnick, Andrew. "Airless bodies of the inner solar system." Contemporary Physics 61, no. 1 (2020): 52–53. http://dx.doi.org/10.1080/00107514.2020.1736166.

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13

Byrne, Paul K. "A comparison of inner Solar System volcanism." Nature Astronomy 4, no. 4 (2019): 321–27. http://dx.doi.org/10.1038/s41550-019-0944-3.

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14

Batygin, Konstantin, Alessandro Morbidelli, and Mathew J. Holman. "CHAOTIC DISINTEGRATION OF THE INNER SOLAR SYSTEM." Astrophysical Journal 799, no. 2 (2015): 120. http://dx.doi.org/10.1088/0004-637x/799/2/120.

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15

Connors, Martin, R. Greg Stacey, Paul Wiegert, and Ramon Brasser. "Inner Solar System dynamical analogs of plutinos." Icarus 194, no. 2 (2008): 789–99. http://dx.doi.org/10.1016/j.icarus.2007.11.011.

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16

Sarafian, Adam R., Erik H. Hauri, Francis M. McCubbin, et al. "Early accretion of water and volatile elements to the inner Solar System: evidence from angrites." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2094 (2017): 20160209. http://dx.doi.org/10.1098/rsta.2016.0209.

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Inner Solar System bodies are depleted in volatile elements relative to chondrite meteorites, yet the source(s) and mechanism(s) of volatile-element depletion and/or enrichment are poorly constrained. The timing, mechanisms and quantities of volatile elements present in the early inner Solar System have vast implications for diverse processes, from planetary differentiation to the emergence of life. We report major, trace and volatile-element contents of a glass bead derived from the D'Orbigny angrite, the hydrogen isotopic composition of this glass bead and that of coexisting olivine and sili

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17

Hallis, L. J. "D/H ratios of the inner Solar System." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2094 (2017): 20150390. http://dx.doi.org/10.1098/rsta.2015.0390.

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The original hydrogen isotope (D/H) ratios of different planetary bodies may indicate where each body formed in the Solar System. However, geological and atmospheric processes can alter these ratios through time. Over the past few decades, D/H ratios in meteorites from Vesta and Mars, as well as from S- and C-type asteroids, have been measured. The aim of this article is to bring together all previously published data from these bodies, as well as the Earth, in order to determine the original D/H ratio for each of these inner Solar System planetary bodies. Once all secondary processes have bee

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18

Meech, Karen J., Bin Yang, Jan Kleyna, et al. "Inner solar system material discovered in the Oort cloud." Science Advances 2, no. 4 (2016): e1600038. http://dx.doi.org/10.1126/sciadv.1600038.

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We have observed C/2014 S3 (PANSTARRS), a recently discovered object on a cometary orbit coming from the Oort cloud that is physically similar to an inner main belt rocky S-type asteroid. Recent dynamical models successfully reproduce the key characteristics of our current solar system; some of these models require significant migration of the giant planets, whereas others do not. These models provide different predictions on the presence of rocky material expelled from the inner solar system in the Oort cloud. C/2014 S3 could be the key to verifying these predictions of the migration-based dy

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19

Omodaka, Yuichi, Kyosuke Hiyama, Thanyalak Srisamranrungruang, Yutaka Oura, and Yukiyasu Asaoka. "Application of Dynamic Insulation Technique to Airflow Window System." E3S Web of Conferences 111 (2019): 03041. http://dx.doi.org/10.1051/e3sconf/201911103041.

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It is necessary to improve solar blocking performance and reduce solar heat gain coefficient (SHGC) of openings in office buildings in order to reduce the cooling loads. Airflow windows are often practiced in Japan’s office buildings. In this research, we apply a Dynamic Insulation (DI) technique into an airflow window system to improve the solar blocking performance. Computational fluid dynamics (CFD) analyses have been used to measure the thermal performance of the numerical opening model. In the case of using a conventional airflow window model, the inner-surface temperature of the inner gl

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20

Van Kooten, Elishevah M. M. E., Daniel Wielandt, Martin Schiller, et al. "Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites." Proceedings of the National Academy of Sciences 113, no. 8 (2016): 2011–16. http://dx.doi.org/10.1073/pnas.1518183113.

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The short-lived 26Al radionuclide is thought to have been admixed into the initially 26Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent 54Cr and 26Mg*, the decay product of 26Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling 26Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of s

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21

Meech, Karen. "Origins of water in the Solar System leading to habitable worlds." Proceedings of the International Astronomical Union 11, A29B (2015): 400. http://dx.doi.org/10.1017/s1743921316005639.

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AbstractLife on Earth depends on an aqueous biochemistry, and water is a key component of habitability on Earth and for likely other habitable environments in the solar system. While water is ubiquitous in the interstellar medium, and plays a key role in protoplanetary disk chemistry, the inner solar system is relatively dry. We now have evidence for potentially thousands of extrasolar planets, dozens of which may be located in their host stars habitable zones. Understanding how planets in the habitable zone accrete their water, is key to understanding the likelihood for habitability. Given th

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22

Yoshizaki, Takashi, and William F. McDonough. "Earth and Mars – Distinct inner solar system products." Geochemistry 81, no. 2 (2021): 125746. http://dx.doi.org/10.1016/j.chemer.2021.125746.

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23

Nuth, Joseph A., Neyda Abreu, Frank T. Ferguson, et al. "Volatile-rich Asteroids in the Inner Solar System." Planetary Science Journal 1, no. 3 (2020): 82. http://dx.doi.org/10.3847/psj/abc26a.

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24

Tabachnik, S. A., and N. W. Evans. "Asteroids in the inner Solar system - I. Existence." Monthly Notices of the Royal Astronomical Society 319, no. 1 (2002): 63–79. http://dx.doi.org/10.1046/j.1365-8711.2000.03760.x.

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25

Rickman, Hans. "Transport of comets to the Inner Solar System." Proceedings of the International Astronomical Union 2004, IAUC197 (2004): 277–88. http://dx.doi.org/10.1017/s1743921304008774.

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26

Skoglöv, E. "Spin vector evolution for inner solar system asteroids." Planetary and Space Science 47, no. 1-2 (1998): 11–22. http://dx.doi.org/10.1016/s0032-0633(98)00111-1.

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27

van den Bergh, S. "Life and death in the inner solar system." Publications of the Astronomical Society of the Pacific 101 (May 1989): 500. http://dx.doi.org/10.1086/132459.

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28

Murison, Marc A. "A Dynamical Survey of Inner Solar System Asteroids." International Astronomical Union Colloquium 172 (1999): 371–72. http://dx.doi.org/10.1017/s0252921100072766.

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AbstractResults from a numerical integration survey of all 179 currently-known inner solar system asteroids with a ≤ aMars, q ≥ aMercury are presented. A surprising number of asteroids are currently in, or very near, mean-motion resonances with Mercury, Venus, Earth, or Mars. Some of the resonance associations are of high order. Most of the resonance associations are relatively short-lived, with the asteroids wandering in and out of resonance on timescales of hundreds to several thousand years.

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29

Tabachnik, S. A., and N. W. Evans. "Existence of Asteroids in the Inner Solar System." Symposium - International Astronomical Union 202 (2004): 238–40. http://dx.doi.org/10.1017/s007418090021797x.

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Ensembles of in-plane and inclined orbits in the vicinity of the Lagrange points of the terrestrial planets are integrated for up to 100 million years. Mercurian Trojans probably do not exist, although there is evidence for long-lived, corotating horseshoe orbits with small inclinations. Both Venus and the Earth are much more promising, as they possess rich families of stable tadpole and horseshoe orbits. Our survey of in-plane test particles near the Martian Lagrange points shows no survivors after 60 million years. Low inclination test particles do not persist, as their inclinations are quic

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30

Masson, Philippe. "La geologie planetaire; bilan et perspectives." Bulletin de la Société Géologique de France III, no. 1 (1987): 113–14. http://dx.doi.org/10.2113/gssgfbull.iii.1.113.

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Abstract A general statement on the geology of the solar system inner planets is summarized. Relevant unsolved problems are then presented. The main space programs for the exploration of the inner solar system during the ten forthcoming years are described.

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31

Barbato, D., A. Sozzetti, S. Desidera, et al. "Exploring the realm of scaled solar system analogues with HARPS." Astronomy & Astrophysics 615 (July 2018): A175. http://dx.doi.org/10.1051/0004-6361/201832791.

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Context. The assessment of the frequency of planetary systems reproducing the solar system’s architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planets. Aims. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions an

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32

Cadieu, Fred. "Water: The Essential Component of Our Inner Solar System." American Journal of Modern Physics 14, no. 1 (2025): 37–43. https://doi.org/10.11648/j.ajmp.20251401.15.

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If our solar system started with the terrestrial planets initially covered with water, then a reasonable progression of events result in the presently observed inner solar system. Two principal assumptions have been made. One is that molten rock and the iron rich cores of the terrestrial planets can dissolve appreciable quantities of water. The other is that our solar system was formed initially from cold gas and dust which contained due to condensation large quantities of water. Water then became trapped in the cores and molten rock of the forming terrestrial planets. This in essence implies

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33

Laskar, J. "The Chaotic Motion of the Solar System." International Astronomical Union Colloquium 132 (1993): 21. http://dx.doi.org/10.1017/s025292110006588x.

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AbstractIn a previous paper (Laskar, Nature, 338, 237-238), the chaotic nature of the solar system excluding Pluto was established by the numerical computation of the maximum Lyapunov exponent of its secular system over 200 Myr. In the present an explanation is given for the exponential divergence of the orbits: it is due to the transition from libration to circulation of the critical argument of the secular resonance 2(g4−g3)−(s4−s3) related to the motions of perihelions and nodes of the Birth and Mars. An other important secular resonance is identified: (g1−g5)−(s1−s2). Its critical argument

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34

Ueda, Takahiro, Masahiro Ogihara, Eiichiro Kokubo, and Satoshi Okuzumi. "Early Initiation of Inner Solar System Formation at the Dead-zone Inner Edge." Astrophysical Journal Letters 921, no. 1 (2021): L5. http://dx.doi.org/10.3847/2041-8213/ac2f3b.

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35

Grün, Eberhard. "Dust Measurements in the Outer Solar System." Symposium - International Astronomical Union 160 (1994): 367–80. http://dx.doi.org/10.1017/s0074180900046659.

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In-situ measurements of micrometeoroids provide information on the spatial distribution of interplanetary dust and its dynamical properties. Pioneers 10 and 11, Galileo and Ulysses spaceprobes took measurements of interplanetary dust from 0.7 to 18 AU distance from the sun. Distinctly different populations of dust particles exist in the inner and outer solar system. In the inner solar system, out to about 3 AU, zodiacal dust particles are recognized by their scattered light, their thermal emission and by in-situ detection from spaceprobes. These particles orbit the sun on low inclination (i ≤

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36

Девяткин, А. В., В. Н. Львов, С. Д. Цекмейстер, Д. Л. Горшанов, С. Н. Петрова, and А. А. Мартюшева. "Special asteroids in the Solar System." Научные труды Института астрономии РАН, no. 1 (July 22, 2022): 16–22. http://dx.doi.org/10.51194/inasan.2022.7.1.003.

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Представлены результаты выявления астероидов, потенциально опасных для внутренних планет. Исследовано орбитальное движение астероида 2022 АЕ1, троянцев Земли (2010 TK7, 2020 XL5) и «рукотворного» астероида 2020 SO. The results of the detection of potentially hazardous asteroids for the inner planets are presented. The orbital motion of asteroid 2022 AE1, the Earth Trojans (2010 TK7, 2020 XL5), and the “man-made” asteroid 2020 SO has been studied.

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37

Alexander, Conel M. O'D. "Correction to ‘The origin of inner Solar System water’." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 379, no. 2194 (2021): 20200435. http://dx.doi.org/10.1098/rsta.2020.0435.

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38

Wang, Lu, Hongfei Zheng, Yunsheng Zhao, and Xinglong Ma. "Solar-driven natural vacuum desalination system with inner condenser." Applied Thermal Engineering 196 (September 2021): 117320. http://dx.doi.org/10.1016/j.applthermaleng.2021.117320.

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39

Evans, N. W., and S. A. Tabachnik. "Asteroids in the inner Solar system - II. Observable properties." Monthly Notices of the Royal Astronomical Society 319, no. 1 (2002): 80–94. http://dx.doi.org/10.1046/j.1365-8711.2000.03761.x.

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40

Dudley-Flores, Marilyn, and Thomas Gangale. "Forecasting the Political Economy of the Inner Solar System." Astropolitics 10, no. 3 (2012): 183–233. http://dx.doi.org/10.1080/14777622.2012.734948.

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41

Prentice, A. J. R. "Origin and chemical composition of the inner solar system." Geochimica et Cosmochimica Acta 70, no. 18 (2006): A504. http://dx.doi.org/10.1016/j.gca.2006.06.1601.

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42

Gladman, Brett, Luke Dones, Harold F. Levison, and Joseph A. Burns. "Impact Seeding and Reseeding in the Inner Solar System." Astrobiology 5, no. 4 (2005): 483–96. http://dx.doi.org/10.1089/ast.2005.5.483.

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43

Bockelee-Morvan, Dominique. "Water in small bodies of the Solar System." Proceedings of the International Astronomical Union 11, A29B (2015): 401. http://dx.doi.org/10.1017/s1743921316005640.

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AbstractWater in form of ice or vapour is observed in comets, transneptunian objects and icy satellites formed in the outer regions of the Solar System, as well as in objects orbiting in the inner Solar System, such as dwarf planet Ceres. I will present an overview of the water content and properties in these objects and the implications in terms of solar system formation and evolution.

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44

Sokolov, Igor V., and Tamas I. Gombosi. "Physics-based Forecasting of Tomorrow’s Solar Wind at 1 au." Astrophysical Journal 987, no. 1 (2025): 83. https://doi.org/10.3847/1538-4357/add52f.

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Abstract Inspired by the concept of relativity of simultaneity used in the theory of special relativity, a new approach is proposed to simulate future solar wind conditions at any point in the inner solar system. An important distinctive feature of the proposed approach is that the simulation in the solar corona is driven by hourly updated solar magnetograms and is continuously simulated in nearly real time. The model for the inner heliosphere is based on time transformation to a boosted spacetime coordinate system, in which the current state of the solar wind at the solar corona–inner heliosp

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45

Nesvorný, David, Luke Dones, Mario De Prá, Maria Womack, and Kevin J. Zahnle. "Impact Rates in the Outer Solar System." Planetary Science Journal 4, no. 8 (2023): 139. http://dx.doi.org/10.3847/psj/ace8ff.

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Abstract Previous studies of cometary impacts in the outer solar system used the spatial distribution of ecliptic comets (ECs) from dynamical models that assumed ECs began on low-inclination orbits (≲5°) in the Kuiper Belt. In reality, the source population of ECs—the trans-Neptunian scattered disk—has orbital inclinations reaching up to ∼30°. In Nesvorný et al., we developed a new dynamical model of ECs by following comets as they evolved from the scattered disk to the inner solar system. The model was absolutely calibrated from the population of Centaurs and active ECs. Here we use our EC mo

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46

Williams, Curtis D., Matthew E. Sanborn, Céline Defouilloy, et al. "Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk." Proceedings of the National Academy of Sciences 117, no. 38 (2020): 23426–35. http://dx.doi.org/10.1073/pnas.2005235117.

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Dynamic models of the protoplanetary disk indicate there should be large-scale material transport in and out of the inner Solar System, but direct evidence for such transport is scarce. Here we show that the ε50Ti-ε54Cr-Δ17O systematics of large individual chondrules, which typically formed 2 to 3 My after the formation of the first solids in the Solar System, indicate certain meteorites (CV and CK chondrites) that formed in the outer Solar System accreted an assortment of both inner and outer Solar System materials, as well as material previously unidentified through the analysis of bulk mete

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47

Seligman, Darryl Z., Kaitlin M. Kratter, W. Garrett Levine, and Robert Jedicke. "A Sublime Opportunity: The Dynamics of Transitioning Cometary Bodies and the Feasibility of In Situ Observations of the Evolution of Their Activity." Planetary Science Journal 2, no. 6 (2021): 234. http://dx.doi.org/10.3847/psj/ac2dee.

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Abstract The compositional and morphological evolution of minor bodies in the solar system is primarily driven by the evolution of their heliocentric distances, as the level of incident solar radiation regulates cometary activity. We investigate the dynamical transfer of Centaurs into the inner solar system, facilitated by mean motion resonances with Jupiter and Saturn. The recently discovered object P/2019 LD2 will transition from the Centaur region to the inner solar system in 2063. In order to contextualize LD2, we perform N-body simulations of a population of Centaurs and Jupiter-family co

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48

Tanaka, Ryoji, Christian Potiszil, and Eizo Nakamura. "Silicon and Oxygen Isotope Evolution of the Inner Solar System." Planetary Science Journal 2, no. 3 (2021): 102. http://dx.doi.org/10.3847/psj/abf490.

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49

Platz, T., P. K. Byrne, M. Massironi, and H. Hiesinger. "Volcanism and tectonism across the inner solar system: an overview." Geological Society, London, Special Publications 401, no. 1 (2014): 1–56. http://dx.doi.org/10.1144/sp401.22.

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50

Mann, Adam. "Inner Workings: Hunting for microbial life throughout the solar system." Proceedings of the National Academy of Sciences 115, no. 45 (2018): 11348–50. http://dx.doi.org/10.1073/pnas.1816535115.

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