Relevant bibliographies by topics / Solar magnetic field

Academic literature on the topic 'Solar magnetic field'

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Published: 4 June 2021
Last updated: 7 September 2023

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Journal articles on the topic "Solar magnetic field"

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Korotchenkov, O. O. "Magnetic field-stimulated change of photovoltage in solar silicon crystals." Semiconductor Physics Quantum Electronics and Optoelectronics 16, no. 1 (February 28, 2013): 72–75. http://dx.doi.org/10.15407/spqeo16.01.072.

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Benevolenskaya, E. E. "Solar polar magnetic field." Geomagnetism and Aeronomy 53, no. 7 (November 26, 2013): 891–95. http://dx.doi.org/10.1134/s0016793213070037.

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Solanki, Sami K., Bernd Inhester, and Manfred Schüssler. "The solar magnetic field." Reports on Progress in Physics 69, no. 3 (February 7, 2006): 563–668. http://dx.doi.org/10.1088/0034-4885/69/3/r02.

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Nordlund, Å., and R. F. Stein. "Solar Magnetoconvection." Symposium - International Astronomical Union 138 (1990): 191–211. http://dx.doi.org/10.1017/s0074180900044144.

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As a prelude to discussing the interaction of magnetic fields with convection, we first review some general properties of convection in a stratified medium. Granulation, which is the surface manifestation of the major energy carrying convection scales, is a shallow phenomenon. Below the surface, the topology changes to one of filamentary cool downdrafts, immersed in a gently ascending isentropic background. The granular downflows merge into more widely separated downdrafts, on scales of mesogranulation and super-granulation.The local topology and time evolution of the small scale, kilo Gauss, network and facular magnetic field elements are controlled by convection on the scale of granulation. The topology and time evolution of larger scale magnetic field concentrations are controlled by the hierarchical structure of the horizontal components of the large scale velocity field. In sunspots, the small scale magnetic field structure determines the energy balance, the systematic flows and the waves. Below the surface, the small scale structure of the magnetic field may change drastically, with little observable effect at the surface. We discuss results of some recent numerical simulations of sunspot magnetic fields, and some mechanisms that may be relevant in determining the topology of the sub-surface magnetic field. Finally, we discuss the role of active region magnetic fields in the global solar dynamo.
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Hildebrandt, J., B. Kliem, and A. Krüger. "Solar Coronal Magnetic Fields." Symposium - International Astronomical Union 157 (1993): 59–61. http://dx.doi.org/10.1017/s0074180900173875.

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A short compilation of various radio methods of the determination of magnetic fields in the solar corona is given which, completed by observations in other spectral ranges (e.g. the optical and X-ray ranges), results in a complex picture of the magnetic field. Some topics of interest are the following: (1)Comparison with a standard reference magnetic field in the solar corona,(2)Possible evidence of substantial small-scale fluctuations of the magnetic field (e.g. in active regions),(3)Indication of magnetic fields substantially in excess of the standard distribution (e.g. in limb flare events).
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CHAUHAN, B. C., U. C. PANDEY, and S. DEV. "RSFP PREDICTIONS FOR TRANSVERSE SOLAR MAGNETIC FIELD DISTRIBUTION FROM SOLAR NEUTRINO DATA." Modern Physics Letters A 13, no. 15 (May 20, 1998): 1163–70. http://dx.doi.org/10.1142/s0217732398001236.

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Even though the standard solar model (SSM) has been very successful in predicting the thermal and nuclear evolution of the Sun, it does not throw enough light on solar magnetic activity. In the absence of a generally accepted theory of solar dynamo, various general arguments have been put forth to constrain solar magnetic fields. In the absence of reliable knowledge of solar magnetic fields from available astrophysical data, it may be worthwhile to constrain the solar magnetic fields from solar neutrino observations assuming Resonant Spin-Flavor Precession (RSFP) to be responsible for the solar neutrino deficit. The configuration of solar magnetic field derived in this work is in reasonably good agreement with the magnetic field distribution proposed by Akhmedov et al. (Sov. Phys. JETP68, 250 (1989)). However, the magnetic field distribution in the radiation zone used by Pulido (Phys. Rep.211, 167 (1992)) is ruled out. The magnitude of the magnetic field in the radiation and convective zones of the Sun are very sensitive to the value chosen for the neutrino magnetic moment. However, any change in the value of neutrino magnetic moment does not affect the magnetic field distribution as it only scales the magnetic field strength at different points by the same amount.
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Candelaresi, S., D. I. Pontin, and G. Hornig. "Magnetic field line braiding in the solar atmosphere." Proceedings of the International Astronomical Union 12, S327 (October 2016): 77–81. http://dx.doi.org/10.1017/s1743921317001818.

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AbstractUsing a magnetic carpet as model for the near surface solar magnetic field we study its effects on the propagation of energy injectected by photospheric footpoint motions. Such a magnetic carpet structure is topologically highly non-trivial and with its magnetic nulls exhibits qualitatively different behavior than simpler magnetic fields. We show that the presence of magnetic fields connecting back to the photosphere inhibits the propagation of energy into higher layers of the solar atmosphere, like the solar corona. By applying certain types of footpoint motions the magnetic field topology is is greatly reduced through magnetic field reconnection which facilitates the propagation of energy and disturbances from the photosphere.
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Tobias, Steven, and Niget Weiss. "Solar magnetic field poses problems." Physics World 12, no. 12 (December 1999): 56. http://dx.doi.org/10.1088/2058-7058/12/12/18.

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Демидов, Михаил, and Mikhail Demidov. "Possibilities and problems of solar magnetic field observations for space weather forecast." Solar-Terrestrial Physics 3, no. 1 (May 5, 2017): 26–39. http://dx.doi.org/10.12737/article_58f96ef99d4cd9.20657784.

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An essential part of the space weather problem, important in the last decades, is the forecast of near-Earth space parameters, ionospheric and geomagnetic conditions on the basis of observations of various phenomena on the Sun. Of particular importance are measurements of magnetic fields as they determine the spatial structure of outer layers of the solar atmosphere and, to a large extent, solar wind parameters. Due to lack of opportunities to observe magnetic fields directly in the corona, the almost only source of various models for quantitative calculation of heliospheric parameters are daily magnetograms measured in photospheric lines and synoptic maps derived from these magnetograms. It turns out that results of the forecast, in particular of the solar wind velocity in Earth’s orbit and the position of the heliospheric current sheet, greatly depend not only on the chosen calculation model, but also on the original material because magnetograms from different instruments (and often observations in different lines at the same), although being morphologically similar, may differ significantly in a detailed quantitative analysis. A considerable part of this paper focuses on a detailed analysis of this particular aspect of the problem of space weather forecast.
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Мордвинов, Александр, Aleksandr Mordvinov, Алексей Певцов, Aleksey Pevtsov, Лука Бертелло, Luka Bertello, Гордон Петри, and Gordon Petri. "The reversal of the Sun’s magnetic field in cycle 24." Solar-Terrestrial Physics 2, no. 1 (June 1, 2016): 3–18. http://dx.doi.org/10.12737/19856.

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Analysis of synoptic data from the Vector Spectromagnetograph (VSM) of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) and the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope facility shows that the reversals of solar polar magnetic fields exhibit elements of a stochastic process, which may include the development of specific patterns of emerging magnetic flux, and the asymmetry in activity between Northern and Southern hemispheres. The presence of such irregularities makes the modeling and prediction of polar field reversals extremely hard if possible. In a classical model of solar activity cycle, the unipolar magnetic regions (UMRs) of predominantly following polarity fields are transported polewards due to meridional flows and diffusion. The UMRs gradually cancel out the polar magnetic field of the previous cycle, and rebuild the polar field of opposite polarity setting the stage for the next cycle. We show, however, that this deterministic picture can be easily altered by the developing of a strong center of activity, or by the emergence of an extremely large active region, or by a ‘strategically placed’ coronal hole. We demonstrate that the activity occurring during the current cycle 24 may be the result of this randomness in the evolution of the solar surface magnetic field.
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Dissertations / Theses on the topic "Solar magnetic field"

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Virtanen, I. (. Ilpo). "Asymmetry of the heliospheric magnetic field." Doctoral thesis, University of Oulu, 2013. http://urn.fi/urn:isbn:9789526202563.

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Abstract This thesis studies the structure and evolution of the large scale heliospheric magnetic field. The work covers the space age, the period when satellite measurements revolutionized our knowledge about space. Now, this period is known to be the declining phase of the grand modern maximum of solar activity. The thesis addresses how the hemispherical asymmetry of solar activity is seen in the photospheric magnetic field and how it appears in the corona and in the heliosphere until the termination shock. According to geomagnetic and heliospheric observations, the heliospheric current sheet has been southward shifted around the solar minima since 1930s. Using Ulysses probe observations, we derive an accurate estimate of 2° for the southward shift of the heliospheric current sheet during two very different solar minimum in the mid 1990s and 2000s. The overall structure of the heliospheric magnetic field has changed significantly now when the grand modern maximum has come to an end. During the present low solar activity the polar fields are weaker and the heliospheric current sheet covered a wide latitudinal range during the previous minimum. When the heliospheric current sheet is wide the asymmetry is less visible at the Earth’s orbit. We extend our study to the outer heliosphere using measurements made by Voyager and Pioneer probes and show that the hemispherical asymmetry in the coronal hole evolution, and the related southward shift of the heliospheric current sheet, are seen until the termination shock. In order to understand the origin of the hemispherical asymmetry, we complete a multipole analysis of the solar magnetic field since 1976. We find that the minimum time southward shift of the heliospheric current sheet is due to the quadrupole component of the coronal magnetic field. The quadrupole term exists because the generation and transport of the magnetic flux in the Sun tends to proceed differently in the northern and southern hemispheres. During this and the following decade the Sun is most likely going to be less active than it has been since 1920s. Therefore it is probable that the hemispherical asymmetry of the heliospheric magnetic field will be less visible in the ecliptic plane in the near future. Now, when the Sun seems to be at the maximum of cycle 24, we are looking forward to see how the polar fields and the heliospheric magnetic field are formed when approaching the following solar minimum. It is possible that, as the activity rises again after the present and future low cycles, the hemispherical asymmetry will be opposite to that of the 20th century and the minimum time heliospheric current sheet would be northward shifted.
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Virtanen, I. (Iiro). "Surface flux transport simulations of the photospheric magnetic field." Doctoral thesis, Oulun yliopisto, 2019. http://urn.fi/urn:isbn:9789526223292.

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Abstract This thesis studies the long-term evolution of the photospheric magnetic field using surface flux transport simulations. The photospheric magnetic field and magnetic activity are tightly connected to space weather, and affect the whole heliosphere including the Earth. However, due to a lack of reliable observations our understanding of the long-term evolution of the photospheric magnetic field is still poor. Surface flux transport models, which are capable of simulating the evolution of the whole surface field from observations of solar activity, can be used to study the field in times when direct observations are not available. In this thesis we validate our surface flux transport model, optimize its parameters and test its sensitivity to uncertainties in parameter values and input data. We find a need to extend the model with a decay term to properly model the deep and long minimum between solar cycles 23 and 24, and simulate the photospheric magnetic field of cycles 21–24 using magnetographic observations as input. We also study consequences of hemispherically asymmetric activity, and show that activity in one hemisphere is enough to maintain polar fields in both hemispheres through cross-equatorial flow of magnetic flux. We develop a new method to reconstruct active regions from calcium K line and sunspot polarity observations. We show that this reconstruction is able to accurately capture the correct axial dipole moment of active regions. We study the axial dipole moments of observed active regions and find that a significant fraction of them have a sign opposite to the sign expected from Hale’s and Joy’s laws, proving that the new reconstruction method has an advantage over existing methods that rely on Hale’s and Joy’s laws to define polarities. We show one example of a long simulation covering solar cycles 15–21, demonstrating that using the active region reconstruction and surface flux transport model presented in this thesis it is possible to simulate the large-scale evolution of the photospheric magnetic field over the past century
Original papers The original publications are not included in the electronic version of the dissertation. Virtanen, I. O. I., Virtanen, I. I., Pevtsov, A. A., Yeates, A., & Mursula, K. (2017). Reconstructing solar magnetic fields from historical observations. II. Testing the surface flux transport model. Astronomy & Astrophysics, 604, A8. https://doi.org/10.1051/0004-6361/201730415 http://jultika.oulu.fi/Record/nbnfi-fe2017103050356 Virtanen, I. O. I., Virtanen, I. I., Pevtsov, A. A., & Mursula, K. (2018). Reconstructing solar magnetic fields from historical observations. III. Activity in one hemisphere is sufficient to cause polar field reversals in both hemispheres. Astronomy & Astrophysics, 616, A134. https://doi.org/10.1051/0004-6361/201732323 http://jultika.oulu.fi/Record/nbnfi-fe201902205813 Virtanen, I. O. I., Virtanen, I. I., Pevtsov, A. A., Bertello, L., Yeates, A., & Mursula, K. (2019). Reconstructing solar magnetic fields from historical observations. IV. Testing the reconstruction method. Astronomy & Astrophysics, 627, A11. https://doi.org/10.1051/0004-6361/201935606 http://jultika.oulu.fi/Record/nbnfi-fe2019091828628 Virtanen, I. O. I., Virtanen, I. I., Pevtsov, A. A., & Mursula, K. (2019) Axial dipole moment of solar active regions in cycles 21-24. Manuscript
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Crouch, Ashley D. (Ashley David) 1975. "The interaction of solar oscillations with magnetic field." Monash University, School of Mathematical Sciences, 2003. http://arrow.monash.edu.au/hdl/1959.1/9517.

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McCloughan, John Leslie. "Evolving Synoptic Maps of the solar magnetic field." Thesis, The University of Sydney, 2002. http://hdl.handle.net/2123/485.

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McCloughan, John Leslie. "Evolving Synoptic Maps of the solar magnetic field." University of Sydney. Mathematics and Statistics, 2002. http://hdl.handle.net/2123/485.

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Lee, Daniel Thomas. "Three-dimensional topology of the magnetic field in the solar corona." Thesis, University of Central Lancashire, 2018. http://clok.uclan.ac.uk/25371/.

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This thesis investigates the topology of the magnetic field in the solar corona, due to a variety of source configurations and types. To fully understand the complex behaviour of the Sun's magnetic field, it is important to have a complete description of the features present in its structure. The magnetic topologies due to network source configurations are investigated using both the point source description and the continuous source description. A series of case studies involving an emerging bipole in a hexagonal arrangement to simulate a supergranular cell are studied. This has a particular focus on the behaviour of coronal nulls located in the topology, and a particular case may form the underpinning of a model for polar plumes. A new topological feature, called a null-like point, is defined by relaxing the definition of a magnetic null point. Separatix-like surfaces, originating from null-like points, allow quasi-separatrix layers to be found in magnetic topologies due to continuously distributed sources. The squashing factor, Q, is mapped across the source configuration, highlighting the locations of the quasi-separatrix layers. Finally, an algorithm is developed which automatically detects and classifies magnetic events local to X-ray bright points (XBPs). Significant peaks are identified in the gradients of flux curves (positive, negative and absolute flux) local to XBP footpoints, allowing instances of flux emergence and cancellation to be identified and linked to the onset and demise of the XBPs studied. The algorithm correctly classifies 90% of all emergence and cancellation events related to the studied XBPs.
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Kemel, Koen. "From mean-field hydromagnetics to solar magnetic flux concentrations." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2012. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-80817.

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The main idea behind the work presented in this thesis is to investigate if it is possible to find a mechanism that leads to surface magnetic field concentrations and could operate under solar conditions without postulating the presence of magnetic flux tubes rising from the bottom of the convection zone, a commonly used yet physically problematic approach. In this context we study the ‘negative effective magnetic pressure effect’: it was pointed out in earlier work (Kleeorin et al., 1989) that the presence of a weak magnetic field can lead to a reduction of the mean turbulent pressure on large length scales. This reduction is now indeed clearly observed in simulations. As magnetic fluctuations experience an unstable feedback through this effect, it leads, in a stratified medium, to the formation of magnetic structures, first observed numerically in the fifth paper of this thesis. While our setup is relatively simple, one wonders if this instability, as a mechanism able to concentrate magnetic fields in the near surface layers, may play a role in the formation of sunspots, starting from a weak dynamo-generated field throughout the convection zone rather than from strong flux tubes stored at the bottom. A generalization of the studied case is ongoing.

At the time of the the doctoral defence the following paper was unpublished and had a status as follows: Paper nr 7: Submitted

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Gilchrist, Stuart. "Data-driven numerical modelling of the solar coronal magnetic field." Thesis, The University of Sydney, 2013. http://hdl.handle.net/2123/10217.

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The aim of this thesis is the development of numerical models for determining the coronal magnetic field from observations of the magnetic field at the photosphere (coronal magnetic field extrapolation), with an emphasis on numerical methods, computation and code development. Presently, observational methods cannot determine the coronal magnetic field accurately and routinely, motivating numerical modelling. In this thesis we develop improvements to the widely used force-free model of the coronal magnetic field. In Chapter 1 we present motivation for the modelling and its limitations. In Chapter 2 we present free energy estimates for the solar active region AR 11029 derived from a force-free model applied to data from the Hinode Spectropolarimeter and the Synoptic Optical Long-term Investigations of the Sun Vector-Spectromagnetograph. The work illustrates many of the difficulties with modelling discussed in Chapter 1. In Chapter 3 we present a numerical code for solving a magneto-hydrostatic model of the corona which includes pressure forces in the corona. The code is applied to a simple test case to demonstrate its correctness. In Chapter 4 we present a numerical code for solving the nonlinear force-free model in spherical polar coordinates which overcomes the limitations of the Cartesian models. The code is an implementation of the Grad-Rubin method, and is based on a spectral representation of the magnetic field in terms of vector-spherical harmonics. The method is applied to a simple test case to demonstrate the self-consistency of the implementation. In Chapter 5 we derive the vector-spherical harmonic solution to Ampere's law which is presented in Chapter 4 without derivation. This solution forms an important part of the spherical code presented in Chapter 4.
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Mackay, Duncan Hendry. "Basic magnetic field configurations for solar filament channels and filaments." Thesis, University of St Andrews, 1997. http://hdl.handle.net/10023/14188.

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The three-dimensional magnetic structure of solar filament channels and filaments is considered. A simple analytical potential model of a filament channel is setup with line sources representing the overlying arcades and point sources the flux of the filament. A possible explanation of the distinct upper and lower bounds of a filament is given. A more detailed numerical force-free model with discrete flux sources is then developed and the effect of magnetic shear on the separatrix surface explored. Dextral channels are shown to exist for a wider range of negative values of the force-free alpha and sinistral channels for positive values of alpha. Potential models of a variety of coronal structures are then considered. The bending of a filament is modelled and a method of determining the horizontal component of a filament's magnetic field is proposed. Next, the observed opposite skew of arcades lying above switchbacks of polarity inversion lines is shown to be produced by a local flux imbalance at the corner of the switchback. Then, the magnetic structure of a particular filament in a filament channel is modelled using observations from a photospheric magnetogram. It is shown that dips in the filaments magnetic field could result from opposite polarity fragments lying below the filament. Finally, the formation of a specific filament channel and filament is modelled. The formation of the channel is shown to be due to the emergence of new flux in a sheared state. It is shown that convergence and reconnections between the new flux and old remnant flux is required for the filament to form. The field lines that represent the filament form a thin vertical sheet of flux. The changing angle of inclination of the sheet gives the appearance of twist. The method of formation is then generalised to other cases and it is shown that a hemispheric pattern consistent with the results of Martin et al. (1995) can be obtained.
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Lothian, Robert M. "Aspects of magnetic field theory in solar and laboratory plasmas." Thesis, University of St Andrews, 1990. http://hdl.handle.net/10023/14183.

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Using the Magnetohydrodynamic model, two problems in the behaviour of magnetic field structures are investigated. Firstly, the stability of tokamak equilibria to coupled tearing modes is calculated. Secondly, the equilibrium structure of a solar coronal loop is examined. The flux co-ordinate method is used to construct toroidal equilibria of the type found in large aspect ratio tokamaks. In such a field configuration, the analysis of tearing modes is complicated by the coupling of different poloidal fourier modes. The effect of coupling through elliptic shaping of plasma surfaces is calculated. For certain current profiles, this effect may cause instability. The response of coronal loops to twisting at their photospheric footpoints is investigated. Long loops are shown to have an essentially 1-D nature. This observation is used to develop a 1-D, line-tied model for such loops. This model is used to conduct an extensive survey of the non-linear twist regime, including the effects of enhanced fluid pressure. The possibility of non-equilibrium, which would provide energy for coronal heating and compact flares, is examined. When the physical variable of footpoint displacement is specified, no loss of equilibrium is found by twisting. Loss of equilibrium is found for high pressures, which we do not, however, expect to find in the corona.
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Books on the topic "Solar magnetic field"

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Berger, T. E. On the dynamics of small-scale solar magnetic elements. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Berger, T. E. On the dynamics of small-scale solar magnetic elements. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Berger, T. E. On the dynamics of small-scale solar magnetic elements. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Berger, T. E. On the dynamics of small-scale solar magnetic elements. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Hoeksema, Jon Todd. The solar magnetic field, 1976 through 1985: An atlas of photospheric magnetic field observations and computed coronal magnetic fields from the John M. Wilcox Solar Observatory at Stanford, 1976-1985. Boulder, CO, USA (325 Broadway, Boulder 80303): U.S. Dept. of Commerce, National Oceanic and Atmospheric Administration, National Environmental Satellite, Data, and Information Service, National Geophysical Data Center, 1986.

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Matthaeus, W. H. An interplanetary magnetic field ensemble at 1 AU. Greenbelt, Md: National Aeronautics and Space Administration, Goddard Space Flight Center, 1985.

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Spiro, Antiochos, and United States. National Aeronautics and Space Administration., eds. The Solar-B mission: Final report of the Science Definition Team. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Hagyard, M. J. Nonpotential magnetic fields at sites of gamma-ray flares. [Huntsville, Ala.?: Marshall Space Flight Center, 1988.

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Brosius, Jeffrey W. "Plasma properties and magnetic field structure of the solar corona, based on coordinated Max '91 observations fron SERTS, the VLA, and magnetographs": Annual report of work progress on NASA grant NASW-4933 covering the period 12 July 1994 - 11 July 1995. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Brosius, Jeffrey W. Plasma properties and magnetic field structure of the solar corona, based on coordinated Max '91 observations fron SERTS, the VLA, and magnetographs. [Washington, D.C.]: National Aeronautics and Space Administration, 1995.

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Book chapters on the topic "Solar magnetic field"

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Zhang, Hongqi. "Measurements of Solar Magnetic Field." In Solar Magnetism, 1–116. Singapore: Springer Nature Singapore, 2023. http://dx.doi.org/10.1007/978-981-99-1759-4_1.

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Zhang, Hongqi. "Helical Magnetic Field and Solar Cycles." In Solar Magnetism, 265–323. Singapore: Springer Nature Singapore, 2023. http://dx.doi.org/10.1007/978-981-99-1759-4_5.

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Stenflo, Jan Olof. "Introduction to Quantum Field Theory of Polarized Radiative Transfer." In Solar Magnetic Fields, 127–48. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-015-8246-9_7.

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Bolonkin, Alexander A. "Artificial Magnetic Field for Venus." In Inner Solar System, 383–93. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-19569-8_17.

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Čadež, V. M., A. Debosscher, M. Messerotti, P. Zlobec, M. Iurcev, and A. Santin. "Theoretical Modeling of Potential Magnetic Field Distribution in the Corona above Axially Symmetric Photospheric Active Regions in a Uniform Magnetic Field." In Solar Magnetic Phenomena, 279–82. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-2962-4_35.

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Makarchik, D. V., and N. I. Kobanov. "Line-of-Sight Velocity and Magnetic Field in Sunspot Penumbrae." In Solar Magnetic Phenomena, 219–22. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-2962-4_20.

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Petrovay, Kristóf. "Theory of Passive Magnetic Field Transport." In Solar Surface Magnetism, 415–40. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1188-1_35.

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Morschhauser, Achim, Foteini Vervelidou, Paul Thomas, Matthias Grott, Vincent Lesur, and Stuart A. Gilder. "Mars’ Crustal Magnetic Field." In Magnetic Fields in the Solar System, 331–56. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-64292-5_12.

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Kim, I. S. "Observing the Solar Magnetic Field." In Advances in Solar Research at Eclipses from Ground and from Space, 67–83. Dordrecht: Springer Netherlands, 2000. http://dx.doi.org/10.1007/978-94-011-4325-7_5.

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Nagabhushana, B. S. "Estimation of Magnetic Field Components in Prominence Using Magneto Hydrodynamic Model." In Solar Polarization, 421–30. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-015-9329-8_36.

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Conference papers on the topic "Solar magnetic field"

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Merzlyakov, V. L., and L. I. Starkova. "SOLAR CORONA EFFECTS OF MAGNETIC FIELD GENERATION." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2019. http://dx.doi.org/10.31725/0552-5829-2019-293-296.

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Zimbardo, G. "Magnetic Turbulence, Fast Magnetic Field line Diffusion and Small Magnetic Structures in the Solar Wind." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618623.

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Schatten, Kenneth H. "Coronal and interplanetary magnetic field models." In The solar wind nine conference. AIP, 1999. http://dx.doi.org/10.1063/1.58780.

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Derteev, S. B., B. B. Mikhalyaev, and L. N. Dzhimbeeva. "MODEL OF CME WITH A HELICAL MAGNETIC FIELD." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2019. http://dx.doi.org/10.31725/0552-5829-2019-145-148.

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Zhivanovich, I., and A. A. Solov’ev. "DISTRIBUTION OF MAGNETIC FIELD IN BIPOLAR SUNSPOT GROUPS." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2019. http://dx.doi.org/10.31725/0552-5829-2019-173-176.

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Vernova, E. S., M. I. Tyasto, and D. G. Baranov. "FLOWS OF MAGNETIC FIELD IN THE SUN’S PHOTOSPHERE." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2021. http://dx.doi.org/10.31725/0552-5829-2021-79-82.

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Ratkiewicz, Romana. "Interstellar magnetic field effects on the heliosphere." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618700.

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Vandas, M., and E. P. Romashets. "Magnetic field disturbance in front of a super-sonic toroidal magnetic cloud." In SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4811043.

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Merzlyakov, V. L., and L. I. Starkova. "EVOLUTION CHANGES OF MAGNETIC FIELD STRUCTURE OF SOLAR CORONA." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2018. http://dx.doi.org/10.31725/0552-5829-2018-287-290.

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Zhivanovich, I., A. A. Osipova, P. V. Strekalova, and V. G. Ivanov. "INTERPLANETARY MAGNETIC FIELD VARIATIONS ON THE LONG TIME SCALES." In All-Russia Conference on Solar and Solar-Terrestrial Physics. The Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo, 2019. http://dx.doi.org/10.31725/0552-5829-2019-165-168.

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Reports on the topic "Solar magnetic field"

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Cliver, E. W., and A. G. Ling. The Floor in the Solar Wind Magnetic Field Revisited. Fort Belvoir, VA: Defense Technical Information Center, May 2012. http://dx.doi.org/10.21236/ada562846.

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Harvey, John, and Frank Hill. Improvement of Solar Magnetic Field Data for Space Weather Applications. Fort Belvoir, VA: Defense Technical Information Center, September 2011. http://dx.doi.org/10.21236/ada623786.

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Asenovski, Simeon. Investigation of the Different Periods Characterizing Solar Magnetic Field Reversals. "Prof. Marin Drinov" Publishing House of Bulgarian Academy of Sciences, July 2021. http://dx.doi.org/10.7546/crabs.2021.07.09.

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Ulrich, Roger K. Synoptic Solar Magnetic and Velocity Field Observations Using the 150-Foot Solar Tower on Mt. Wilson. Fort Belvoir, VA: Defense Technical Information Center, March 1991. http://dx.doi.org/10.21236/ada263485.

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Nikolic, L. Modelling the magnetic field of the solar corona with potential-field source-surface and Schatten current sheet models. Natural Resources Canada/ESS/Scientific and Technical Publishing Services, 2017. http://dx.doi.org/10.4095/300826.

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Branduardi-Raymont, Graziella, and et al. SMILE Definition Study Report. ESA SCI, December 2018. http://dx.doi.org/10.5270/esa.smile.definition_study_report-2018-12.

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Abstract:
The SMILE definition study report describes a novel self-standing mission dedicated to observing solar wind-magnetosphere coupling via simultaneous in situ solar wind/magnetosheath plasma and magnetic field measurements, X-Ray images of the magnetosheath and magnetic cusps, and UV images of global auroral distributions defining system-level consequences. The Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) will complement all solar, solar wind and in situ magnetospheric observations, including both space- and ground-based observatories, to enable the first-ever observations of the full chain of events that drive the Sun-Earth connection.
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G.S. Choe and C.Z. Cheng. A Model of Solar Flares Based on Arcade Field Reconnection and Merging of Magnetic Islands. Office of Scientific and Technical Information (OSTI), December 2001. http://dx.doi.org/10.2172/792994.

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Richardson, I. G., E. W. Cliver, and H. V. Cane. Long-Term Trends in Interplanetary Magnetic Field Strength and Solar Wind Structure During the Twentieth Century. Fort Belvoir, VA: Defense Technical Information Center, October 2002. http://dx.doi.org/10.21236/ada423110.

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Cliver, E. W., G. J. Petrie, and A. G. Ling. Abrupt Changes of the Photospheric Magnetic Field in Active Regions and the Impulsive Phase of Solar Flares (Preprint). Fort Belvoir, VA: Defense Technical Information Center, August 2012. http://dx.doi.org/10.21236/ada566133.

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Cliver, E. W., G. J. Petrie, and A. G. Ling. Abrupt Changes of the Photospheric Magnetic Field in Active Regions and the Impulsive Phase of Solar Flares (Postprint). Fort Belvoir, VA: Defense Technical Information Center, August 2012. http://dx.doi.org/10.21236/ada599264.

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