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Journal articles on the topic 'Planetary magnetic fields'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Stevenson, David J. "Planetary magnetic fields." Earth and Planetary Science Letters 208, no. 1-2 (2003): 1–11. http://dx.doi.org/10.1016/s0012-821x(02)01126-3.

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2

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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3

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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4

Sabin, L., Q. Zhang, A. A. Zijlstra, et al. "Magnetic fields in Proto Planetary Nebulae." Proceedings of the International Astronomical Union 9, S302 (2013): 398–99. http://dx.doi.org/10.1017/s1743921314002592.

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AbstractThe role of magnetic field in late type stars such as proto-planetary and planetary nebulae (PPNe/PNe), is poorly known from an observational point of view. We present submillimetric observations realized with the Submillimeter Array (SMA) which unveil the dust continuum polarization in the envelopes of two well known PPNe: CRL 618 and OH 231.8+4.2. Assuming the current grain alignment theory, we were then able to trace the geometry of the magnetic field.

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5

Smith, Andy. "Terrestrial, planetary and interplanetary magnetic fields." Astronomy and Geophysics 41, no. 3 (2000): 3.32–3.33. http://dx.doi.org/10.1046/j.1468-4004.2000.00332.x.

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6

Schubert, G., and K. M. Soderlund. "Planetary magnetic fields: Observations and models." Physics of the Earth and Planetary Interiors 187, no. 3-4 (2011): 92–108. http://dx.doi.org/10.1016/j.pepi.2011.05.013.

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7

Stevenson, David J. "Planetary Magnetic Fields: Achievements and Prospects." Space Science Reviews 152, no. 1-4 (2009): 651–64. http://dx.doi.org/10.1007/s11214-009-9572-z.

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8

Jones, Chris A. "Planetary Magnetic Fields and Fluid Dynamos." Annual Review of Fluid Mechanics 43, no. 1 (2011): 583–614. http://dx.doi.org/10.1146/annurev-fluid-122109-160727.

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9

Greaves, J. S. "Toroidal magnetic fields around planetary nebulae." Astronomy & Astrophysics 392, no. 1 (2002): L1—L4. http://dx.doi.org/10.1051/0004-6361:20021002.

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10

Schulz, Michael, and George A. Paulikas. "Planetary magnetic fields: A comparative view." Advances in Space Research 10, no. 1 (1990): 55–64. http://dx.doi.org/10.1016/0273-1177(90)90086-f.

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11

Xu, Shaosui, Janet G. Luhmann, David L. Mitchell, et al. "Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars." Astrophysical Journal Letters 957, no. 2 (2023): L29. http://dx.doi.org/10.3847/2041-8213/ad0784.

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Abstract Mars’s magnetosphere is hybrid, having contributions from both an induced magnetosphere like Venus and the localized crustal magnetic fields. However, the planetary fields also include large-scale, more global components. In this study, we investigate their role in Mars’s magnetospheric topological responses to the interplanetary magnetic field (IMF) clock angle using observations from the Mars Atmospheric Volatile and EvolutioN mission. We show that the large-scale planetary field has a “dipole-like” influence on the Mars global magnetosphere by examining the open field topology. We

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12

D’Angelo, C. Villarreal, M. Schneiter, and A. Esquivel. "On the influence of magnetic fields in neutral planetary wakes." Proceedings of the International Astronomical Union 12, S328 (2016): 192–97. http://dx.doi.org/10.1017/s174392131700388x.

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AbstractWe present a 3D magnetohydrodynamic study of the effect that stellar and planetary magnetic fields have on the calculated Lyα absorption during the planetary transit, employing parameters that resemble the exoplanet HD209458b. We assume a dipolar magnetic field for both the star and the planet, and use the Parker solution to initialize the stellar wind. We also consider the radiative processes and the radiation pressure.We use the numerical MHD code Guacho to run several models varying the values of the planetary and stellar magnetic moments within the range reported in the literature.

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13

Rädler, Karl-Heinz, and Norman F. Ness. "The symmetry properties of planetary magnetic fields." Journal of Geophysical Research 95, A3 (1990): 2311. http://dx.doi.org/10.1029/ja095ia03p02311.

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14

Pascoli, G., and L. Lahoche. "Shaping of Planetary Nebulae by Magnetic Fields." Publications of the Astronomical Society of the Pacific 120, no. 874 (2008): 1267–70. http://dx.doi.org/10.1086/594377.

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15

García-Segura, Guillermo. "MHD Models of Planetary Nebulae: Review." Symposium - International Astronomical Union 209 (2003): 457–64. http://dx.doi.org/10.1017/s0074180900209352.

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When we discuss about MHD effects in planetary nebulae (PNe), there naturally arises a basic question: which magnetic field do we study? One possibility is the ISM magnetic field (e.g. Heiligman 1980), even more if we are concerned with moving PNe (e.g. Soker & Dgani 1997). The next possibility is the internal or stellar magnetic field (Gurzadian 1962). It is important to start this review by quoting Aller (1958): “It has been pointed out by Minkowski and others that the structural appearance of many planetary nebulae strongly suggest the presence of magnetic fields. It seems unlikely that

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16

Vlemmings, Wouter. "Magnetic fields during the evolution towards planetary nebulae." Proceedings of the International Astronomical Union 7, S283 (2011): 176–79. http://dx.doi.org/10.1017/s1743921312010903.

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AbstractMagnetic fields appear ubiquitous throughout the envelopes of evolved stars. However, their origin and role in the formation of planetary nebulae is still unclear. As observations of magnetic fields are complicated and time consuming, the observed samples of AGB and post-AGB stars and planetary nebulae are still small. Still, magnetic energy seems to dominate the energy budget out to a distance of several tens of AU from the central star and the field morphology often appears to be well ordered. A short summary is given of the current observations and the potential of new instruments s

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17

Vlemmings, W. H. T. "Magnetic fields around AGB stars and Planetary Nebulae." Proceedings of the International Astronomical Union 9, S302 (2013): 389–97. http://dx.doi.org/10.1017/s1743921314002580.

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AbstractStars with a mass up to a few solar masses are one of the main contributors to the enrichment of the interstellar medium in dust and heavy elements. However, while significant progress has been made, the process of the mass-loss responsible for this enrichment is still not exactly known and forces beyond radiation pressure might be required. Often, the mass lost in the last phases of the stars life will become a spectacular planetary nebula. The shaping process of often strongly a-spherical PNe is equally elusive. Both binaries and magnetic fields have been suggested to be possible age

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18

Jordan, S., S. Bagnulo, K. Werner, and S. J. O’Toole. "Magnetic fields in central stars of planetary nebulae?" Astronomy & Astrophysics 542 (June 2012): A64. http://dx.doi.org/10.1051/0004-6361/201219175.

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19

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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20

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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21

Nellis, W. J. "The unusual magnetic fields of Uranus and Neptune." Modern Physics Letters B 29, no. 01 (2015): 1430018. http://dx.doi.org/10.1142/s021798491430018x.

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Voyager 2 discovered the unusual non-dipolar and non-axisymmetric magnetic fields of Uranus and Neptune (U/N) in the 1980s. The cause of the unique fields of U/N has been a major scientific question since then. The answer lies in physical properties of fluids that generate planetary magnetic fields by a dynamo: convecting, electrically-conducting fluids at high pressures P and temperatures T in planetary interiors. Fluids in planets at finite temperatures are degenerate condensed matter because of high densities: T/T F ≪1, where T F is Fermi temperature. For metallic fluid H , T/T F ≈0.015. Th

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22

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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23

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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24

Vlemmings, W. H. T. "Maser polarization and magnetic fields." Proceedings of the International Astronomical Union 8, S287 (2012): 31–40. http://dx.doi.org/10.1017/s1743921312006606.

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AbstractMaser polarization observations can reveal unique information on the magnetic field strength and structure for a large number of very different astronomical objects. As the different masers for which polarization is measured, such as silicon-monoxide, water, hydroxil and methanol, probe different physical conditions, the masers can even be used to determine for example the relation between magnetic field and density. In particular, maser polarization observations have improved our understanding of the magnetic field strength in, among others, the envelopes around evolved stars, Planeta

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25

Herpin, Fabrice, A. Baudy, E. Josselin, C. Thum, and H. Wiesemeyer. "Magnetic fields in AGB stars and (proto-) Planetary Nebulae." Proceedings of the International Astronomical Union 4, S259 (2008): 47–52. http://dx.doi.org/10.1017/s1743921309030051.

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AbstractDuring its quick transition to the Planetary Nebula stage, the Asymptotic Giant Branch star will completely change its geometry. This AGB stellar evolution stage is characterized by a high mass loss driven by the radiation pressure. Strong magnetic field may rule the mass loss geometry and the global shaping of these objects. Following our previous work on the polarization of the SiO maser emission in a representative sample of O-rich evolved stars, we present here a study towards C-rich objects and PPN/PN objects to obtain unbiased conclusions. Using Xpol at the IRAM-30 m telescope, w

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26

Zhou, Jingyi, Kaijun Liu, Riku Jarvinen, et al. "Hybrid Simulations of the Martian Magnetotail Twist." Astrophysical Journal 976, no. 1 (2024): 7. http://dx.doi.org/10.3847/1538-4357/ad8159.

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Abstract Three-dimensional global hybrid simulations are performed to explore how the interplanetary magnetic field (IMF), the Martian crustal fields, and planetary pickup ions affect the twisting of the Martian magnetotail. The results agree with previous studies that the crustal magnetic fields cause the Martian magnetotail to twist counterclockwise or clockwise depending on the sign of the IMF Y-component in the Mars solar orbital coordinates. However, the twist is more pronounced when the crustal fields are on the nightside, contradicting the early explanation that the crustal fields affec

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27

Khodachenko, Maxim L., H. Lammer, H. I. M. Lichtenegger, J. M. Grießmeier, M. Holmström, and A. Ekenbäck. "The role of intrinsic magnetic fields in planetary evolution and habitability: the planetary protection aspect." Proceedings of the International Astronomical Union 4, S259 (2008): 283–94. http://dx.doi.org/10.1017/s1743921309030622.

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AbstractThe widely used definition of a habitable zone (HZ) for planets as a circumstellar area, where the star's luminosity is sufficiently intense to maintain liquid water at the surface of a planet, is shown to be too simplified. The role of a host star's activity and the intrinsic magnetic field of a planet with respect to their influence on mass loss processes of close-in gas giants and a definition of a HZ for the terrestrial-type exoplanets are discussed. The stellar X-ray/EUV radiation and the stellar wind result in ionization, heating, chemical modification, and slow erosion of the pl

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28

Steffen, M., S. Hubrig, H. Todt, et al. "Weak magnetic fields in central stars of planetary nebulae?" Astronomy & Astrophysics 570 (October 2014): A88. http://dx.doi.org/10.1051/0004-6361/201423842.

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29

Mizutani, Hitoshi, Tetsuo Yamamoto, and Akio Fujimura. "A new scaling law of the planetary magnetic fields." Advances in Space Research 12, no. 8 (1992): 265–79. http://dx.doi.org/10.1016/0273-1177(92)90397-g.

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30

Sabin, L., Albert A. Zijlstra, and J. S. Greaves. "Magnetic fields in planetary nebulae and post-AGB nebulae." Monthly Notices of the Royal Astronomical Society 376, no. 1 (2007): 378–86. http://dx.doi.org/10.1111/j.1365-2966.2007.11445.x.

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31

Soderlund, Krista M., Eric M. King, and Jonathan M. Aurnou. "The influence of magnetic fields in planetary dynamo models." Earth and Planetary Science Letters 333-334 (June 2012): 9–20. http://dx.doi.org/10.1016/j.epsl.2012.03.038.

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32

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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33

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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34

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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35

Hu, J. Y. "The Magnetic Fields in the Envelopes of Proto-Planetary Nebulae." Symposium - International Astronomical Union 155 (1993): 381. http://dx.doi.org/10.1017/s0074180900171700.

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It is possible that the magnetic field plays important role in the formation of planetary nebulae(Poscoli, 1992). In order to measure the strength of magnetic field in the envelope of protoplanetary nebulae(PPNe) we have used the Max-Planck-Institut fur Radioastronomie 100-m telescope at Effelsberg to obtain the high frequency resolution and high signal-to-noise ratio 1612 MHz spectra of PPNe, IRAS08005-2356, 18276-1431, and 20406+2953 in both circular polarization. The nature of PPN of these objects are confirmed by Slikhuis et al.(1991), Le Bertre(1987), and Hu et al.(1992) based on the exte

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36

Blackman, Eric G. "Magnetic fields in Planetary Nebulae: paradigms and related MHD frontiers." Proceedings of the International Astronomical Union 4, S259 (2008): 35–46. http://dx.doi.org/10.1017/s174392130903004x.

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AbstractMany, if not all, post AGB stellar systems swiftly transition from a spherical to a powerful aspherical pre-planetary nebula (pPNE) outflow phase before waning into a PNe. The pPNe outflows require engine rotational energy and a mechanism to extract this energy into collimated outflows. Just radiation and rotation are insufficient but a symbiosis between rotation, differential rotation and large scale magnetic fields remains promising. Present observational evidence for magnetic fields in evolved stars is suggestive of dynamically important magnetic fields, but both theory and observat

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37

Farrell, W. M., T. Joseph W. Lazio, M. D. Desch, T. S. Bastian, and P. Zarka. "Radio Emission from Extrasolar Planets." Symposium - International Astronomical Union 213 (2004): 73–76. http://dx.doi.org/10.1017/s0074180900193003.

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By virtue of their planetary-scale magnetic fields, the Earth and all of the gas giants in our solar system possess solar-wind deformed magnetospheres. The magnetic polar regions of these “magnetic planets” produce intense, aurora-related radio emission from solar-wind powered electron currents. Simple scaling laws suggest that Jovian-mass planets close to their host stars should produce radio emission; detecting such emission would be the first direct detection of many of these planets. We describe searches using the Very Large Array (VLA) for radio emission from the planets orbiting HD 11476

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38

Uscanga, L., J. F. Gómez, J. A. Green, et al. "Magnetic fields and radio emission processes in maser-emitting planetary nebulae." Proceedings of the International Astronomical Union 13, S336 (2017): 397–98. http://dx.doi.org/10.1017/s1743921317010092.

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AbstractWe present polarimetric observations of the 4 ground-state transitions of OH, toward a sample of maser-emitting planetary nebulae (PNe) using the Australia Telescope Compact Array. This sample includes confirmed OH-emitting PNe, confirmed and candidate H2O-maser-emitting PNe. Polarimetric observations provide information related to the magnetic field of these sources. Maser-emitting PNe are very young PNe and magnetic fields are a key ingredient in the early evolution and shaping process of PNe. Our preliminary results suggest that magnetic field strengths may change very rapidly in yo

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39

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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40

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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41

Jordan, Stefan. "Magnetic fields in White Dwarfs and their direct progenitors." Proceedings of the International Astronomical Union 4, S259 (2008): 369–78. http://dx.doi.org/10.1017/s1743921309030749.

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AbstractThe paper provides an overview on the results of the analyses of spectro-polarimetric observations of white dwarfs, subdwarfs, and central stars of planetary nebulae. It will also discuss the question of the origin of the magnetic fields in white dwarfs.

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42

Carilli, C. L., and G. B. Taylor. "Cluster Magnetic Fields." Annual Review of Astronomy and Astrophysics 40, no. 1 (2002): 319–48. http://dx.doi.org/10.1146/annurev.astro.40.060401.093852.

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43

Stenflo, J. O. "Solar magnetic fields." Journal of Astrophysics and Astronomy 29, no. 1-2 (2008): 19–28. http://dx.doi.org/10.1007/s12036-008-0003-4.

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44

Hazra, Soumitra, Ofer Cohen, and Igor V. Sokolov. "Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations." Astrophysical Journal 936, no. 2 (2022): 144. http://dx.doi.org/10.3847/1538-4357/ac8978.

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Abstract We perform a series of time-dependent magnetohydrodynamic simulations of the HD 189733 star–planet system in order to predict radio transit modulations due to the interaction between the stellar wind and planetary magnetic field. The simulation combines a model for the stellar corona and wind with an exoplanet that is orbiting the star in a fully dynamic, time-dependent manner. Our simulations generate synthetic radio images that enable us to obtain synthetic radio light curves in different frequencies. We find a clear evidence for the planetary motion in the radio light curves. Moreo

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45

Jordan, S., K. Werner, and S. J. O'Toole. "Discovery of magnetic fields in central stars of planetary nebulae." Astronomy & Astrophysics 432, no. 1 (2005): 273–79. http://dx.doi.org/10.1051/0004-6361:20041993.

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46

Runcorn, S. K. "Planetary Magnetic Fields as a Test of the Dynamo Theory." Geophysical Journal of the Royal Astronomical Society 15, no. 1-2 (2007): 183–89. http://dx.doi.org/10.1111/j.1365-246x.1968.tb05757.x.

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47

Simpson, David G., and Adolfo F. Vinas. "NASA Computational Case Study: Modeling Planetary Magnetic and Gravitational Fields." Computing in Science & Engineering 16, no. 4 (2014): 73–79. http://dx.doi.org/10.1109/mcse.2014.78.

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48

Jones, C. A., A. M. Soward, and Keke Zhang. "Dynamics and magnetic fields of the Earth and planetary interiors." Physics of the Earth and Planetary Interiors 128, no. 1-4 (2001): 1. http://dx.doi.org/10.1016/s0031-9201(01)00272-2.

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Lundin, Rickard, Helmut Lammer, and Ignasi Ribas. "Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution." Space Science Reviews 129, no. 1-3 (2007): 245–78. http://dx.doi.org/10.1007/s11214-007-9176-4.

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Vidotto, A. A., M. Jardine, and Ch Helling. "EARLY UV INGRESS IN WASP-12b: MEASURING PLANETARY MAGNETIC FIELDS." Astrophysical Journal 722, no. 2 (2010): L168—L172. http://dx.doi.org/10.1088/2041-8205/722/2/l168.

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