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Готові списки джерел за темами / Planetary Gravity; Planetary Magnetic Field; Planets / Статті в журналах

Щоб переглянути інші типи публікацій з цієї теми, перейдіть за посиланням: Planetary Gravity; Planetary Magnetic Field; Planets.

Статті в журналах з теми "Planetary Gravity; Planetary Magnetic Field; Planets"

Автор: Grafiati

Опубліковано: 3 червня 2025

Оновлено: 31 липня 2025

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1

Hamouda, Samir A., Eman A. Alsslam Alfadeel, and Mohamed Belhasan Mohamed. "PLANETARY MAGNETIC FIELD AND GRAVITY IN THE SOLAR SYSTEM." International Journal of Research -GRANTHAALAYAH 5, no. 9 (2017): 145–51. http://dx.doi.org/10.29121/granthaalayah.v5.i9.2017.2224.

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Gravity plays a major role in the planetary formation and the development of the solar system. Gravity attraction is the essence of a power that holds and governs the universe; it makes the planets in the solar system revolve around the sun and the moons around their planets. Magnetic fields are also an important phenomenon in the solar system and beyond. Their causes are complex and have a variety of effects on their surroundings; they have become a critical tool for the exploration of solar system bodies. However, the study of the mechanisms of planets formation in the solar system is a diff

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2

Samir, A. Hamouda, A. Alsslam Alfadeel Eman, and Belhasan Mohamed Mohamed. "PLANETARY MAGNETIC FIELD AND GRAVITY IN THE SOLAR SYSTEM." International Journal of Research - Granthaalayah 5, no. 9 (2017): 145–51. https://doi.org/10.5281/zenodo.1002135.

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Gravity plays a major role in the planetary formation and the development of the solar system. Gravity attraction is the essence of a power that holds and governs the universe; it makes the planets in the solar system revolve around the sun and the moons around their planets. Magnetic fields are also an important phenomenon in the solar system and beyond. Their causes are complex and have a variety of effects on their surroundings; they have become a critical tool for the exploration of solar system bodies. However, the study of the mechanisms of planets formation in the solar system is a diff

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3

Johansen, Anders. "The role of magnetic fields for planetary formation." Proceedings of the International Astronomical Union 4, S259 (2008): 249–58. http://dx.doi.org/10.1017/s1743921309030592.

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AbstractThe role of magnetic fields for the formation of planets is reviewed. Protoplanetary disc turbulence driven by the magnetorotational instability has a huge influence on the early stages of planet formation. Small dust grains are transported both vertically and radially in the disc by turbulent diffusion, counteracting sedimentation to the mid-plane and transporting crystalline material from the hot inner disc to the outer parts. The conclusion from recent efforts to measure the turbulent diffusion coefficient of magnetorotational turbulence is that turbulent diffusion of small particle

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4

Lutephy, Mohsen. "Interplanetary External Driven Quasidynamo as the Origin of Geomagnetic Jerks Correlated with Length of Day and Gravity Anomaly." Contributions to Geophysics and Geodesy 48, no. 1 (2018): 23–74. http://dx.doi.org/10.2478/congeo-2018-0002.

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Abstract We report phenomenological inevitable correlation between the Sun’s magnetic field oscillation through the Earth and the Jupiter, with sinusoidal geomagnetic jerks observed at the Earth, additionally aligned with the gravity and length of day sinusoidal variations and we observe too that the Sun and Jovian planets alignments with Jupiter are origin of the observable abrupt geomagnetic jerks whether historical or new, and experimental results demonstrate a possible explanation on the base of the planetary induced currents upon the metallic liquid cores of the planets upon the varying e

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5

Galanti, E., and Y. Kaspi. "Combined magnetic and gravity measurements probe the deep zonal flows of the gas giants." Monthly Notices of the Royal Astronomical Society 501, no. 2 (2020): 2352–62. http://dx.doi.org/10.1093/mnras/staa3722.

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ABSTRACT During the past few years, both the Cassini mission at Saturn and the Juno mission at Jupiter provided measurements with unprecedented accuracy of the gravity and magnetic fields of the two gas giants. Using the gravity measurements, it was found that the strong zonal flows observed at the cloud level of the gas giants are likely to extend thousands of kilometres deep into the planetary interior. However, the gravity measurements alone, which are by definition an integrative measure of mass, cannot constrain with high certainty the exact vertical structure of the flow. Taking into acc

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6

Lin, Zifan, Sara Seager, and Benjamin P. Weiss. "Interior and Gravity Field Models for Uranus Suggest a Mixed-composition Interior: Implications for the Uranus Orbiter and Probe." Planetary Science Journal 6, no. 2 (2025): 27. https://doi.org/10.3847/psj/ada124.

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Abstract The interior composition and structure of Uranus are ambiguous. It is unclear whether Uranus is composed of fully differentiated layers dominated by an icy mantle or has smooth compositional gradients. The Uranus Orbiter and Probe (UOP), the next NASA flagship mission prioritized by the Planetary Science and Astrobiology Survey 2023–2032, will constrain the planet's interior by measuring its gravity and magnetic fields. To characterize the Uranian interior, here we present CORGI, a newly developed planetary interior and gravity model. We confirm that high degrees of mixing are require

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7

Stevenson, David J. "Jupiter's Interior as Revealed by Juno." Annual Review of Earth and Planetary Sciences 48, no. 1 (2020): 465–89. http://dx.doi.org/10.1146/annurev-earth-081619-052855.

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Jupiter is in the class of planets that we call gas giants, not because they consist of gas but because they were primarily made from hydrogen-helium gas, which upon gravitational compression becomes a metallic fluid. Juno, in orbit about Jupiter since 2016, has changed our view: The gravity data are much improved, and the simplest interpretation of the higher order even harmonics implies that the planet may have a diluted central concentration of heavy elements. Jupiter has strong winds extending to perhaps ∼3,000-km depth that are evident in the odd zonal harmonics of the gravity field. Jupi

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8

Soyuer, Deniz, François Soubiran, and Ravit Helled. "Constraining the depth of the winds on Uranus and Neptune via Ohmic dissipation." Monthly Notices of the Royal Astronomical Society 498, no. 1 (2020): 621–38. http://dx.doi.org/10.1093/mnras/staa2461.

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ABSTRACT Determining the depth of atmospheric winds in the outer planets of the Solar system is a key topic in planetary science. We provide constraints on these depths in Uranus and Neptune via the total induced Ohmic dissipation, due to the interaction of the zonal flows and the planetary magnetic fields. An upper bound can be placed on the induced dissipation via energy and entropy flux throughout the interior. The induced Ohmic dissipation is directly linked to the electrical conductivity profile of the materials involved in the flow. We present a method for calculating electrical conducti

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9

Kislyakova, Kristina, and Lena Noack. "Electromagnetic induction heating as a driver of volcanic activity on massive rocky planets." Astronomy & Astrophysics 636 (April 2020): L10. http://dx.doi.org/10.1051/0004-6361/202037924.

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Aims. We investigate possible driving mechanisms of volcanic activity on rocky super-Earths with masses exceeding 3–4 M⊕. Due to high gravity and pressures in the mantles of these planets, melting in deep mantle layers can be suppressed, even if the energy release due to tidal heating and radioactive decay is substantial. Here we investigate whether a newly identified heating mechanism, namely induction heating by the star’s magnetic field, can drive volcanic activity on these planets due to its unique heating pattern in the very upper part of the mantle. In this region the pressure is not yet

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10

Miguel, Yamila, and Allona Vazan. "Interior and Evolution of the Giant Planets." Remote Sensing 15, no. 3 (2023): 681. http://dx.doi.org/10.3390/rs15030681.

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The giant planets were the first to form and hold the key to unveiling the solar system’s formation history in their interiors and atmospheres. Furthermore, the unique conditions present in the interiors of the giant planets make them natural laboratories for exploring different elements under extreme conditions. We are at a unique time to study these planets. The missions Juno to Jupiter and Cassini to Saturn have provided invaluable information to reveal their interiors like never before, including extremely accurate gravity data, atmospheric abundances and magnetic field measurements that r

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11

Hart, David. "The Influence of Magnetic Fields, Including the Planetary Magnetic Field, on Complex Life Forms: How Do Biological Systems Function in This Field and in Electromagnetic Fields?" Biophysica 4, no. 1 (2024): 1–21. http://dx.doi.org/10.3390/biophysica4010001.

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Life on Earth evolved to accommodate the biochemical and biophysical boundary conditions of the planet millions of years ago. The former includes nutrients, water, and the ability to synthesize other needed chemicals. The latter includes the 1 g gravity of the planet, radiation, and the geomagnetic field (GMF) of the planet. How complex life forms have accommodated the GMF is not known in detail, considering that Homo sapiens evolved a neurological system, a neuromuscular system, and a cardiovascular system that developed electromagnetic fields as part of their functioning. Therefore, all of t

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12

Lutephy, Mohsen. "Evidences of the charge fundamental asymmetry." Contributions to Geophysics and Geodesy 49, no. 1 (2019): 67–107. http://dx.doi.org/10.2478/congeo-2019-0005.

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Abstract There is an infinitesimal small non polarizable electric inertial charge in the individual atoms or in a number neutral matter included to equal number of the electrons and protons. We refer to the pure calculations verified by the experimental laboratorial results, also planetary phenomena and cosmic observations. This inertial electric charge is origin of a part of the measurable magnetic field in addition to self-consistent dynamo, together as complementary origins to generate very complex magnetism of the celestial bodies. Ultimately we refer to the null results of the test experi

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13

Volwerk, Martin, Beatriz Sánchez-Cano, Daniel Heyner, et al. "Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby." Annales Geophysicae 39, no. 5 (2021): 811–31. http://dx.doi.org/10.5194/angeo-39-811-2021.

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Abstract. Out of the two Venus flybys that BepiColombo uses as a gravity assist manoeuvre to finally arrive at Mercury, the first took place on 15 October 2020. After passing the bow shock, the spacecraft travelled along the induced magnetotail, crossing it mainly in the YVSO direction. In this paper, the BepiColombo Mercury Planetary Orbiter Magnetometer (MPO-MAG) data are discussed, with support from three other plasma instruments: the Planetary Ion Camera (SERENA-PICAM) of the SERENA suite, the Mercury Electron Analyser (MEA), and the BepiColombo Radiation Monitor (BERM). Behind the bow sho

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14

Ray, L. C., C. T. S. Lorch, J. O'Donoghue, et al. "Why is the H 3 + hot spot above Jupiter's Great Red Spot so hot?" Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2154 (2019): 20180407. http://dx.doi.org/10.1098/rsta.2018.0407.

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Recent observations of Jupiter's Great Red Spot indicate that the thermosphere above the storm is hotter than its surroundings by more than 700 K. Possible suggested sources for this heating have thus far included atmospheric gravity waves and lightning-driven acoustic waves. Here, we propose that Joule heating, driven by Great Red Spot vorticity penetrating up into the lower stratosphere and coupling to the thermosphere, may contribute to the large observed temperatures. The strength of Joule heating will depend on the local inclination angle of the magnetic field and thus the observed emissi

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15

Bromley, Benjamin C., and Scott J. Kenyon. "Magnetic Interactions in Orbital Dynamics." Astronomical Journal 164, no. 6 (2022): 229. http://dx.doi.org/10.3847/1538-3881/ac9301.

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Abstract The magnetic field of a host star can impact the orbit of a stellar partner, planet, or asteroid if the orbiting body is itself magnetic or electrically conducting. Here, we focus on the instantaneous magnetic forces on an orbiting body in the limit where the dipole approximation describes its magnetic properties as well as those of its stellar host. A permanent magnet in orbit about a star will be inexorably drawn toward the stellar host if the magnetic force is comparable to gravity due to the steep radial dependence of the dipole–dipole interaction. While magnetic fields in observe

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16

Militzer, Burkhard, William B. Hubbard, Sean Wahl, et al. "Juno Spacecraft Measurements of Jupiter’s Gravity Imply a Dilute Core." Planetary Science Journal 3, no. 8 (2022): 185. http://dx.doi.org/10.3847/psj/ac7ec8.

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Abstract The Juno spacecraft measured Jupiter’s gravity field and determined the even and odd zonal harmonics, J n , with unprecedented precision. However, interpreting these observations has been a challenge because it is difficult to reconcile the unexpectedly small magnitudes of the moments J 4 and J 6 with conventional interior models that assume a large, distinct core of rock and ice. Here we show that the entire set of gravity harmonics can be matched with models that assume an ab initio equation of state, wind profiles, and a dilute core of heavy elements that are distributed as far out

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17

Wicht, J., T. Gastine, L. D. V. Duarte, and W. Dietrich. "Dynamo action of the zonal winds in Jupiter." Astronomy & Astrophysics 629 (September 2019): A125. http://dx.doi.org/10.1051/0004-6361/201935682.

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The new data delivered by NASA’s Juno spacecraft significantly increase our understanding of the internal dynamics of Jupiter. The gravity data constrain the depth of the zonal flows observed at cloud level and suggest that they slow down considerably at a depth of about 0.96 rJ, where rJ is the mean radius at the one bar level. The magnetometer onboard Juno reveals the internal magnetic field of the planet. We combine the new zonal flow and magnetic field models with an updated electrical conductivity profile to assess the zonal-wind-induced dynamo action, concentrating on the outer part of t

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18

Vaytet, N., B. Commerçon, J. Masson, M. González, and G. Chabrier. "Protostellar birth with ambipolar and ohmic diffusion." Astronomy & Astrophysics 615 (July 2018): A5. http://dx.doi.org/10.1051/0004-6361/201732075.

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Context. The transport of angular momentum is fundamental during the formation of low-mass stars; too little removal and rotation ensures stellar densities are never reached, too much and the absence of rotation means no protoplanetary disks can form. Magnetic diffusion is seen as a pathway to resolving this long-standing problem. Aims. We aim to investigate the impact of including resistive magnetohydrodynamics (MHD) in simulations of the gravitational collapse of a 1 M⊙ gas sphere, from molecular cloud densities to the formation of the protostellar seed; the second Larson core. Methods. We u

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19

Moscadelli, Luca, Alberto Sanna, Henrik Beuther, André Oliva, and Rolf Kuiper. "Snapshot of a magnetohydrodynamic disk wind traced with water masers." Proceedings of the International Astronomical Union 18, S380 (2022): 167–71. http://dx.doi.org/10.1017/s1743921323002132.

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AbstractDisk-jet systems are common in astrophysical sources of different nature, from black holes to gaseous giant planets. The disk drives the mass accretion onto a central compact object and the jet ejects material along the disk rotation axis. Magnetohydrodynamic disk winds can provide the link between mass accretion and ejection, which is essential to ensure that the excess angular momentum is removed and accretion can proceed. However, up to now, we have been lacking direct observational proof of disk winds. This work presents a direct view of the velocity field of a disk wind around a f

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20

Alekseev, Victor R., Jiang-Shiou Hwang, and Margarita A. Levinskikh. "Effect of Space Flight Factor on Dormant Stages in Aquatic Organisms: A Review of International Space Station and Terrestrial Experiments." Life 12, no. 1 (2021): 47. http://dx.doi.org/10.3390/life12010047.

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This work is a review of the experiments carried out in the Russian segment of the ISS (inside and outside) from 2005 to 2016 on the effect of the space flight factor on the resting stages of organisms. In outer space, ultraviolet, a wide range of high and low temperatures, cosmic radiation, altered gravity, modified electromagnetic field, vacuum, factors of technical origin, ultrasound, microwave radiation, etc. and their combination determine the damaging effect on living organisms. At the same time, biological dormancy, known in a wide range of bacteria, fungi, animals and plants, allows th

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21

OHLSEN, DANIEL R., and PETER B. RHINES. "Laboratory studies of equatorially trapped waves using ferrofluid." Journal of Fluid Mechanics 338 (May 10, 1997): 35–58. http://dx.doi.org/10.1017/s0022112096004776.

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We introduce a new technique to model spherical geophysical fluid dynamics in the terrestrial laboratory. The local vertical projection of planetary vorticity, f, varies with latitude on a rotating spherical planet and allows an important class of waves in large-scale atmospheric and oceanic flows. These Rossby waves have been extensively studied in the laboratory for middle and polar latitudes. At the equator f changes sign where gravity is perpendicular to the planetary rotation. This geometry has made laboratory studies of geophysical fluid dynamics near the equator very limited. We use fer

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22

Unitsky, A. E., D. A. Isaev, V. L. Looksha, I. E. Labazava, and A. A. Telegina. "The role of geocosmic transport in the large-scale industrialization of the space." Bulletin of the South Ural State University series "Mechanical engineering industry" 23, no. 3 (2023): 39–50. http://dx.doi.org/10.14529/engin230304.

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Today, humanity is faced with a number of environmental problems, the solution of which depends on our continued existence. The authors propose a systematic approach to get out of this situation, which is described in detail in the EcoSpace program. The main vector of further industrial development will be space, but its implementation requires transport that has a number of unique characteristics. The authors of the article proposed the design of a general planetary vehicle (GPV), which is a self-supporting aircraft (with a length of 40,076 km, a total mass without payload of about 30 million

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23

Hamouda, Samir Ahmed, Nada Eaz-Alden Emgau, Rabab Muftah Bohagar, and Aisha Mohammed Eissa. "STUDY OF PLANETARY MAGNETIC FIELDS." International Journal of Research -GRANTHAALAYAH 5, no. 3 (2017): 29–44. http://dx.doi.org/10.29121/granthaalayah.v5.i3.2017.1752.

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Magnetic fields are an important phenomenon in the solar system and beyond. Their causes are complex and have a variety of effects on their surroundings; they have become a critical tool for the exploration of solar system bodies. Magnetic fields play a very important role in the Sun. From sunspots to coronal heating, from solar ares to coronal mass ejections all these apparently diverse phenomena have magnetic fields as their ultimate cause. The study of the terrestrial dynamo is a difficult problem made more so by the inability to construct planetary-scale dynamos for laboratory study. Howev

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24

Samir, Ahmed Hamouda, Eaz-Alden Emgau Nada, Muftah Bohagar Rabab, and Mohammed Eissa Aisha. "STUDY OF PLANETARY MAGNETIC FIELDS." International Journal of Research -GRANTHAALAYAH 5, no. 3 (2017): 29–44. https://doi.org/10.5281/zenodo.439552.

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Magnetic fields are an important phenomenon in the solar system and beyond. Their causes are complex and have a variety of effects on their surroundings; they have become a critical tool for the exploration of solar system bodies. Magnetic fields play a very important role in the Sun. From sunspots to coronal heating, from solar ares to coronal mass ejections all these apparently diverse phenomena have magnetic fields as their ultimate cause. The study of the terrestrial dynamo is a difficult problem made more so by the inability to construct planetary-scale dynamos for laboratory study. Howev

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25

Masset, Frédéric S. "Planetary migration in gaseous protoplanetary disks." Proceedings of the International Astronomical Union 3, S249 (2007): 331–46. http://dx.doi.org/10.1017/s1743921308016797.

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AbstractTides come from the fact that different parts of a system do not fall in exactly the same way in a non-uniform gravity field. In the case of a protoplanetary disk perturbed by an orbiting, prograde protoplanet, the protoplanet tides raise a wake in the disk which causes the orbital elements of the planet to change over time. The most spectacular result of this process is a change in the protoplanet's semi-major axis, which can decrease by orders of magnitude on timescales shorter than the disk lifetime. This drift in the semi-major axis is called planetary migration. In a first part, w

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26

Fossati, L., G. Guilluy, I. F. Shaikhislamov, et al. "The GAPS Programme at TNG." Astronomy & Astrophysics 658 (February 2022): A136. http://dx.doi.org/10.1051/0004-6361/202142336.

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Context. Because of its proximity to an active K-type star, the hot Jupiter WASP-80b has been identified as a possible excellent target for detecting and measuring He I absorption in the upper atmosphere. Aims. Our aim was to look for, and eventually measure and model, metastable He I atmospheric absorption. Methods. We observed four primary transits of WASP-80b in the optical and near-infrared using the HARPS-N and GIANO-B high-resolution spectrographs attached to the Telescopio Nazionale Galileo telescope, focusing the analysis on the He I triplet. We further employed a three-dimensional hyd

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27

Doelman, David S., Jordan M. Stone, Zackery W. Briesemeister, et al. "L-band Integral Field Spectroscopy of the HR 8799 Planetary System." Astronomical Journal 163, no. 5 (2022): 217. http://dx.doi.org/10.3847/1538-3881/ac5d52.

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Abstract Understanding the physical processes sculpting the appearance of young gas-giant planets is complicated by degeneracies confounding effective temperature, surface gravity, cloudiness, and chemistry. To enable more detailed studies, spectroscopic observations covering a wide range of wavelengths are required. Here we present the first L-band spectroscopic observations of HR 8799 d and e and the first low-resolution wide-bandwidth L-band spectroscopic measurements of HR 8799 c. These measurements were facilitated by an upgraded LMIRCam/ALES instrument at the Large Binocular Telescope, t

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28

Verliat, Antoine, Patrick Hennebelle, Anaëlle J. Maury, and Mathilde Gaudel. "Protostellar disk formation by a nonrotating, nonaxisymmetric collapsing cloud: model and comparison with observations." Astronomy & Astrophysics 635 (March 2020): A130. http://dx.doi.org/10.1051/0004-6361/201936394.

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Context. Planet-forming disks are fundamental objects that are thought to be inherited from large scale rotation through the conservation of angular momentum during the collapse of a prestellar dense core. Aims. We investigate the possibility for a protostellar disk to be formed from a motionless dense core that contains nonaxisymmetric density fluctuations. The rotation is thus generated locally by the asymmetry of the collapse. Methods. We study the evolution of the angular momentum in a nonaxisymmetric collapse of a dense core from an analytical point of view. To test the theory, we perform

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29

MacLeod, Morgan, Antonija Oklopčić, Fabienne Nail, and Dion Linssen. "Streams and Bubbles: Tidal Shaping of Hydrodynamic Planetary Outflows." Astrophysical Journal 988, no. 1 (2025): 63. https://doi.org/10.3847/1538-4357/ade0b7.

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Abstract Planets, especially those close to their host stars, lose mass to atmospheric outflows, a process that is thought to shape the bimodal population of gaseous giant and rocky terrestrial exoplanets in close orbits. We model the hydrodynamic escape of planetary atmospheres in idealized, three-dimensional gas dynamic simulations in order to study their emergent morphology. As we vary the simulated system parameters, model outflows show a range of shapes from fast, isotropic outflows bounded by bow shocks to slower motion confined to thin streams. We show that a crucial factor is the role

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30

Kramm, Ulrike, Nadine Nettelmann, and Ronald Redmer. "Constraining planetary interiors with the Love number k2." Proceedings of the International Astronomical Union 6, S276 (2010): 482–84. http://dx.doi.org/10.1017/s1743921311020898.

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AbstractFor the solar sytem giant planets the measurement of the gravitational moments J2 and J4 provided valuable information about the interior structure. However, for extrasolar planets the gravitational moments are not accessible. Nevertheless, an additional constraint for extrasolar planets can be obtained from the tidal Love number k2, which, to first order, is equivalent to J2. k2 quantifies the quadrupolic gravity field deformation at the surface of the planet in response to an external perturbing body and depends solely on the planet's internal density distribution. On the other hand,

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31

Fronsdal, Christian. "Rotating planets in newtonian gravity." Low Temperature Physics 49, no. 2 (2023): 158–70. http://dx.doi.org/10.1063/10.0016840.

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Variational techniques have been used in applications of hydrodynamics in special cases. What is needed is an action that is general enough to deal with potential flows, as well as vortex flows, with rotating fluids, in Nature, and in the laboratory; it has become available only recently. Of special note is a new theory of the sounds of He II. This paper is one of several that aim to test and develop the Action Principle for hydrodynamics in diverse contexts. We study models of rotating planets, compressible fluid bodies in a stationary state of motion, under the influence of a fixed gravitati

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32

Busse, F. H., and R. Simitev. "Dynamos of giant planets." Proceedings of the International Astronomical Union 2, S239 (2006): 467–74. http://dx.doi.org/10.1017/s1743921307000920.

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AbstractPossibilities and difficulties of applying the theory of magnetic field generation by convection flows in rotating spherical fluid shells to the Giant Planets are outlined. Recent progress in the understanding of the distribution of electrical conductivity in the Giant Planets suggests that the dynamo process occurs predominantly in regions of semiconductivity. In contrast to the geodynamo the magnetic field generation in the Giant Planets is thus characterized by strong radial conductivity variations. The importance of the constraint on the Ohmic dissipation provided by the planetary

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Grießmeier, J. M., M. Khodachenko, H. Lammer, J. L. Grenfell, A. Stadelmann, and U. Motschmann. "Stellar activity and magnetic shielding." Proceedings of the International Astronomical Union 5, S264 (2009): 385–94. http://dx.doi.org/10.1017/s1743921309992961.

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AbstractStellar activity has a particularly strong influence on planets at small orbital distances, such as close-in exoplanets. For such planets, we present two extreme cases of stellar variability, namely stellar coronal mass ejections and stellar wind, which both result in the planetary environment being variable on a timescale of billions of years. For both cases, direct interaction of the streaming plasma with the planetary atmosphere would entail servere consequences. In certain cases, however, the planetary atmosphere can be effectively shielded by a strong planetary magnetic field. The

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Egan, Hilary, Riku Jarvinen, Yingjuan Ma, and David Brain. "Planetary magnetic field control of ion escape from weakly magnetized planets." Monthly Notices of the Royal Astronomical Society 488, no. 2 (2019): 2108–20. http://dx.doi.org/10.1093/mnras/stz1819.

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ABSTRACT Intrinsic magnetic fields have long been thought to shield planets from atmospheric erosion via stellar winds; however, the influence of the plasma environment on atmospheric escape is complex. Here we study the influence of a weak intrinsic dipolar planetary magnetic field on the plasma environment and subsequent ion escape from a Mars-sized planet in a global three-dimensional hybrid simulation. We find that increasing the strength of a planet’s magnetic field enhances ion escape until the magnetic dipole’s standoff distance reaches the induced magnetosphere boundary. After this poi

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Kriaa, Quentin, Benjamin Favier, and Michael Le Bars. "Dynamics of snow zones in solidifying planetary cores." Europhysics News 56, no. 1 (2025): 28–31. https://doi.org/10.1051/epn/2025107.

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Iron-rich cores of small rocky planets solidify in original ways. Crystals can form, settle and remelt deep in the core, nourishing fluid motions that may sustain a planetary magnetic field. Interpreting magnetic observations requires advancing the limits of large-scale models and understanding the crucial influence of crystals on the resulting flow.

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Hasegawa, Yasuhiro, Kazuhiro D. Kanagawa, and Neal J. Turner. "Magnetic Fields and Accreting Giant Planets around PDS 70." Astrophysical Journal 923, no. 1 (2021): 27. http://dx.doi.org/10.3847/1538-4357/ac257b.

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Abstract Recent high-spatial/spectral-resolution observations have enabled the formation mechanisms of giant planets to be constrained, especially at the final stages. The current interpretation of such observations is that these planets undergo magnetospheric accretion, suggesting the importance of planetary magnetic fields. We explore the properties of accreting, magnetized giant planets surrounded by their circumplanetary disks, using the physical parameters inferred for PDS 70 b/c. We compute the magnetic field strength and the resulting spin rate of giant planets and find that these plane

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Tachinami, Chihiro, Hiroki Senshu, and Shigeru Ida. "Thermal evolution and magnetism of terrestrial planets." Proceedings of the International Astronomical Union 3, S249 (2007): 159–62. http://dx.doi.org/10.1017/s1743921308016542.

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AbstractWe evaluate a numerical model on the thermal evolution of terrestrial planets to estimate life-time of planetary intrinsic magnetic field for various mass planets. In this model, we take into account the pressure-dependency of density profile of the planet by using Birch-Murnaghun equation of state, and simulate thermal evolution of the planet by means of mixing length theory. According to our numerical results, the planetary mass must be between 0.1 and 1.4 Earth mass to sustain the intrinsic magnetic field for 4.5Gyr. If existence of intrinsic magnetic field were a key factor to make

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Elias-López, Albert, Fabio Del Sordo, Daniele Viganò, et al. "Planetary dynamos in evolving cold gas giants." Astronomy & Astrophysics 696 (April 2025): A161. https://doi.org/10.1051/0004-6361/202453372.

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Context. The discovery of thousands of exoplanets has started a new era of planetary science that expands our ability to characterize diverse planetary features. However, magnetic fields remain one of the least understood aspects of exoplanetary systems. A deeper understanding of planetary dynamos and the evolution of surface magnetic properties throughout the lifetime of a planet is a key scientific purpose. It has implications for planetary evolution, habitability, and atmospheric dynamics. Aims. We modeled the evolution of magnetic fields generated by dynamo action in cold gaseous giant pla

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Sánchez-Lavega, A. "The Magnetic Field in Giant Extrasolar Planets." Astrophysical Journal 609, no. 2 (2004): L87—L90. http://dx.doi.org/10.1086/422840.

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Cridland, A. J. "Magnetically induced termination of giant planet formation." Astronomy & Astrophysics 619 (November 2018): A165. http://dx.doi.org/10.1051/0004-6361/201833611.

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Here a physical model for terminating giant planet formation is outlined and compared to other methods of late-stage giant planet formation. As has been pointed out before, gas accreting into a gap and onto the planet will encounter the planetary dynamo-generated magnetic field. The planetary magnetic field produces an effective cross section through which gas is accreted. Gas outside this cross section is recycled into the protoplanetary disk, hence only a fraction of mass that is accreted into the gap remains bound to the planet. This cross section inversely scales with the planetary mass, w

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Kislyakova, Kristina G. "Electromagnetic induction heating of planets orbiting late M dwarfs." Proceedings of the International Astronomical Union 14, S345 (2018): 232–33. http://dx.doi.org/10.1017/s1743921318008232.

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AbstractWe propose induction heating of planetary interiors as an energy source in the planetary mantles. Induction heating arises when a changing magnetic field induces currents in a conducting planetary mantle which then dissipate to heat the planet, mostly within an upper layer called the skin depth. This physical process can play a role in planetary interiors around strongly magnetized stars such as low mass M dwarfs with kG magnetic fields, which are common among these stars.

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Gazzano, Jean-Christophe, Magali Deleuil, Patrick De Laverny, et al. "From stars to planets." Proceedings of the International Astronomical Union 4, S253 (2008): 404–5. http://dx.doi.org/10.1017/s174392130802677x.

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AbstractA large program of multi-fibre (FLAMES) spectroscopic observations of the stellar population in two CoRoT/Exoplanet field with the GIRAFFE/VLT, took place in spring 2008. It aims at characterizing the brightest dwarf population and providing the ground for statistical analysis of the planetary population found by CoRoT.To perform such an ambitious analysis, we use an automated software based on the MATISSE algorithm, originally designed for the GAIA/RVS spectral analysis. This software derives the atmospheric stellar parameters: effective temperature, surface gravity and the overall me

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Gupta, Sakshi, Arnab Basak, and Dibyendu Nandy. "Impact of Changing Stellar and Planetary Magnetic Fields on (Exo)planetary Environments and Atmospheric Mass Loss." Astrophysical Journal 953, no. 1 (2023): 70. http://dx.doi.org/10.3847/1538-4357/acd93b.

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Abstract The magnetic activity of a star—which modulates the stellar wind outflow—shapes the immediate environments of orbiting (exo)planets and induces atmospheric loss, thereby impacting their habitability. We perform a detailed parameter space study using three-dimensional magnetohydrodynamic simulations to understand the effect of changing stellar wind magnetic field and planetary magnetic field strengths on planetary magnetospheric topology and atmospheric losses. It is observed that the relative strengths of stellar and planetary magnetic fields play a significant role in determining the

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Gunell, Herbert, Romain Maggiolo, Hans Nilsson, et al. "Why an intrinsic magnetic field does not protect a planet against atmospheric escape." Astronomy & Astrophysics 614 (June 2018): L3. http://dx.doi.org/10.1051/0004-6361/201832934.

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The presence or absence of a magnetic field determines the nature of how a planet interacts with the solar wind and what paths are available for atmospheric escape. Magnetospheres form both around magnetised planets, such as Earth, and unmagnetised planets, like Mars and Venus, but it has been suggested that magnetised planets are better protected against atmospheric loss. However, the observed mass escape rates from these three planets are similar (in the approximate (0.5–2) kg s−1 range), putting this latter hypothesis into question. Modelling the effects of a planetary magnetic field on the

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Vidotto, A. A., M. Jardine, J. Morin, J. F. Donati, P. Lang, and A. J. B. Russell. "Planetary protection in the extreme environments of low-mass stars." Proceedings of the International Astronomical Union 9, S302 (2013): 237–38. http://dx.doi.org/10.1017/s1743921314002166.

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AbstractRecent results showed that the magnetic field of M-dwarf (dM) stars, currently the main targets in searches for terrestrial planets, is very different from the solar one, both in topology as well as in intensity. In particular, the magnetised environment surrounding a planet orbiting in the habitable zone (HZ) of dM stars can differ substantially to the one encountered around the Earth. These extreme magnetic fields can compress planetary magnetospheres to such an extent that a significant fraction of the planet's atmosphere may be exposed to erosion by the stellar wind. Using observed

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Riols, A., W. Xu, G. Lesur, M. W. Kunz, and H. Latter. "Gravito-turbulence and dynamo in poorly ionized protostellar discs – I. Zero-net-flux case." Monthly Notices of the Royal Astronomical Society 506, no. 1 (2021): 1407–26. http://dx.doi.org/10.1093/mnras/stab1637.

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ABSTRACT In their early stages, protoplanetary discs are sufficiently massive to undergo gravitational instability (GI). This instability is thought to be involved in mass accretion, planet formation via gas fragmentation, the generation of spiral density waves, and outbursts. A key and very recent area of research is the interaction between the GI and magnetic fields in young protoplanetary discs, in particular whether this instability is able to sustain a magnetic field via a dynamo. We conduct 3D, stratified shearing-box simulations using two independent codes, PLUTO and Athena++, to charac

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47

Mangiorou, Eleni. "Magnetometry in Space Exploration." Key Engineering Materials 644 (May 2015): 266–69. http://dx.doi.org/10.4028/www.scientific.net/kem.644.266.

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Magnetometry in space exploration is a field utilizing physical laws of magnetism and electromagnetism, which studies the magnetosphere of planets and their possible satellites in order to map the planetary or interplanetary magnetic fields and to extract information on the structural composition of the planets (targeting mining mapping) and the complex interactions between the plasma and the solar wind. However, in order to achieve this kind of magnetic measurements based on highly sensitive magnetometers, magnetic cleanliness must be prevailed. This makes necessary the knowledge of the magne

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P. Boss, Alan. "Formation of Planetary-Mass Brown Dwarfs in Magnetic Molecular Clouds." Symposium - International Astronomical Union 211 (2003): 23–26. http://dx.doi.org/10.1017/s007418090021019x.

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Searches for very low mass objects in young star clusters have uncovered evidence for free-floating objects with inferred masses possibly as low as 5 to 15 Jupiter masses (MJup), similar to the masses of several extrasolar planets. We show here that the process which forms single and multiple protostars, namely collapse and fragmentation of molecular clouds, might be able to produce self-gravitating objects with initial masses less than ˜ 1MJup. Models are calculated with a three dimensional, finite differences code which solves the equations of hydrodynamics, gravitation, and radiative transf

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Cuartas-Restrepo, Pablo. "Planetary Magnetic Fields and Habitability in Super Earths." Open Astronomy 27, no. 1 (2018): 183–231. http://dx.doi.org/10.1515/astro-2018-0026.

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Abstract This work seeks to summarize some special aspects of a type of exoplanets known as super-Earths (SE), and the direct influence of these aspects in their habitability. Physical processes like the internal thermal evolution and the generation of a protective Planetary Magnetic Field (PMF) are directly related with habitability. Other aspects such as rotation and the formation of a solid core are fundamental when analyzing the possibilities that a SE would have to be habitable. This work analyzes the fundamental theoretical aspects on which the models of thermal evolution and the scaling

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Grebowsky, Joseph M., and Arthur C. Aikin. "Planetary ionospheres – sources and dynamic drivers." Proceedings of the International Astronomical Union 4, S257 (2008): 499–510. http://dx.doi.org/10.1017/s1743921309029780.

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AbstractExternal energy inputs into all planetary upper atmospheres (including more than a half dozen moons with atmospheres) are comprised of combinations of solar EUV, soft x-rays, solar energetic particles, solar wind charged particles, magnetospherically accelerated particles, solar wind electric field, interplanetary dust particles as well as propagating lower atmosphere disturbances. Each input has analogous physical interactions with all planetary ionospheres and upper atmospheres, but the integrated consequences of the multiple energy inputs vary from planet to planet. The Earth forms

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