Relevant bibliographies by topics / Magnetic activity / Journal articles
To see the other types of publications on this topic, follow the link: Magnetic activity.

Journal articles on the topic 'Magnetic activity'

Author: Grafiati
Published: 4 June 2021
Last updated: 17 June 2025

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the top 50 journal articles for your research on the topic 'Magnetic activity.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.

1

Strassmeier, K. G., T. A. Carroll, M. Weber, et al. "Binary-induced magnetic activity?" Astronomy & Astrophysics 535 (November 2011): A98. http://dx.doi.org/10.1051/0004-6361/201117167.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Briand, C. "Solar activity I: aspects of magnetic activity." Astronomische Nachrichten 324, no. 4 (2003): 357–61. http://dx.doi.org/10.1002/asna.200310127.

Full text
APA, Harvard, Vancouver, ISO, and other styles
3

Vennerstrom, S., M. Menvielle, J. M. G. Merayo, and T. V. Falkenberg. "Magnetic activity at Mars – Mars Surface Magnetic Observatory." Planetary and Space Science 73, no. 1 (2012): 364–75. http://dx.doi.org/10.1016/j.pss.2012.08.001.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Kahar, Gertrudis V., Abdul Wahid, and Hadi Imam Sutaji. "ANALISIS KEJADIAN BADAI MAGNETIK BERDASARKAN DATA VARIASI HARIAN MAGNETIK DI KOTA KUPANG." Jurnal Fisika : Fisika Sains dan Aplikasinya 3, no. 1 (2018): 12–20. http://dx.doi.org/10.35508/fisa.v3i1.589.

Full text
Abstract:
ABSTRAK
 Telah dilakukan penelitian analisis kejadian badai magnetik di Kota Kupang bulan Oktober 2014 sampai bulan September 2016. Penelitian ini bertujuan untuk menentukan karateristik kejadian badai magnetik serta menentukan periode kemunculan badai magnetik di Kota Kupang. Pengolahan data dengan menggunakan Software Microsoft Excel untuk dibuat grafik data komponen magnet bumi terhadap waktu dan Software Matlab 2011 untuk penentuan periodesitas kejadian badai magnetik menggunakan transformasi fourier cepat (FFT). Berdasarkan hasil pengolahan data, karateristik kejadian badai magnetik yang terdapat di daerah penelitian untuk bulan Oktober 2014 sampai September 2016 adalah untuk tingkat aktivitas gangguan magnetik maksimum ditandai dengan nilai K indeks=8, A indeks=54.875 dan penurunan nilai Dst= -121 nT, sehingga dikategorikan badai menengah dan tingkat aktivitas gangguan magnetik minimum ditandai dengan nilai K indeks=3, A indeks=11.5 serta penurunan nilai Dst = -17 nT, sehingga dikategorikan relatif tenang. Periode kemunculan aktivitas magnetik bulan Oktober 2014-September 2016 adalah berada dalam periode satu harian sampai sepuluh harian. 
 Kata kunci : Variasi harian magnetik, badai magnetik, periodesitas, K indeks, A indeks.
 ABSTRACT 
 The research about analysis of magnetic storm events in Kupang City from October 2014 to September 2016 has been done. The purpose of this study is to determine the characteristic of storm events and the period of emergence magnetic storm from Kupang City. The data used is the daily magnetic variation data obtained from Meteorogical Climatological and Geophysical Agency in Kupang City. The data processing using by Microsoft Excel software to create graph data of the earth magnetic components against time and Matlab 2011 sofware to determining the periodicity of magnetic storm events using Fast Fourier Transform (FFT). From the results of data processing, the characteristic of magnetic storm events in the study area from October 2014 to September 2016 were for the maximum magnetic interference activity level occurring on june 22th, 2015 due to burst of CME marked by the value of K index = 8, A index = 54.875 and degradation value of DST = -121 nT, so category middle storm and minimum magnetic interference activity level occurred on February 10th, 2015 due to burst of CME and flare marked with value K index = 3, A index =11.5, and decreasing value of DST =-17 nT, thus categorized relatively quietly. The period of occurrence magnetic activity from October 2014 to September 2016 is within a period of one daily to ten daily.
 
 Keywords : Daily magnetic variation, magnetic storm, K index, A index.
APA, Harvard, Vancouver, ISO, and other styles
5

Bayraktar, V. N. "MAGNETIC FIELD EFFECT ON YEAST Saccharomyces cerevisiae ACTIVITY AT GRAPE MUST FERMENTATION." Biotechnologia Acta 6, no. 1 (2013): 125–37. http://dx.doi.org/10.15407/biotech6.01.125.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Baishev, Dmitry, and Georgy Makarov. "Isolated substorms according to magnetic measurements at Tixie during minimum solar activity." Solar-Terrestrial Physics 9, no. 4 (2023): 78–82. http://dx.doi.org/10.12737/stp-94202310.

Full text
Abstract:
A catalog of isolated substorms in 2016–2020 has been compiled from data on the H component of the geomagnetic field, obtained at Tixie. From the catalog data, it has been found that during this period changes in the number of substorms and the number of sunspots are well approximated by quadratic functions with minima at the end of 2017 and in the middle of 2019 respectively; during the year, disturbances more often occurred during solstice; within 24 hours, substorms more often occurred at local midnight. The intensity and duration of substorm disturbances, the duration of their expansion phase do not show a noticeable dependence on the time of occurrence; however, from average values of these parameters in hourly ranges, it has been found that the intensity takes lower values around 0–3 MLT; in the midnight sector, the duration of disturbances and the duration of their expansion phase are shorter than those in the dawn sector. Compared to the data from mid-latitude stations [Chu et al., 2015], the average duration of substorms and the duration of their expansion phase are longer.
APA, Harvard, Vancouver, ISO, and other styles
7

Hill, Colin A. "Magnetic activity of interacting binaries." Proceedings of the International Astronomical Union 12, S328 (2016): 54–60. http://dx.doi.org/10.1017/s1743921317004112.

Full text
Abstract:
AbstractInteracting binaries provide unique parameter regimes, both rapid rotation and tidal distortion, in which to test stellar dynamo theories and study the resulting magnetic activity. Close binaries such as cataclysmic variables (CVs) have been found to differentially rotate, and so can provide testbeds for tidal dissipation efficiency in stellar convective envelopes, with implications for both CV and planet-star evolution. Furthermore, CVs show evidence of preferential emergence of magnetic flux tubes towards the companion star, as well as large, long-lived prominences that form preferentially within the binary geometry. Moreover, RS CVn binaries also show clear magnetic interactions between the two components in the form of coronal X-ray emission. Here, we review several examples of magnetic interactions in different types of close binaries.
APA, Harvard, Vancouver, ISO, and other styles
8

Vidotto, A. A. "Stellar magnetic activity and exoplanets." EPJ Web of Conferences 160 (2017): 05011. http://dx.doi.org/10.1051/epjconf/201716005011.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Valdivia, J. A., D. Vassiliadis, A. Klimas, A. S. Sharma, and K. Papadopoulos. "Spatiotemporal activity of magnetic storms." Journal of Geophysical Research: Space Physics 104, A6 (1999): 12239–50. http://dx.doi.org/10.1029/1999ja900152.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

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.

Full text
Abstract:
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 efficiency of this shielding is determined by the planetary magnetic dipole moment, which is difficult to constrain by either models or observations. We present different factors which influence the strength of the planetary magnetic dipole moment. Implications are discussed, including nonthermal atmospheric loss, atmospheric biomarkers, and planetary habitability.
APA, Harvard, Vancouver, ISO, and other styles
11

Sakurai, T., and M. Hagino. "Magnetic helicity and flare activity." Advances in Space Research 32, no. 10 (2003): 1943–48. http://dx.doi.org/10.1016/s0273-1177(03)90630-2.

Full text
APA, Harvard, Vancouver, ISO, and other styles
12

Gnedin, Yu N. "Chromospheres, activity and magnetic fields." Symposium - International Astronomical Union 189 (1997): 245–52. http://dx.doi.org/10.1017/s0074180900116754.

Full text
Abstract:
This brief review presents the current state of observations of stellar activity effects including the fluxes of chromospheric emission lines: CaII H+K, MgII h+k, SiII 1812 Å multiplet, CIV, as well as radio and X-ray fluxes versus B-V colours and luminosity classes, rotation periods, Rossby number and especially versus the mean magnetic flux density 〈fB〉. Results of stellar magnetic field measurements are presented.
APA, Harvard, Vancouver, ISO, and other styles
13

Gray, David F. "Magnetic activity in evolved stars." Advances in Space Research 6, no. 8 (1986): 161–69. http://dx.doi.org/10.1016/0273-1177(86)90429-1.

Full text
APA, Harvard, Vancouver, ISO, and other styles
14

Parker, Eugene N. "Theoretical Interpretation of Magnetic Activity." International Astronomical Union Colloquium 143 (1994): 264–69. http://dx.doi.org/10.1017/s0252921100024763.

Full text
Abstract:
Magnetic fields generated and driven by thermal convection are the primary cause of solar activity. There are many facets of the activity, such as plages, flares, sunspots, coronal heating, and the variation of solar luminosity or irradiance whose nature and cause are understood only partially or not at all, although detailed superficial observational descriptions are available. It is suggested that the inferred 105 gauss azimuthal field bundles may be a direct result of the emergence of Ω-loops to form bipolar magnetic regions on the surface in association with an increase in solar irradiance.
APA, Harvard, Vancouver, ISO, and other styles
15

Tebaldi, C., M. Ottaviani, and F. Porcelli. "Bifurcations and intermittent magnetic activity." Plasma Physics and Controlled Fusion 38, no. 4 (1996): 619–25. http://dx.doi.org/10.1088/0741-3335/38/4/011.

Full text
APA, Harvard, Vancouver, ISO, and other styles
16

Xu, WenYao. "Uncertainty in magnetic activity indices." Science in China Series E: Technological Sciences 51, no. 10 (2008): 1659–64. http://dx.doi.org/10.1007/s11431-008-0261-z.

Full text
APA, Harvard, Vancouver, ISO, and other styles
17

Vahia, M. N., and A. R. Rao. "Magnetic activity in interbinary regions." Advances in Space Research 10, no. 2 (1990): 191–94. http://dx.doi.org/10.1016/0273-1177(90)90140-u.

Full text
APA, Harvard, Vancouver, ISO, and other styles
18

Lundstedt, H. "Solar magnetic activity: Topologically explored." European Physical Journal Conferences 1 (2009): 225–34. http://dx.doi.org/10.1140/epjconf/e2009-00923-x.

Full text
APA, Harvard, Vancouver, ISO, and other styles
19

Järvinen, S. P., H. Korhonen, S. V. Berdyugina, et al. "Magnetic activity on V889 Herculis." Astronomy & Astrophysics 488, no. 3 (2008): 1047–55. http://dx.doi.org/10.1051/0004-6361:200809837.

Full text
APA, Harvard, Vancouver, ISO, and other styles
20

Schrijver, C. J. "Magnetic activity in cool stars." Space Science Reviews 40, no. 1-2 (1985): 3–24. http://dx.doi.org/10.1007/bf00212861.

Full text
APA, Harvard, Vancouver, ISO, and other styles
21

Makarov, V. I., A. A. Ruzmaikin, and S. V. Starchenko. "Magnetic waves of solar activity." Solar Physics 111, no. 2 (1987): 267–77. http://dx.doi.org/10.1007/bf00148519.

Full text
APA, Harvard, Vancouver, ISO, and other styles
22

Wang, Jingxiu. "Driving Layer of Solar Activity." Highlights of Astronomy 12 (2002): 371–77. http://dx.doi.org/10.1017/s1539299600013794.

Full text
Abstract:
AbstractThere should be a driving layer on the Sun, in which the interaction between magnetic field and plasma motion would provide enough magnetic energy and necessary topology for the explosion of solar activity in the corona.Although the exact location of the driving layer is not known, phenomenologically, the photosphere is acting, in many aspects, as the driving layer. Vector magnetic field measurements on the photosphere are greatly needed in clarifying the nature of the driving.Two elementary processes, flux emergence and cancellation, andone basic structure, magnetic interface between topology-independent magnetic loops, are key elements in the driving.
APA, Harvard, Vancouver, ISO, and other styles
23

Vida, K., L. Kriskovics, K. Oláh, et al. "Investigating magnetic activity in very stable stellar magnetic fields." Astronomy & Astrophysics 590 (April 28, 2016): A11. http://dx.doi.org/10.1051/0004-6361/201527925.

Full text
APA, Harvard, Vancouver, ISO, and other styles
24

Nindos, A. "Magnetic helicity ejections and coronal activity." Proceedings of the International Astronomical Union 8, S294 (2012): 519–30. http://dx.doi.org/10.1017/s1743921313003074.

Full text
Abstract:
AbstractMagnetic helicity quantifies the degree of linkage and/or twistedness in the magnetic field. It is probably the only physical quantity which is approximately conserved even in resistive MHD. This makes it an ideal tool for the exploration of the physics of solar eruptions. In this article, I discuss the sources of magnetic helicity injected into active regions and I point out that coronal mass ejections (CMEs) are probably necessary to remove at least part of the excess helicity produced in the Sun. I also discuss the importance of magnetic helicity in the overall coronal evolution that may lead to eruptions.
APA, Harvard, Vancouver, ISO, and other styles
25

NEWITT, L. R., and J. K. WALKER. "Removing magnetic activity from high latitude magnetic repeat station observations." Journal of geomagnetism and geoelectricity 42, no. 8 (1990): 937–49. http://dx.doi.org/10.5636/jgg.42.937.

Full text
APA, Harvard, Vancouver, ISO, and other styles
26

Boro Saikia, Sudeshna, Theresa Lüftinger, and Manuel Guedel. "Magnetic geometry and activity of cool stars." Proceedings of the International Astronomical Union 14, S345 (2018): 341–42. http://dx.doi.org/10.1017/s1743921319001935.

Full text
Abstract:
AbstractStellar magnetic field manifestations such as stellar winds and EUV radiation are the key drivers of planetary atmospheric loss and escape. To understand how the central star influences habitability, it is very important to perform detailed investigation of the star’s magnetic field. We investigate the surface magnetic field geometry and chromospheric activity of 51 sun-like stars. The magnetic geometry is reconstructed using Zeeman Doppler imaging. Chromospheric activity is measured using the Ca II H& K lines. We confirm that the Sun’s large-scale geometry is dominantly poloidal, which is also true for slowly rotating stars. Contrary to the Sun, rapidly rotating stars can have a strong toroidal field and a weak poloidal field. This separation in field geometry appears at Ro=1. Our results show that detailed investigation of stellar magnetic field is important to understand its influence on planetary habitability.
APA, Harvard, Vancouver, ISO, and other styles
27

Krainev, Mikhail. "MANIFESTATIONS OF TWO BRANCHES OF SOLAR ACTIVITY IN THE HELIOSPHERE AND GCR INTENSITY." Solar-Terrestrial Physics 5, no. 4 (2019): 10–20. http://dx.doi.org/10.12737/stp-54201902.

Full text
Abstract:
This paper provides insight into heliospheric processes and galactic cosmic ray (GCR) modulation occurring due to the presence of two branches of solar activity in this solar layer. According to the topology of solar magnetic fields, these branches are called toroidal (active regions, sunspots, flares, coronal mass ejections, etc.) and poloidal (high-latitude magnetic fields, polar coronal holes, zonal unipolar magnetic regions, etc.). The main cause of different manifestations of the two branches on the solar surface and in the heliosphere — the layer at the base of the heliosphere in which the main energetic factor is the magnetic field — is formulated. In this case, the magnetic fields of the poloidal branch, which have a larger scale but a lower intensity, gain an advantage in penetrating into the heliosphere. A connection is shown between the poloidal branch and the heliospheric characteristics (solar wind velocity field, size of the heliosphere, form of the heliospheric current sheet, regular heliospheric magnetic field and its fluctuations) that, according to modern notions, determine GCR propagation in the heliosphere.
APA, Harvard, Vancouver, ISO, and other styles
28

Lundstedt, Henrik. "Solar magnetic activity: topology and prediction." Acta Geophysica 57, no. 1 (2008): 31–41. http://dx.doi.org/10.2478/s11600-008-0062-6.

Full text
APA, Harvard, Vancouver, ISO, and other styles
29

Poppenhaeger,, K. "Stellar magnetic activity – Star-Planet Interactions." EPJ Web of Conferences 101 (2015): 05002. http://dx.doi.org/10.1051/epjconf/201510105002.

Full text
APA, Harvard, Vancouver, ISO, and other styles
30

Trahms, L., S. N. Erne, R. Stehr, E. Seibertz, and A. Friederici. "Multichannel magnetic recording of P300 activity." Physiological Measurement 14, no. 4A (1993): A85—A89. http://dx.doi.org/10.1088/0967-3334/14/4a/015.

Full text
APA, Harvard, Vancouver, ISO, and other styles
31

Gray, David F., and Sallie L. Baliunas. "Magnetic activity variations of epsilon Eridani." Astrophysical Journal 441 (March 1995): 436. http://dx.doi.org/10.1086/175368.

Full text
APA, Harvard, Vancouver, ISO, and other styles
32

Maniewski, R., T. Katila, T. Poutanen, P. Siltanen, T. Varpula, and J. P. Wikswo. "Magnetic measurements of cardiac mechanical activity." IEEE Transactions on Biomedical Engineering 35, no. 9 (1988): 662–70. http://dx.doi.org/10.1109/10.7267.

Full text
APA, Harvard, Vancouver, ISO, and other styles
33

Cowen, R. "Magnetic Activity: A Flare for Research." Science News 142, no. 4 (1992): 54. http://dx.doi.org/10.2307/3976794.

Full text
APA, Harvard, Vancouver, ISO, and other styles
34

Jordan, Carole. "Magnetic Activity in Late-Type Stars." Astronomy & Geophysics 38, no. 2 (1997): 10–14. http://dx.doi.org/10.1093/astrogeo/38.2.10.

Full text
APA, Harvard, Vancouver, ISO, and other styles
35

Shuttleworth, Ian. "The Catalytic Activity of Magnetic Surfaces." Magnetochemistry 10, no. 6 (2024): 40. http://dx.doi.org/10.3390/magnetochemistry10060040.

Full text
Abstract:
High-performance catalysts for the oxygen reduction and hydrogen evolution reactions (ORR and HER, respectively) are highly sought-after, particularly with the commitment of numerous agencies to the removal of conventional gas vehicles in the next few decades. Surprisingly little focus has been placed on the development of magnetic models to describe these systems. The current work will review the current understanding of surface heterogeneous catalysis across select magnetic surfaces, with attention focused on studies involving extended surfaces, which inherently are more accessible to fundamental analysis than the more applied nanoparticle systems. However, even the most up-to-date magnetic variants of this theory have focused on the tight binding limit of the d-band model. In this limit, the reactivity of the surface is governed by the position of the center of the d-band, and the model does not account for the higher moments of the d-band, such as the width, asymmetry, and modality. A summary of the theory supporting this analysis will be presented, along with a summary of the current literature on this level of analysis. The review will then conclude with a discussion of suggested directions for future investigations.
APA, Harvard, Vancouver, ISO, and other styles
36

Strassmeier, Klaus G. "Starspots: signatures of stellar magnetic activity." Proceedings of the International Astronomical Union 4, S259 (2008): 363–68. http://dx.doi.org/10.1017/s1743921309030737.

Full text
Abstract:
AbstractStarspots, just as Sunspots, are among the most obvious tracers and signatures of stellar surface magnetic activity. Emphasized already several decades ago as the origin for the rotationally modulated brightness of cool late-type stars, it is just now that we start to trace individual surface features in great enough detail to understand their magnetic behavior and interaction. Starspots also became the most important “noise” for detecting extra-solar planets and could possibly be decisive when it comes to detect another Earth. Since this is not a review, and because indirect imaging techniques are covered in other papers in this volume, I focus in this paper on some specific detections of starspots and introduce four new facilities particularly suited for starspot research in the near future.
APA, Harvard, Vancouver, ISO, and other styles
37

Montmerle, T. "Magnetic Activity of T Tauri Stars." Highlights of Astronomy 9 (1992): 653–54. http://dx.doi.org/10.1017/s1539299600009941.

Full text
Abstract:
T Tauri stars (TTS) are low-mass (M ≲ 1M⊙) pre-main sequence (PMS) stars (for a general review, see Bertout 1989). They have long been known to be variable from near-TIV to near-IR wavelengths, on timescales ranging from a few minutes to a few decades. They are observed to flare in many wavenlength rages, from X-rays to the radio, and all the existing evidence is consistent with a very strong magnetic activity, in many ways analogous to solar activity (for a review, see, e.g., Montmerle et al. 1991).
APA, Harvard, Vancouver, ISO, and other styles
38

Basri, Gibor. "Magnetic Activity at Very Low Masses." Symposium - International Astronomical Union 219 (2004): 275–84. http://dx.doi.org/10.1017/s0074180900182245.

Full text
APA, Harvard, Vancouver, ISO, and other styles
39

Hawley, Suzanne L. "Magnetic activity in low-mass stars." Publications of the Astronomical Society of the Pacific 105 (September 1993): 955. http://dx.doi.org/10.1086/133262.

Full text
APA, Harvard, Vancouver, ISO, and other styles
40

Vaz, Christopher A., and Nitish V. Thakor. "Monitoring Brain Electrical and Magnetic Activity." IEEE Engineering in Medicine and Biology Magazine 5, no. 3 (1986): 11–15. http://dx.doi.org/10.1109/memb.1986.5006305.

Full text
APA, Harvard, Vancouver, ISO, and other styles
41

Wright, Nicholas J. "Stellar Magnetic Dynamos and Activity Cycles." Proceedings of the International Astronomical Union 9, S302 (2013): 190–93. http://dx.doi.org/10.1017/s1743921314002038.

Full text
Abstract:
AbstractUsing a new uniform sample of 824 solar and late-type stars with measured X-ray luminosities and rotation periods we have studied the relationship between rotation and stellar activity that is believed to be a probe of the underlying stellar dynamo. Using an unbiased subset of the sample we calculate the power law slope of the unsaturated regime of the activity – rotation relationship as LX / Lbol ∝ Roβ, where β = − 2.70 ± 0.13. This is inconsistent with the canonical β = − 2 slope to a confidence of 5σ and argues for an interface-type dynamo. We map out three regimes of coronal emission as a function of stellar mass and age, using the empirical saturation threshold and theoretical super-saturation thresholds. We find that the empirical saturation timescale is well correlated with the time at which stars transition from the rapidly rotating convective sequence to the slowly rotating interface sequence in stellar spin-down models. This may be hinting at fundamental changes in the underlying stellar dynamo or internal structure. We also present the first discovery of an X-ray unsaturated, fully convective M star, which may be hinting at an underlying rotation - activity relationship in fully convective stars hitherto not observed. Finally we present early results from a blind search for stellar X-ray cycles that can place valuable constraints on the underlying ubiquity of solar-like activity cycles.
APA, Harvard, Vancouver, ISO, and other styles
42

Lockwood, D. J., K. R. Hoffman, and W. M. Yen. "Magnetic Raman optical activity in FeF2." Journal of Luminescence 100, no. 1-4 (2002): 147–54. http://dx.doi.org/10.1016/s0022-2313(02)00453-2.

Full text
APA, Harvard, Vancouver, ISO, and other styles
43

Aleksandrova, G. P., L. A. Grishchenko, A. S. Bogomyakov, B. G. Sukhov, V. I. Ovcharenko, and B. A. Trofimov. "Magnetic activity of nanostructured biopolymeric nanomagnets." Russian Chemical Bulletin 59, no. 12 (2010): 2318–22. http://dx.doi.org/10.1007/s11172-010-0394-7.

Full text
APA, Harvard, Vancouver, ISO, and other styles
44

Benevolenskaya, E. E. "Double magnetic cycle of solar activity." Solar Physics 161, no. 1 (1995): 1–8. http://dx.doi.org/10.1007/bf00732080.

Full text
APA, Harvard, Vancouver, ISO, and other styles
45

Soker, N., and R. Tylenda. "Magnetic activity in stellar merger products." Monthly Notices of the Royal Astronomical Society 375, no. 3 (2007): 909–12. http://dx.doi.org/10.1111/j.1365-2966.2006.11351.x.

Full text
APA, Harvard, Vancouver, ISO, and other styles
46

Lundstedt, H. "Wavelet reconstructions of solar magnetic activity." Journal de Physique IV (Proceedings) 139, no. 1 (2006): 167–74. http://dx.doi.org/10.1051/jp4:2006139012.

Full text
APA, Harvard, Vancouver, ISO, and other styles
47

Lanza, A. F. "Hot Jupiters and stellar magnetic activity." Astronomy & Astrophysics 487, no. 3 (2008): 1163–70. http://dx.doi.org/10.1051/0004-6361:200809753.

Full text
APA, Harvard, Vancouver, ISO, and other styles
48

Noyes, Robert W. "Stellar analogs of solar magnetic activity." Solar Physics 100, no. 1-2 (1985): 385–96. http://dx.doi.org/10.1007/bf00158437.

Full text
APA, Harvard, Vancouver, ISO, and other styles
49

Melrose, Donald B., James A. Klimchuk, A. O. Benz, et al. "Commission 10: Solar Activity." Proceedings of the International Astronomical Union 1, T26A (2005): 75–88. http://dx.doi.org/10.1017/s1743921306004388.

Full text
Abstract:
AbstractCommission 10 aims at the study of various forms of solar activity, including networks, plages, pores, spots, fibrils, surges, jets, filaments/prominences, coronal loops, flares, coronal mass ejections (CMEs), solar cycle, microflares, nanoflares, coronal heating etc., which are all manifestation of the interplay of magnetic fields and solar plasma. Increasingly important is the study of solar activities as sources of various disturbances in the interplanetary space and near-Earth “space weather”.Over the past three years a major component of research on the active Sun has involved data from the RHESSI spacecraft. This review starts with an update on current and planned solar observations from spacecraft. The discussion of solar flares gives emphasis to new results from RHESSI, along with updates on other aspects of flares. Recent progress on two theoretical concepts, magnetic reconnection and magnetic helicity is then summarized, followed by discussions of coronal loops and heating, the magnetic carpet and filaments. The final topic discussed is coronal mass ejections and space weather.The discussions on each topic is relatively brief, and intended as an outline to put the extensive list of references in context.The review was prepared jointly by the members of the Organizing Committee, and the names of the primary contributors to the various sections are indicated in parentheses.
APA, Harvard, Vancouver, ISO, and other styles
50

Volwerk, M., M. Delva, Y. Futaana, et al. "Substorm activity in Venus's magnetotail." Annales Geophysicae 27, no. 6 (2009): 2321–30. http://dx.doi.org/10.5194/angeo-27-2321-2009.

Full text
Abstract:
Abstract. The magnetotail of the induced magnetosphere of Venus is investigated through the magnetic field and plasma data of Venus Express. A comparison is made between two neutral sheet crossings. One crossing shows the magnetic field is rather quiet and the plasma instrument indicates a change from energetic (few 100 eV) to low energy (few 10 eV) ions. The other crossing shows more dynamics in the magnetic field, including signatures that are interpreted as characteristic of a reconnection site, and the plasma instrument indicates ions that are energized to 1500 to 2000 eV, in the same magnetospheric region where in the first crossing only low energy ions showed up.
APA, Harvard, Vancouver, ISO, and other styles
You might also be interested in the bibliographies on the topic 'Magnetic activity' for other source types:
Dissertations / Theses Books
We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!

To the bibliography