scholarly journals Probing the innermost regions of AGN jets and their magnetic fields with RadioAstron. IV. The quasar 3C 345 at 18 cm: Magnetic field structure and brightness temperature

2021 ◽  
Author(s):  
F. M. Pötzl ◽  
A. P. Lobanov ◽  
E. Ros ◽  
J. L. Gómez ◽  
G. Bruni ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Brightness Temperature ◽  
Field Structure ◽  
Magnetic Field Structure

scholarly journals Magnetic Fields in Quasar 3C147 on Milliarcsecond Scales

2001 ◽  
Vol 182 ◽  
pp. 143-146
Author(s):  
H.Y. Zhang ◽  
R.D. Nan
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Structure ◽  
Magnetic Field Structure ◽  
Intrinsic Magnetic Field ◽  
Rotation Measure ◽  
Bright Feature ◽  
5 Ghz ◽  
Arch Shape

AbstractVLBA polarimetric observations of the steep-spectrum quasar 3C147 were made at four frequencies in the available 5 GHz band, from which polarization in one bright feature in the inner jet was detected. The rotation measure of this feature (~ 1300 rad m−2) agrees with the known high rotation measure of the source, which makes it possible to remove the Faraday screen pixel-by-pixel and obtain the intrinsic magnetic field structure. The arch shape of B vectors suggests that a relativistic and distorted jet is being seen in projection.

scholarly journals Evolution of a Filament/CH/Magnetic Field Complex

1998 ◽  
Vol 167 ◽  
pp. 393-396
Author(s):  
B.A. Ioshpa ◽  
E.I. Mogilevsky ◽  
V.N. Obridko
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Magnetic Fields ◽  
Large Scale ◽  
Coronal Holes ◽  
Field Structure ◽  
Potential Approximation ◽  
Magnetic Field Structure ◽  
Single Complex ◽  
The Magnetic Field

AbstractSOHO and YOHKOH images, as well as Hα filtergrams and magnetograms from IZMIRAN have been used to analyze the evolution of the related solar phenomena – filament, active region, and accompanying pair of coronal holes – during six solar rotations, with an emphasis on the events observed during August–September, 1996. The whole complex has been considered against the large–scale magnetic fields calculated under the potential approximation. A peculiar point has been found along the changing filament. It is shown that the phenomena under investigation (filament, active region, and coronal hole) form a single complex connected with the magnetic field structure.

scholarly journals Magnetic fields in massive star forming regions: wide-field NIR polarimetry of M42 and Mon R2

2008 ◽  
Vol 4 (S259) ◽  
pp. 97-98 ◽  
Author(s):  
Nobuhiko Kusakabe ◽  
Motohide Tamura ◽  
Ryo Kandori ◽  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Massive Star ◽  
Near Infrared ◽  
Polarized Light ◽  
Field Structure ◽  
Wide Field ◽  
Magnetic Field Structure ◽  
Star Forming ◽  
Star Forming Regions

AbstractMagnetic fields are believed to play an important role in star formation. We observed M42 and Mon R2 massive star forming regions using the wide-field (8′ × 8′) near-infrared imaging polarimeter SIRPOL in South Africa. Magnetic fields are mapped on the basis of dichroic polarized light from hundreds of young stars embedded in the regions. We found “hourglass shaped” magnetic field structure toward OMC-1 region, which is very consistent with magnetic fields traced by using dust emission polarimetry at sub-mm to FIR wavelengths. In the Mon R2 region, we found “S-shaped” magnetic field structure across the massive protostar IRS 1 and IRS 2. We will present the results of comparison of magnetic fields at NIR with those at other wavelengths.

scholarly journals Distortion of Magnetic Fields in a Starless Core II: 3D Magnetic Field Structure of FeSt 1-457

2017 ◽  
Vol 848 (2) ◽  
pp. 110 ◽  
Author(s):  
Ryo Kandori ◽  
Motohide Tamura ◽  
Kohji Tomisaka ◽  
Yasushi Nakajima ◽  
Nobuhiko Kusakabe ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Field Structure ◽  
Magnetic Field Structure

scholarly journals The Intrinsic Magnetic Field Orientation in NGC 4631: Dynamo or Outflow ?

1993 ◽  
Vol 157 ◽  
pp. 299-303
Author(s):  
Götz Golla ◽  
Edsko Hummel
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Central Region ◽  
Field Structure ◽  
Field Orientation ◽  
Magnetic Field Structure ◽  
Magnetic Field Orientation ◽  
Radio Halo ◽  
Intrinsic Magnetic Field ◽  
Field Lines

The interacting galaxy NGC4631 is unique among edge-on galaxies in that it shows a prominent synchrotron radio halo. We derive the intrinsic magnetic field structure in this halo. The field lines are mainly radially outgoing from the central region. The possible mechanisms generating such magnetic fields in the halo, i.e. outflows and dynamo processes, are discussed.

scholarly journals The Magnetic Be Star Sigma Orionis E

1987 ◽  
Vol 92 ◽  
pp. 82-83 ◽  
Author(s):  
C. T. Bolton ◽  
A. W. Fullerton ◽  
D. Bohlender ◽  
J. D. Landstreet ◽  
D. R. Gies
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
High Signal ◽  
Rotational Period ◽  
Magnetic Field Structure ◽  
The Past ◽  
Distribution Of Elements ◽  
Be Star ◽  
Hα Emission ◽  
The Magnetic Field

Over the past two years, we have obtained high resolution high signal/noise (S/N) spectra of the magnetic Be star σ Ori E at the Canada-France-Hawaii Telescope and McDonald Observatory. These spectra, which cover the spectral regions 399-417.5 and 440-458.5 nm and the Hα line and have typical S/N>200 and spectral resolution ≃0.02 nm, were obtained at a variety of rotational phases in order to study the magnetic field structure, the distribution of elements in the photosphere, and the effects of the magnetic field on the emission envelope. Our analysis of these spectra confirms, refines and extends the results obtained by Landstreet & Borra (1978), Groote & Hunger (1982 and references therein), and Nakajima (1985).The Hα emission is usually double-peaked, but it undergoes remarkable variations with the 1.19081 d rotational period of the star, which show that the emitting gas is localized into two regions which co-rotate with the star.

scholarly journals Propagation of an MHD Shock in the Vicinity of a Magnetic Neutral Sheet

1980 ◽  
Vol 91 ◽  
pp. 323-326
Author(s):  
D. J. Mullan ◽  
R. S. Steinolfson
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Solar Corona ◽  
Large Scale ◽  
Field Structure ◽  
Neutral Sheet ◽  
Solar Cosmic Rays ◽  
Magnetic Field Structure ◽  
Large Scale Magnetic Field ◽  
Highly Correlated

The acceleration of solar cosmic rays in association with certain solar flares is known to be highly correlated with the propagation of an MHD shock through the solar corona (Svestka, 1976). The spatial structure of the sources of solar cosmic rays will be determined by those regions of the corona which are accessible to the flare-induced shock. The regions to which the flare shock is permitted to propagate are determined by the large scale magnetic field structure in the corona. McIntosh (1972, 1979) has demonstrated that quiescent filaments form a single continuous feature (a “baseball stitch”) around the surface of the sun. It is known that helmet streamers overlie quiescent filaments (Pneuman, 1975), and these helmet streamers contain large magnetic neutral sheets which are oriented essentially radially. Hence the magnetic field structure in the low solar corona is characterized by a large-scale radial neutral sheet which weaves around the entire sun following the “baseball stitch”. There is therefore a high probability that as a shock propagates away from a flare, it will eventually encounter this large neutral sheet.

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