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Journal articles on the topic 'Radio field strength'

Author: Grafiati

Published: 3 June 2025

Last updated: 31 July 2025

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1

Zhang, Yu, and Hui-Chun Wu. "Upper Field-strength Limit of Fast Radio Bursts." Astrophysical Journal 929, no. 2 (2022): 164. http://dx.doi.org/10.3847/1538-4357/ac5e2f.

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Abstract Fast radio bursts (FRBs) are cosmological radio transients with an unclear generation mechanism. Known characteristics such as their luminosity, duration, spectrum, and repetition rate, etc., suggest that FRBs are powerful coherent radio signals at GHz frequencies, but the status of FRBs near the source remains unknown. As an extreme astronomical event, FRBs should be accompanied by energy-comparable or even more powerful X/γ-ray counterparts. Here, particle-in-cell simulations of ultrastrong GHz radio pulse interaction with GeV photons show that at ≳3 × 1012 V cm−1 field strengths, q

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2

Zhang, Yu, and Hui-Chun Wu. "Upper Field-strength Limit of Fast Radio Bursts." Astrophysical Journal 929, no. 2 (2022): 164. http://dx.doi.org/10.3847/1538-4357/ac5e2f.

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Abstract Fast radio bursts (FRBs) are cosmological radio transients with an unclear generation mechanism. Known characteristics such as their luminosity, duration, spectrum, and repetition rate, etc., suggest that FRBs are powerful coherent radio signals at GHz frequencies, but the status of FRBs near the source remains unknown. As an extreme astronomical event, FRBs should be accompanied by energy-comparable or even more powerful X/γ-ray counterparts. Here, particle-in-cell simulations of ultrastrong GHz radio pulse interaction with GeV photons show that at ≳3 × 1012 V cm−1 field strengths, q

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3

Beck, Rainer. "Measuring interstellar magnetic fields by radio synchrotron emission." Proceedings of the International Astronomical Union 4, S259 (2008): 3–14. http://dx.doi.org/10.1017/s1743921309030014.

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AbstractRadio synchrotron emission, its polarization and its Faraday rotation are powerful tools to study the strength and structure of interstellar magnetic fields. The total intensity traces the strength and distribution of total magnetic fields. Total fields in gas-rich spiral arms and bars of nearby galaxies have strengths of 20–30 μGauss, due to the amplification of turbulent fields, and are dynamically important. In the Milky Way, the total field strength is about 6 μG near the Sun and several 100 μG in filaments near the Galactic Center. – The polarized intensity measures ordered fields

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4

Gao, Zhisheng, Yaoshun Li, and Chunzhi Xie. "Parameter Estimation for the Field Strength of Radio Environment Maps." Wireless Communications and Mobile Computing 2017 (2017): 1–13. http://dx.doi.org/10.1155/2017/2475439.

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The parameters of a radio environment map play an important role in radio management and cognitive radio. In this paper, a method for estimating the parameters of the radio environment map based on the sensing data of monitoring nodes is presented. According to the principles of radio transmission signal intensity losses, a theoretical variogram model based on a propagation model is proposed, and the improved theoretical variation function is more in line with the attenuation of radio signal propagation. Furthermore, a weight variogram fitting method is proposed based on the characteristics of

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5

Jayati, Ari Endang, Wahyu Minarti, and Sri Heranurweni. "Analisa Teknis Penetapan Kanal Frekuensi Radio Untuk Lembaga Penyiaran Radio Komunitas Wilayah Kabupaten Batang." Jurnal ELTIKOM 5, no. 2 (2021): 73–80. http://dx.doi.org/10.31961/eltikom.v5i2.361.

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The radio frequency spectrum constitutes a limited and strategic natural resource with high economic value, so it must be managed effectively and efficiently to obtain optimal benefits by observing national and international legal principles. Radio Community Broadcasting Institution uses limited frequency allocation in three channels, namely, in the frequency channels 202 (107.7 MHz), 203 (107.8 MHz), and 204 (107.9 MHz), with limited transmit power and area coverage. The problem in this research is the frequency overlap with other community radios in an area. The issue raised is whether it is

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6

Tsedilina, E. E. "HF radio field strength and total propagation invariants." Radio Science 29, no. 1 (1994): 127–34. http://dx.doi.org/10.1029/93rs02502.

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7

Krause, Marita. "Magnetic Fields and Halos in Spiral Galaxies." Galaxies 7, no. 2 (2019): 54. http://dx.doi.org/10.3390/galaxies7020054.

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Radio continuum and polarization observations reveal best the magnetic field structure and strength in nearby spiral galaxies. They show a similar magnetic field pattern, which is of spiral shape along the disk plane and X-shaped in the halo, sometimes accompanied by strong vertical fields above and below the central region of the disk. The strength of the total halo field is comparable to that of the disk. The small- and large-scale dynamo action is discussed to explain the observations with special emphasis on the rôle of star formation on the α − Ω dynamo and the magnetic field strength and

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8

Adekunle, Titus Adediji, Oluwadare Adebusola Samuel, and Sunday Ojo Joseph. "Variability of Microwave Radio Refractivity and Field Strength over Some Selected Locations in Nigeria." Physical Science International Journal 14, no. 3 (2017): 1–11. https://doi.org/10.9734/PSIJ/2017/33447.

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In this study, results of the variation of radio field strength derived from the computation of surface refractivity through measurements of temperature, relative humidity and pressure across seven locations ((Akure (7<em>.</em>15°N<em>, </em>5<em>.</em>12°E<em>)</em>, Lagos (6.30°N, 3.20°E), Abuja (7.10°N, 9.25°E), Jos (9.50°N, 8.50°E), Makurdi (7.30°N, 8.53°E), Port-Harcourt (4.20°N, 7.00°E), and Nsukka (6.90°N, 7.67°E)) in Nigeria are presented. Two years (Jan., 2011–Dec., 2012) archived data as provided by Tropospheric Data Acquisition Network (TRODAN) of the Centre for Atmospheric Researc

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Ibrahim, U., Bawa Musa, and M. Lawal. "Estimating the Variability of Tropospheric Radio Refractivity and Field Strength over Enugu, South-East Nigeria." International Journal of Science for Global Sustainability 10, no. 2 (2024): 251–57. http://dx.doi.org/10.57233/ijsgs.v10i2.678.

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The field strength variability (FSV) assessment highlights the significant impact of atmospheric conditions on radio signal propagation. A diurnal variation in radio refractivity is the primary driver of FSV, with local topography and environmental factors also playing important roles. This study investigated the variation of tropospheric radio refractivity and field strength in Enugu, South-East Nigeria. Through a comprehensive measurement of temperature, humidity and pressure obtained from the network of Vantage Pro 2 automatic weather station installed at the study location for a period of

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10

Sarma, SBSS. "Estimation of Magnetic Field Strength from Enhanced Solar Radio Emission." Australian Journal of Physics 47, no. 6 (1994): 811. http://dx.doi.org/10.1071/ph940811.

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The manifestation of solar activity on radio noise records at 28.6 MHz is discussed with special emphasis on Type-I noise storms and the associated coronal magnetic fields above the active regions in time. Magnetic fields are estimated, assuming that the Type-I radio emission at decametre wavelengths is due to shock waves, by making use of the observed shock velocity. The results are comparable with the existing estimates.

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11

Gelfreikh, G. B., V. M. Bogod, V. E. Abramov-Maximov, and S. V. Tsvetkov. "Measurements of Solar Magnetic Fields Using Radio Observations with the RATAN-600." International Astronomical Union Colloquium 141 (1993): 271–74. http://dx.doi.org/10.1017/s0252921100029213.

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AbstractThree ways of measuring magnetic fields in the corona and chromosphere have been developed based on spectral polarization observations with high spatial resolution using the radio telescope RATAN-600. The methods rely on effects from the theory of the generation and propagation of microwaves in the solar atmosphere: thermal bremsstrahlung, thermal cyclotron emission, and inversion of the polarization sign in quasi-transverse field regions. The new radio spectrograph (PAS) at the RATAN-600 resulted in higher accuracy measurements of the strength and structure of coronal magnetic fields.

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12

Adediji, A. T., J. S. Ojo, and O. A. Abimbola. "Chaotic characteristics of microwave radio field strength over Nigeria." Journal of Physics: Conference Series 2034, no. 1 (2021): 012024. http://dx.doi.org/10.1088/1742-6596/2034/1/012024.

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13

GEVEKE, DAVID J., and CHRISTOPHER BRUNKHORST. "Inactivation of Saccharomyces cerevisiae with Radio Frequency Electric Fields†." Journal of Food Protection 66, no. 9 (2003): 1712–15. http://dx.doi.org/10.4315/0362-028x-66.9.1712.

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The application of radio frequency (RF) electric fields as a nonthermal alternative to thermal inactivation of microorganisms in liquids was investigated. A novel RF system producing frequencies in the range of 20 to 60 kHz was developed. Electric field strengths of 20 and 30 kV/cm were applied to suspensions of Saccharomyces cerevisiae in water over a temperature range of 35 to 55°C. The flow rate was 1.2 liters/min. The S. cerevisiae population was reduced by 2.1 ± 0.1 log units following exposure to a 30-kV/cm field at 40°C. The results of the present study provide the first evidence that s

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14

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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15

Kim, Vitaliy, Adel Umirbayeva, and Yerlan Aimuratov. "Estimates of the Surface Magnetic Field Strength of Radio Pulsars." Universe 9, no. 7 (2023): 334. http://dx.doi.org/10.3390/universe9070334.

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We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle (β) between the spin and magnetic dipole axes of a neutron star (NS) in the ejector stage is considered within the frame of the magnetic dipole energy loss mechanism. We estimate the surface magnetic field strength (Bns) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated Bns(β) may differ by an order of magnitude from the values without considering the angle β. It is shown that Bns(β) lies in the range 108–1014G for a known population of s

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16

Govoni, Federica, and Matteo Murgia. "Magnetic Fields in Galaxy Clusters." Highlights of Astronomy 13 (2005): 322–26. http://dx.doi.org/10.1017/s1539299600015884.

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AbstractMagnetic fields in galaxy clusters can be investigated using a variety of techniques. Recent studies including radio halos, Inverse Compton hard X-ray emissions and Faraday rotation measure, are briefly outlined. A numerical approach for investigating cluster magnetic fields strength and structure is presented. It consists of producing simulated rotation measure, radio halo images, and radio halo polarization, obtained from 3-dimensional multi-scale cluster magnetic field models, and comparing with observations.

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17

Adediji, Adekunle Titus, Mahamod Ismail, and Jit Singh Mandeep. "Performance Analysis of Microwave Radio Refractivity on Radio Field Strength and Radio Horizon Distance Over Akure, Nigeria." Wireless Personal Communications 79, no. 3 (2014): 1893–909. http://dx.doi.org/10.1007/s11277-014-1963-0.

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18

Bartelmann, Matthias, Klaus Dolag, and Harald Lesch. "The Evolution of Magnetic Fields in Galaxy Clusters." Symposium - International Astronomical Union 208 (2003): 189–98. http://dx.doi.org/10.1017/s0074180900207146.

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Cosmological simulations of magnetic fields in galaxy clusters show that remarkable agreement between simulations and observations of Faraday rotation and radio haloes can be achieved assuming that seed fields of ∼ 10−9 G were present at redshifts ∼ 15−20. The structure of the seed field is irrelevant for the final intracluster field. On average, the field grows exponentially with decreasing cluster redshift, but merger events cause steep transient increases in the field strength. Typical field-reversal scales are of order 50h−1kpc. In most cases, the intracluster fields are dynamically unimpo

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19

Adediji, A. T., Mahamod Ismail, and J. S. Mandeep. "Variation of radio field strength and radio horizon distance over three stations in Nigeria." Journal of Atmospheric and Solar-Terrestrial Physics 109 (March 2014): 1–6. http://dx.doi.org/10.1016/j.jastp.2013.12.006.

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20

Hoeft, Matthias, Kamlesh Rajpurohit, Denis Wittor, Gabriella di Gennaro, and Paola Domínguez-Fernández. "On the Polarisation of Radio Relics." Galaxies 10, no. 1 (2022): 10. http://dx.doi.org/10.3390/galaxies10010010.

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Radio relics are extended radio emission features which trace shock waves in the periphery of galaxy clusters originating from cluster mergers. Some radio relics show a highly polarised emission, which make relics an excellent probe for the magnetisation of the intra-cluster medium. The origin of the relic polarisation is still debated. It could be a result of tangentially stretching the magnetic field at the shock surface. This scenario would naturally explain the alignment of the polarisation (E-vectors) with the shock normal. We have implemented a toy model for the relic polarisation accord

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21

Dacunha, Tara, Sergio Martin-Alvarez, Susan E. Clark, and Enrique Lopez-Rodriguez. "The Fallibility of Equipartition Magnetic Field Strengths from Synchrotron Emission Using Synthetically Observed Galaxies." Astrophysical Journal 980, no. 2 (2025): 197. https://doi.org/10.3847/1538-4357/adab72.

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Abstract Understanding the role that magnetic fields play on the stage of galaxy formation requires accurate methods for inferring the properties of extragalactic magnetic fields. Radio synchrotron emission has been the most promising avenue to infer magnetic field strengths across galaxies, with the application of a central assumption: that galactic cosmic rays are in energy equipartition with the magnetic field. In this work, we leverage flexible synthetic observations of a high-resolution magnetohydrodynamic simulation of a Milky Way–like galaxy to review whether true equipartition is capab

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22

Wasserman, I., J. M. Cordes, S. Chatterjee, and G. Batra. "Nonaxisymmetric Precession of Magnetars and Fast Radio Bursts." Astrophysical Journal 928, no. 1 (2022): 53. http://dx.doi.org/10.3847/1538-4357/ac38a6.

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Abstract The repeating fast radio bursts (FRBs) 180916.J0158 and 121102 are visible during periodically occurring windows in time. We consider the constraints on internal magnetic fields and geometries if the cyclical behavior observed for FRB 180916.J0158 and FRB 121102 is due to the precession of magnetars. In order to frustrate vortex line pinning we argue that internal magnetic fields must be stronger than about 1016 G, which is large enough to prevent superconductivity in the core and destroy the crustal lattice structure. We conjecture that the magnetic field inside precessing magnetars

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23

Ikegami, F., T. Takeuchi, and S. Yoshida. "Theoretical prediction of mean field strength for urban mobile radio." IEEE Transactions on Antennas and Propagation 39, no. 3 (1991): 299–302. http://dx.doi.org/10.1109/8.76325.

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24

Franssen, W. M. J., Y. L. A. Rezus, and A. P. M. Kentgens. "High radio-frequency field strength nutation NMR of quadrupolar nuclei." Journal of Magnetic Resonance 273 (December 2016): 33–39. http://dx.doi.org/10.1016/j.jmr.2016.09.018.

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25

Tsedilina, Elena E. "HF radio wave field strength on long mid-latitude paths." Radio Science 27, no. 6 (1992): 981–90. http://dx.doi.org/10.1029/92rs00928.

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26

Beck, Rainer. "Magnetism in galaxies – Observational overview and next generation radio telescopes." Proceedings of the International Astronomical Union 6, S274 (2010): 325–32. http://dx.doi.org/10.1017/s1743921311007228.

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AbstractThe strength and structure of cosmic magnetic fields is best studied by observations of radio continuum emission, its polarization and its Faraday rotation. Fields with a well-ordered spiral structure exist in many types of galaxies. Total field strengths in spiral arms and bars are 20–30 μG and dynamically important. Strong fields in central regions can drive gas inflows towards an active nucleus. The strongest regular fields (10–15 μG) are found in interarm regions, sometimes forming “magnetic spiral arms” between the optical arms. The typical degree of polarization is a few % in spi

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27

Krause, Marita. "Interplay of CR-driven galactic wind, magnetic field, and galactic dynamo in spiral galaxies." Proceedings of the International Astronomical Union 4, S259 (2008): 547–48. http://dx.doi.org/10.1017/s1743921309031263.

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AbstractFrom our radio observations of the magnetic field strength and large-scale pattern of spiral galaxies of different Hubble types and star formation rates (SFR) we conclude that – though a high SFR in the disk increases the total magnetic field strength in the disk and the halo – the SFR does not change the global field configuration nor influence the global scale heights of the radio emission. The similar scale heights indicate that the total magnetic field regulates the galactic wind velocities. The galactic wind itself may be essential for an effective dynamo action.

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28

Wiltschko, Roswitha, Peter Thalau, Dennis Gehring, Christine Nießner, Thorsten Ritz, and Wolfgang Wiltschko. "Magnetoreception in birds: the effect of radio-frequency fields." Journal of The Royal Society Interface 12, no. 103 (2015): 20141103. http://dx.doi.org/10.1098/rsif.2014.1103.

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The avian magnetic compass, probably based on radical pair processes, works only in a narrow functional window around the local field strength, with cryptochrome 1a as most likely receptor molecule. Radio-frequency fields in the MHz range have been shown to disrupt the birds' orientation, yet the nature of this interference is still unclear. In an immuno-histological study, we tested whether the radio-frequency fields interfere with the photoreduction of cryptochrome, but this does not seem to be the case. In behavioural studies, birds were not able to adjust to radio-frequency fields like the

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29

Costa, M. E., P. M. McCulloch, and P. A. Hamilton. "The magnetic field strength in the Large Magellanic Cloud." Symposium - International Astronomical Union 148 (1991): 101–2. http://dx.doi.org/10.1017/s0074180900200107.

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We have measured a value of 4±5m--2rad for the rotation measure of the radio pulsar PSR0529-66 in the LMC and, after allowing for the dispersion and rotation measures of our Galaxy on the pulsar's line of sight, we deduce that the magnetic field strength in the LMC is in the range 0 to 5μGauss oriented away from the Sun.

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Yamasaki, Shotaro, Kazım Yavuz Ekşi, and Ersin Göğüş. "Angular dependence of coherent radio emission from magnetars with multipolar magnetic fields." Monthly Notices of the Royal Astronomical Society 512, no. 3 (2022): 3189–94. http://dx.doi.org/10.1093/mnras/stac699.

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ABSTRACT The recent detection of a fast radio burst (FRB) from a Galactic magnetar secured the fact that neutron stars (NSs) with superstrong magnetic fields are capable of producing these extremely bright coherent radio bursts. One of the leading mechanisms to explain the origin of such coherent radio emission is the curvature radiation process within the dipolar magnetic field structure. It has, however, already been demonstrated that magnetars likely have a more complex magnetic field topology. Here, we critically investigate curvature radio emission in the presence of inclined dipolar and

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31

Beuermann, K., and Y. G. Kim. "Correlation Between Galactic Non-Thermal Continuum Emission and HI-Column Density." Symposium - International Astronomical Union 140 (1990): 59–60. http://dx.doi.org/10.1017/s0074180900189533.

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The distribution of magnetic field strengths in the interstellar gas is an important datum which relates to the formation of dense cloud complexes as well as to the distribution and propagation of cosmic rays. Brown and Chang (1983) found the brightness temperature of the radio continuum emission to be correlated with the HI column density NH and deduced a field strength which increases with particle density as <H> ~ <n>0.44. Troland and Heiles (1986) critized their approach and pointed out that Zeeman measurements suggest no increase in field strength for particle densities n ≤ 10

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Weratschnig, J., S. Schindler, and M. Gitti. "XMM Observation of the Galaxy Cluster Abell 514." Proceedings of the International Astronomical Union 2, S235 (2006): 256. http://dx.doi.org/10.1017/s1743921306006521.

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AbstractWe present XMM-Newton observations of the galaxy cluster Abell 514. This cluster shows a very complex X-ray morphology. Radio observations show that there are six radio sources located inside the cluster. This makes it possible to determine the magnetic field strength using the Faraday rotation method. This cluster is an example for the hierarchical growth of structure and a very interesting object for studying the correlation between magnetic field strength and X-ray properties.

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Wang, S. Q., J. B. Wang, D. Z. Li, et al. "Change of Rotation Measure during the Eclipse of a Black Widow PSR J2051−0827." Astrophysical Journal 955, no. 1 (2023): 36. http://dx.doi.org/10.3847/1538-4357/acea81.

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Abstract Black widows are millisecond pulsars ablating their companions. The material blown from the companion blocks the radio emission, resulting in radio eclipses. The properties of the eclipse medium are poorly understood. Here, we present direct evidence of the existence of magnetic fields in the eclipse medium of the black widow PSR J2051−0827 using observations made with the Five-hundred-meter Aperture Spherical radio Telescope. We detect a regular decrease in rotation measure (RM) in the egress of the eclipse, changing from 60 to −28.7 rad m−2. The RM gradually changes back to normal w

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Beck, R., U. R. Buczilowski, and J. I. Harnett. "Polarized Radio Emission from NGC 6946." Symposium - International Astronomical Union 140 (1990): 213–14. http://dx.doi.org/10.1017/s0074180900190011.

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New VLA radio observations of NGC 6946 reveal a complicated structure of the magnetic field with possibly radial changes in the foreground Faraday rotation, the strength of the uniform field and the particular dynamo mode in operation. The uniform field is strongest in the interarm regions, but shows no deducible large-scale structure in the radius range of the optical spiral arms. The high star formation rate in NGC 6946 apparently increases the turbulence of the interstellar magnetic field.

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Carley, Eoin P., Nicole Vilmer, Paulo J. A. Simões, and Brían Ó Fearraigh. "Estimation of a coronal mass ejection magnetic field strength using radio observations of gyrosynchrotron radiation." Astronomy & Astrophysics 608 (December 2017): A137. http://dx.doi.org/10.1051/0004-6361/201731368.

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Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the low solar corona into interplanetary space. These eruptions are often associated with the acceleration of energetic electrons which produce various sources of high intensity plasma emission. In relatively rare cases, the energetic electrons may also produce gyrosynchrotron emission from within the CME itself, allowing for a diagnostic of the CME magnetic field strength. Such a magnetic field diagnostic is important for evaluating the total magnetic energy content of the CME, which is ultimately what drives

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Han, J. L. "Magnetic Fields in our Galaxy: How much do we Know? I. Disk fields within a few kpc of the Sun." International Astronomical Union Colloquium 182 (2001): 181–84. http://dx.doi.org/10.1017/s0252921100000932.

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AbstractThe large scale magnetic fields of our Galaxy have been mostly revealed by rotation measures (RMs) of pulsars and extragalactic radio sources. In the disk of our Galaxy, the average field strength over a few kpc scale is about 1.8 μG, while the total field, including the random fields on smaller scales, has a strength of about 5 μG. The local regular field, if it is part of the large scale field of a bisymmetric form, has a pitch angle of about −8°. There are at least three, and perhaps five, field reversals from the Norma arm to the outer skirt of our Galaxy.

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Livingston, J. D., N. M. McClure-Griffiths, S. A. Mao, et al. "A radio polarization study of magnetic fields in the Small Magellanic Cloud." Monthly Notices of the Royal Astronomical Society 510, no. 1 (2021): 260–75. http://dx.doi.org/10.1093/mnras/stab3375.

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ABSTRACT Observing the magnetic fields of low-mass interacting galaxies tells us how they have evolved over cosmic time and their importance in galaxy evolution. We have measured the Faraday rotation of 80 extra-galactic radio sources behind the Small Magellanic Cloud (SMC) using the CSIRO Australia Telescope Compact Array (ATCA) with a frequency range of 1.4–3.0 GHz. Both the sensitivity of our observations and the source density are an order-of-magnitude improvement on previous Faraday rotation measurements of this galaxy. The SMC generally produces negative rotation measures after accountin

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38

Young, M. D., R. N. Manchester, and S. Johnston. "Ha, ha, ha, ha, staying alive, staying alive: A radio pulsar with an 8.5-s period challenges emission models." International Astronomical Union Colloquium 177 (2000): 185–88. http://dx.doi.org/10.1017/s025292110005942x.

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AbstractWe report the discovery of the longest known radio pulsar period. PSR J2144–3933, previously thought to have a period of 2.84 s, actually has a period of 8.51 s. Under the usual assumptions about the stellar equation of state, this pulsar has an average surface dipolar magnetic field strength of ~ 2.0 × 1012G. According to popular theories of the emission mechanism this pulsar should not be emitting radio waves because its long period and magnetic field strength make pair creation impossible for all reasonable magnetic field configurations. Either assumptions about the equation of stat

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39

Ristic, Miroslav, Radomir Rankovic, Mirjana Vojnovic, Violeta Stankovic, and Goran Poparic. "Dissociation of N2 by electron impact in electric and magnetic RF fields." Journal of the Serbian Chemical Society, no. 00 (2022): 66. http://dx.doi.org/10.2298/jsc220710066r.

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Rate coefficients for electron impact dissociation of the N2 molecule under the influence of crossed radio-frequency (RF) electric and magnetic fields are calculated for field frequencies of 13.56, 100 and 200 MHz and for root mean square values of the reduced electric field strength of 300 and 500 Td. Root mean square values of the reduced magnetic field were varied from 0 to 2000 Hx. ?he effects of the strength of RF fields and their frequency on rates for the dissociation to neutral fragments and for the dissociative ionization are discussed. The temporal evolution of the rate coefficients

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40

Wexler, David B., Elizabeth A. Jensen, and Carl Heiles. "Middle Corona Magnetic Field Strength Determined by Spacecraft Radio Faraday Rotation." Research Notes of the AAS 5, no. 7 (2021): 165. http://dx.doi.org/10.3847/2515-5172/ac1521.

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41

Almeida, M. P. C., L. da Silva Mello, J. A. C. Braz, et al. "Measurements of Field Strength and HD Radio Reception Quality at VHF." IEEE Antennas and Wireless Propagation Letters 14 (2015): 201–4. http://dx.doi.org/10.1109/lawp.2014.2359001.

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O. O., Oladapo, Oni E. A., Aremu A. A., et al. "Assessment of Radio Frequency Electromagnetic Field Exposure from Wi-Fi Routers in LAUTECH Campus, Ogbomoso, Nigeria." Asian Journal of Current Research 9, no. 4 (2024): 51–59. http://dx.doi.org/10.56557/ajocr/2024/v9i48871.

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Wi-Fi routers play a crucial role in enabling internet connectivity within the academic environment. However, there are concerns that radiofrequency electromagnetic field exposure from Wi-Fi routers may be hazardous to human health. The main objective of the research is to assess the safety of RF-EMF exposure in educational environments. A total of 14 Wi-Fi routers were randomly selected and investigated across LAUTECH campus using stratified random sampling method. Measurement of the power density and the electric field strength from these routers were taken using a hand-held electrosmog, TES

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Pivovaroff, M. J., V. M. Kaspi, and F. Camilo. "X-ray observations of the high magnetic field radio pulsar PSR J1814–1744." International Astronomical Union Colloquium 177 (2000): 349–50. http://dx.doi.org/10.1017/s0252921100059959.

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AbstractWe present X-ray observations of PSR J1814–1744, a 4 s radio pulsar with inferred surface dipole magnetic field strength 5.5 × 1013G recently discovered in the on-going Parkes multibeam survey. This pulsar’s spin parameters are very similar to those of anomalous X-ray pulsars (AXPs). X-ray emission is not detected from the position of the radio pulsar in observations withROSATandASCA. The derived upper flux limit implies an X-ray luminosity significantly smaller than those of all known AXPs. These results argue that magnetar mechanism invoked to explain X-ray emission from AXPs must de

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Orlando, S., M. Miceli, O. Petruk, et al. "3D MHD modeling of the expanding remnant of SN 1987A." Astronomy & Astrophysics 622 (January 29, 2019): A73. http://dx.doi.org/10.1051/0004-6361/201834487.

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Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field in the dynamics of the expanding remnant of SN 1987A, and the origin and evolution of the radio emission from the remnant, in particular during the interaction of the blast wave with the nebula surrounding the SN. Methods. We modeled the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula using three-dimensional magnetohydrodynamic simulations. The model considers the radiative cooling, the deviations from equilibrium of

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Shinnaga, Hiroko, Mark J. Claussen, Satoshi Yamamoto, and Shimojo Masumi. "Strong magnetic field of the peculiar red supergiant VY Canis Majoris." Proceedings of the International Astronomical Union 13, S336 (2017): 391–92. http://dx.doi.org/10.1017/s1743921317010948.

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AbstractWe report on magnetic field measurements associated with the well-known extreme red supergiant (RSG), VY Canis Majoris (VY CMa). We measured both linear and circular polarization of the SiO v = 0, J = 1 − 0 transition using a sensitive radio interferometer. The measured magnetic field strengths are surprisingly high. A lower limit for the field strength is expected to be at least ~ 10 Gauss based on the high degree of linear polarization. Since the field strengths are very high, the magnetic field must be a key element in understanding the stellar evolution of VY CMa as well as the dyn

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Андрущак, І., В. Кошелюк, О. Сіваковська, М. Потейчук, and В. Марценюк. "Features of information technology distribution of radio waves by frequency bands." КОМП’ЮТЕРНО-ІНТЕГРОВАНІ ТЕХНОЛОГІЇ: ОСВІТА, НАУКА, ВИРОБНИЦТВО, no. 36 (November 20, 2019): 5–10. http://dx.doi.org/10.36910/6775-2524-0560-2019-36-1.

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The article justifies the propagation of radio waves. The basics of their distribution in an inhomogeneous atmosphere are outlined. The principles of field strength reduction and classification of the main radio path models, both open and in the case of interference of various types, including those that screen the field, are presented. Attention is paid to modern models of attenuation of radio waves in the conditions of dense construction in metropolitan areas, as well as indoors and buildings.

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Miroshnichenko, Alla. "Independent estimates of energies of steep-spectrum radio sources." Proceedings of the International Astronomical Union 9, S304 (2013): 96–99. http://dx.doi.org/10.1017/s1743921314003445.

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AbstractWe examine properties of galaxies and quasars with steep low-frequency spectra from the UTR-2 catalogue. The number of the objects have the non-thermal X-ray emission due to the inverse Compton scattering of radio photons of the microwave background by relativistic electrons. So, it is possible to estimate the magnetic field strength and the ratio of energies of the magnetic field and relativistic particles, independently. As we have received the determined values of magnetic field strength are near to one order less than those at the well-known energy equipartition condition. We concl

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Adebahr, B., M. Brienza, and R. Morganti. "Polarised structures in the radio lobes of B2 0258+35." Astronomy & Astrophysics 622 (February 2019): A209. http://dx.doi.org/10.1051/0004-6361/201833988.

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Context. The contribution of active galactic nuclei to the magnetisation of the Universe can be constrained by knowing their duty cycles, jet and magnetic field morphologies, and the physical processes dominating their interaction with the surrounding environment. Aims. The magnetic field morphology and strength of radio lobes of AGN has an influence on the mechanisms for the propagation of cosmic rays into intergalactic space. Using the source B2 0258+35 we want to investigate the interaction of its radio lobes with the surrounding environment and examine the underlying physical effects. Meth

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Hu, Jinlian, Huaqiang Li, Rong Song, et al. "Continuously tunable radio frequency electrometry with Rydberg atoms." Applied Physics Letters 121, no. 1 (2022): 014002. http://dx.doi.org/10.1063/5.0086357.

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We demonstrate a continuously tunable electric field measurement based on the far off-resonant AC stark effect in a Rydberg atomic vapor cell. In this configuration, a strong far off-resonant field, denoted as a local oscillator (LO) field, acts as a gain to shift the Rydberg level to a high sensitivity region. An incident weak signal field with a few hundreds of kHz difference from the LO field is mixed with the LO field in the Rydberg system to generate an intermediate frequency signal, which is read out by Rydberg electromagnetically induced transparency (Rydberg-EIT) spectroscopy. Not like

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Michail, Joseph M., Farhad Yusef-Zadeh, and Mark Wardle. "Detection of a 20-min time lag observed from Sgr A* between 8 and 10 GHz with the VLA." Monthly Notices of the Royal Astronomical Society 505, no. 3 (2021): 3616–23. http://dx.doi.org/10.1093/mnras/stab1529.

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ABSTRACT We report the detection and analysis of a radio flare observed on 17 April 2014 from Sgr A* at 9 GHz using the VLA in its A-array configuration. This is the first reported simultaneous radio observation of Sgr A* across 16 frequency windows between 8 and 10 GHz. We cross-correlate the lowest and highest spectral windows centred at 8.0 and 9.9 GHz, respectively, and find the 8.0 GHz light-curve lagging $18.37^{+2.17}_{-2.18}$ min behind the 9.9 GHz light curve. This is the first time lag found in Sgr A*’s light curve across a narrow radio frequency bandwidth. We separate the quiescent

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