Efficiency for electron acceleration in solar energy release region as estimated in the context of plasma mechanism of radio emission

1994 ◽  
Vol 90 ◽  
pp. 713 ◽  
Author(s):  
B. N. Levin ◽  
V. M. Fridman ◽  
O. A. Sheiner
Keyword(s):  
Solar Energy ◽  
Radio Emission ◽  
Energy Release ◽  
Electron Acceleration ◽  
Energy Release Region

Possible two-step solar energy release mechanism due to turbulent magnetic reconnection

2005 ◽  
Vol 12 (5) ◽  
pp. 052901 ◽  
Author(s):  
Quan-Lin Fan ◽  
Xue-Shang Feng ◽  
Chang-Qing Xiang
Keyword(s):  
Solar Energy ◽  
Magnetic Reconnection ◽  
Energy Release ◽  
Release Mechanism

scholarly journals VLBI for probing large-scale magnetic structures of stars

1996 ◽  
Vol 176 ◽  
pp. 173-180
Author(s):  
J.-F. Lestrade
Keyword(s):  
Magnetic Fields ◽  
Radio Emission ◽  
Large Scale ◽  
Electron Acceleration ◽  
High Gravity ◽  
Magnetic Structures

By VLBI astrometry, we show that the two RSCVn type binaries, UX Ari and σ2 CrB, have a preferred site of radio emission which is the intra-system region. It is known that radio emission from these stars is from the gyro-synchrotron process associated with large-scale magnetic fields. High gravity in the intra-system region might favor dense magnetic loops. Interactions in this region between loops attached to the surfaces of the two stellar components might produce reconnections required for electron acceleration.

Radio emission of solar flare of February 12, 2010, and electron acceleration modes

2015 ◽  
Vol 55 (3) ◽  
pp. 295-298 ◽  
Author(s):  
R. V. Gorgutsa ◽  
V. A. Kovalev ◽  
I. G. Kostuchenko ◽  
A. K. Markeev ◽  
D. E. Sobolev ◽  
...  
Keyword(s):  
Solar Flare ◽  
Radio Emission ◽  
Electron Acceleration

Effect of shock ripples on electron acceleration and reflection at the quasi-perpendicular bow shock

2020 ◽  
Author(s):  
Daniel Graham ◽  
Yuri Khotyaintsev ◽  
Andris Vaivads ◽  
Mats Andre ◽  
Ahmad Lalti ◽  
...  
Keyword(s):  
Radio Emission ◽  
Test Particle ◽  
Plasma Frequency ◽  
Electron Beams ◽  
Electron Acceleration ◽  
Bow Shock ◽  
Magnetospheric Multiscale ◽  
Particle Simulations ◽  
Normal Angle ◽  
Beam Mode

<p>At Earth’s bow shock electrons can be reflected and accelerated along magnetic fields lines, which can then form electron beams and excite Langmuir and beam-mode waves. These electron beams form when the shock normal angle is close to 90 degrees. However, recent observations have shown that quasi-perpendicular shocks can be non-stationary and exhibit ripples, which can modify the local shock-normal angle and cross-shock potential. We use Magnetospheric Multiscale (MMS) data to investigate the effects of shock ripples on the accelerated electrons observed in the electron foreshock. We compare the results with test-particle simulations to determine the effect of shock ripples on electron acceleration. We discuss the implications of these results for the generation of plasma frequency waves and radio emission in the electron foreshock region.<span> </span></p>

scholarly journals Sources of type III solar microwave bursts

2016 ◽  
Vol 2 (2) ◽  
pp. 15-27 ◽  
Author(s):  
Дмитрий Жданов ◽  
Dmitriy Zhdanov ◽  
Сергей Лесовой ◽  
Sergey Lesovoi ◽  
Сусанна Тохчукова ◽  
...  
Keyword(s):  
Energy Release ◽  
Complex Analysis ◽  
Primary Energy ◽  
Original Method ◽  
Burst Source ◽  
Energy Release Region ◽  
Siberian Solar Radio Telescope ◽  
Solar Microwave ◽  
Fine Structures ◽  
Microwave Bursts

Microwave fine structures allow us to study plasma evolution in an energy release region. The Siberian Solar Radio Telescope (SSRT) is a unique instrument designed to examine fine structures at 5.7 GHz. A complex analysis of data from RATAN-600, 4–8 GHz spectropolarimeter, and SSRT, simultaneously with EUV data, made it possible to localize sources of III type microwave bursts in August 10, 2011 event within the entire frequency band of burst occurrence, as well as to determine the most probable region of primary energy release. To localize sources of III type bursts from RATAN-600 data, an original method for data processing has been worked out. At 5.7 GHz, the source of bursts was determined along two coordinates, whereas at 4.5, 4.7, 4.9, 5.1, 5.3, 5.5, and 6.0 GHz, their locations were identified along one coordinate. The size of the burst source at 5.1 GHz was found to be maximum as compared to those at other frequencies.

Incorporating Inner Magnetosphere Current-driven Electron Acceleration in Numerical Simulations of Exoplanet Radio Emission

2021 ◽  
Vol 914 (1) ◽  
pp. 60
Author(s):  
Anthony Sciola ◽  
Frank Toffoletto ◽  
David Alexander ◽  
Kareem Sorathia ◽  
Viacheslav Merkin ◽  
...  
Keyword(s):  
Radio Emission ◽  
Numerical Simulations ◽  
Electron Acceleration ◽  
Inner Magnetosphere

scholarly journals Radio emission from accreting isolated black holes in our galaxy

2019 ◽  
Vol 488 (2) ◽  
pp. 2099-2107 ◽  
Author(s):  
Daichi Tsuna ◽  
Norita Kawanaka
Keyword(s):  
Black Holes ◽  
Radio Emission ◽  
Interstellar Medium ◽  
Binary Systems ◽  
Electron Acceleration ◽  
Stellar Mass ◽  
Synchrotron Emission ◽  
Accelerated Electrons ◽  
Accretion Flow

ABSTRACT Apart from the few tens of stellar-mass black holes discovered in binary systems, an order of 108 isolated black holes (IBHs) are believed to be lurking in our Galaxy. Although some IBHs are able to accrete matter from the interstellar medium, the accretion flow is usually weak and thus radiatively inefficient, which results in significant material outflow. We study electron acceleration generated by the shock formed between this outflow and the surrounding material, and the subsequent radio synchrotron emission from accelerated electrons. By numerically calculating orbits of IBHs to obtain their spatial and velocity distributions, we estimate the number of IBHs detectable by surveys using SKA1-mid (SKA2) as ∼30 (∼700) for the most optimistic case. The SKA’s parallax measurements may accurately give their distances, possibly shedding light on the properties of the black holes in our Galaxy.

scholarly journals Efficiency for Electron Acceleration in Solar Energy Release Region as Estimated in the Context of Plasma Mechanism of Radio Emission

1994 ◽  
Vol 142 ◽  
pp. 713-717
Author(s):  
B. N. Levin ◽  
V. M. Fridman ◽  
O. A. Sheiner
Keyword(s):  
Magnetic Trap ◽  
Inhomogeneous Plasma ◽  
Spectral Characteristics ◽  
Electron Acceleration ◽  
Plasma Radiation ◽  
Frequency Range ◽  
Superthermal Electrons ◽  
Radiation Mechanisms ◽  
Energy Release Region ◽  
Gyrosynchrotron Emission

AbstractThe paper is devoted to the interpretation of spectrographic data within the frequency range 8-12 GHz. Some spectral characteristics of weak solar steplike radio bursts are reported. To explain some parameters of the emission the ability to keep superthermal electrons in a magnetic trap with dense inhomogeneous plasma is theoretically studied. On the basis of this model we estimate the energy and number of accelerated electrons, and the flux density of precipitating electrons which are the source of enhanced plasma radiation. For the obtained efficiency of electron acceleration the calculated intensity of gyrosynchrotron emission proves to be less than the observed one.Subject headings: acceleration of particles — radiation mechanisms: nonthermal — Sun: flares — Sun: radio radiation

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