An Observation of the Longitudinal Magnetic Field in a Sunspot Group.

1964 ◽  
Vol 139 ◽  
pp. 1336 ◽  
Author(s):  
Richard G. Teske ◽  
Helen W. Dodson ◽  
E. Ruth Hedeman
Keyword(s):  
Magnetic Field ◽  
Sunspot Group ◽  
Longitudinal Magnetic Field

scholarly journals The Formation of a Moat Around a Sunspot as Observed on Longitudinal–Field Magnetograms (?)

1993 ◽  
Vol 141 ◽  
pp. 75-77
Author(s):  
L.V. Ermakova
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Spatial Resolution ◽  
Sunspot Group ◽  
Longitudinal Magnetic Field ◽  
Photospheric Magnetic Field ◽  
Longitudinal Field ◽  
Maximum Area ◽  
Spot Group

In this paper the dynamics of the photospheric magnetic field near the sunspot of the active region McMath 15508 is considered on the basis of longitudinal magnetic field B11 magnetograms. The magnetograms were obtained at the panoramic magnetograph of the Sayan Observatory. The time taken to obtain one magnetogram was 5 min. The spatial resolution was 1.8“ × 3.6“. In the active region McMath 15508 a new bipolar spot group formed westward of the existing sunspot group on September 1; the next day the main sunspots had penumbras, and on September 3 the new sunspot group reached a maximum area and began decaying thereafter.

scholarly journals Small Scale Magnetic Structures in Active Centers

1990 ◽  
Vol 138 ◽  
pp. 157-160
Author(s):  
A. Dollfus
Keyword(s):  
Magnetic Field ◽  
Sunspot Group ◽  
Longitudinal Magnetic Field ◽  
Driving Forces ◽  
Doppler Velocity ◽  
Small Scale ◽  
Active Centers ◽  
Magnetic Structures ◽  
Small Elements

Active sunspot group n° 4567 was observed with high angular magnification on Sept. 2, 1984, using the instrument FPSS at Meudon Observatory. Within the sunspots umbrae, the longitudinal magnetic field shows a collection of small elements down to the limit of resolution of around 600 km. Between the trailing and leading spots, there were very sharp gradients, both in magnetization (450 gauss over 1000 km) and in Doppler velocity (350 m s-1 over 1 000 km). The line defined by these gradients was the location of a flare. Evershed driving forces may be responsible for building up these gradients and flare.

Refinement of metal structure in arc surfacing under the effect of longitudinal magnetic field

2019 ◽  
Vol 2019 (2) ◽  
pp. 19-21
Author(s):  
A.D. Razmyshlyaev ◽  
◽  
M.V. Ageeva ◽  
E.V. Lavrova ◽  
◽  
...  
Keyword(s):  
Magnetic Field ◽  
Longitudinal Magnetic Field ◽  
Metal Structure

scholarly journals Design and evaluation of 10-kA class superconducting DC power cable based on longitudinal magnetic field effect

2021 ◽  
Vol 1975 (1) ◽  
pp. 012037
Author(s):  
Y Kinoshita ◽  
T Yonenaka ◽  
Y Ichiki ◽  
T Akasaka ◽  
E S Otabe ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Effect ◽  
Longitudinal Magnetic Field ◽  
Magnetic Field Effect ◽  
Power Cable ◽  
Dc Power

scholarly journals Magnetic field of the classical Cepheid η Aql: new results

2013 ◽  
Vol 9 (S302) ◽  
pp. 381-382
Author(s):  
V. Butkovskaya ◽  
S. Plachinda ◽  
D. Baklanova ◽  
V. Butkovskyi
Keyword(s):  
Magnetic Field ◽  
Longitudinal Magnetic Field ◽  
Mean Value ◽  
Stellar Rotation ◽  
Classical Cepheid ◽  
Pulsation Cycle

AbstractWe present the results of the spectropolarimetric study of the classical Cepheid η Aql in 2002, 2004, 2010, and 2012. The longitudinal magnetic field of η Aql was found to be variable with the pulsation cycle of 7.176726 day. The amplitude, phase, and mean value of the field vary from year to year presumably due to stellar rotation or dynamo mechanisms.

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