53 research outputs found
Photospheric plasma motions in the magnetic field of a single sunspot umbra
The analysis of observed velocity fields in sunspots shows that the plasma motions above a sunspot umbra do not agree with the equation of continuity. We assumed that in the temperature minimum region above a sunspot umbra there is an effective diffusion of plasma across the lines of force in the region of the magnetic field. It leads to the formation of the steady flow of plasma in the temperature minimum, i.e., photosphere region. We determined the parameters in this steady flow. The calculated parameters do not contradict observational data on moving plasma in the magnetic field above a sunspot umbra
Interaction between a fast rotating sunspot and ephemeral regions as the origin of the major solar event on 2006 December 13
The major solar event on 2006 December 13 is characterized by the
approximately simultaneous occurrence of a heap of hot ejecta, a great
two-ribbon flare and an extended Earth-directed coronal mass ejection. We
examine the magnetic field and sunspot evolution in active region NOAA AR
10930, the source region of the event, while it transited the solar disk centre
from Dec. 10 to Dec. 13. We find that the obvious changes in the active region
associated with the event are the development of magnetic shear, the appearance
of ephemeral regions and fast rotation of a smaller sunspot. Around the area of
the magnetic neutral line of the active region, interaction between the fast
rotating sunspot and the ephemeral regions triggers continual brightening and
finally the major flare. It is indicative that only after the sunspot rotates
up to 200 does the major event take place. The sunspot rotates at
least 240 about its centre, the largest sunspot rotation angle which
has been reported.Comment: 4 pages, 6 figures, ApJ Letters inpres
Statistics of Flares Sweeping across Sunspots
Flare ribbons are always dynamic, and sometimes sweep across sunspots.
Examining 588 (513 M-class and 75 X-class) flare events observed by Transition
Region and Coronal Explorer (TRACE) satellite and Hinode Solar Optical
Telescope (SOT) from 1998 May to 2009 May, we choose the event displaying that
one of the flare ribbons completely sweeps across the umbra of a main sunspot
of the corresponding active region, and finally obtain 20 (7 X-class and 13
M-class) events as our sample. In each event, we define the main sunspot
completely swept across by the flare ribbon as A-sunspot, and its nearby
opposite polarity sunspots, B-sunspot. Observations show that the A-sunspot is
a following polarity sunspot in 18 events, and displays flux emergence in 13
cases. All the B-sunspots are relatively simple, exhibiting either one main
sunspot or one main sunspot and several small neighboring sunspots (pores). In
two days prior to the flare occurrence, the A-sunspot rotates in all the cases,
while the B-sunspot, in 19 events. The total rotating angle of the A-sunspot
and B-sunspot is 193 degrees on average, and the rotating directions, are the
same in 12 events. In all cases, the A-sunspot and B-sunspot manifest shear
motions with an average shearing angle of 28.5 degrees, and in 14 cases, the
shearing direction is opposite to the rotating direction of the A-sunspot. We
suggest that the emergence, the rotation and the shear motions of the A-sunspot
and B-sunspot result in the phenomenon that flare ribbons sweep across sunspots
completely.Comment: 12 pages, 3 figures, 2 tables, accepted by ApJ Letter
The Horizontal Component of Photospheric Plasma Flows During the Emergence of Active Regions on the Sun
The dynamics of horizontal plasma flows during the first hours of the
emergence of active region magnetic flux in the solar photosphere have been
analyzed using SOHO/MDI data. Four active regions emerging near the solar limb
have been considered. It has been found that extended regions of Doppler
velocities with different signs are formed in the first hours of the magnetic
flux emergence in the horizontal velocity field. The flows observed are
directly connected with the emerging magnetic flux; they form at the beginning
of the emergence of active regions and are present for a few hours. The Doppler
velocities of flows observed increase gradually and reach their peak values
4-12 hours after the start of the magnetic flux emergence. The peak values of
the mean (inside the +/-500 m/s isolines) and maximum Doppler velocities are
800-970 m/s and 1410-1700 m/s, respectively. The Doppler velocities observed
substantially exceed the separation velocities of the photospheric magnetic
flux outer boundaries. The asymmetry was detected between velocity structures
of leading and following polarities. Doppler velocity structures located in a
region of leading magnetic polarity are more powerful and exist longer than
those in regions of following polarity. The Doppler velocity asymmetry between
the velocity structures of opposite sign reaches its peak values soon after the
emergence begins and then gradually drops within 7-12 hours. The peak values of
asymmetry for the mean and maximal Doppler velocities reach 240-460 m/s and
710-940 m/s, respectively. An interpretation of the observable flow of
photospheric plasma is given.Comment: 20 pages, 10 figures, 3 tables. The results of article were presented
at the ESPM-13 (12-16 September 2011, Rhodes, Greece, Abstract Book p. 102,
P.4.12,
http://astro.academyofathens.gr/espm13/documents/ESPM13_abstract_programme_book.pdf
Sunspot rotation, filament, and flare: The event on 2000 February 10
We find that a sunspot with positive polarity had an obvious
counter-clockwise rotation and resulted in the formation and eruption of an
inverse S-shaped filament in NOAA active region (AR) 08858 from 2000 February 9
to 10. The sunspot had two umbrae which rotated around each other by 195
degrees within about twenty-four hours. The average rotation rate was nearly 8
degrees per hour. The fastest rotation in the photosphere took place during
14:00UT to 22:01UT on February 9, with the rotation rate of nearly 16 degrees
per hour. The fastest rotation in the chromosphere and the corona took place
during 15:28UT to 19:00UT on February 9, with the rotation rate of nearly 20
degrees per hour. Interestingly, the rapid increase of the positive magnetic
flux just occurred during the fastest rotation of the rotating sunspot, the
bright loop-shaped structure and the filament. During the sunspot rotation, the
inverse S-shaped filament gradually formed in the EUV filament channel. The
filament experienced two eruptions. In the first eruption, the filament rose
quickly and then the filament loops carrying the cool and the hot material were
seen to spiral into the sunspot counterclockwise. About ten minutes later, the
filament became active and finally erupted. The filament eruption was
accompanied with a C-class flare and a halo coronal mass ejection (CME). These
results provide evidence that sunspot rotation plays an important role in the
formation and eruption of the sigmoidal active-region filament.Comment: 20 pages, 9 figures, Accepted for publication in Ap
The Relationship Between Plasma Flow Doppler Velocities and Magnetic Field Parameters During the Emergence of Active Regions at the Solar Photospheric Level
A statistical study has been carried out of the relationship between plasma
flow Doppler velocities and magnetic field parameters during the emergence of
active regions at the solar photospheric level with data acquired by the
Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory
(SOHO). We have investigated 224 emerging active regions with different spatial
scales and positions on the solar disc. The following relationships for the
first hours of the emergence of active regions have been analysed: i) of peak
negative Doppler velocities with the position of the emerging active regions on
the solar disc; ii) of peak plasma upflow and downflow Doppler velocities with
the magnetic flux growth rate and magnetic field strength for the active
regions emerging near the solar disc centre (the vertical component of plasma
flows); iii) of peak positive and negative Doppler velocities with the magnetic
flux growth rate and magnetic field strength for the active regions emerging
near the limb (the horizontal component of plasma flows); iv) of the magnetic
flux growth rate with the density of emerging magnetic flux; v) of the Doppler
velocities and magnetic field parameters for the first hours of the appearance
of active regions with the total unsigned magnetic flux at the maximum of their
development.Comment: 14 pages, 8 figures. The results of article were presented at the
ESPM-13 (12-16 September 2011, Rhodes, Greece, Abstract Book p. 102-103,
P.4.13,
http://astro.academyofathens.gr/espm13/documents/ESPM13_abstract_programme_book.pdf
Discovery of inward moving magnetic enhancements in sunspot penumbrae
Sunspot penumbrae show a fine structure in continuum intensity that displays
considerable dynamics. The magnetic field, in contrast, although also highly
structured, has appeared to be relatively static. Here we report the discovery
of inward moving magnetic enhancements in the penumbrae of two regular sunspots
based on time series of SOHO/MDI magnetograms. Local enhancements of the LOS
component of the magnetic field in the inner part of the penumbral region move
inward to the umbra-penumbra boundary with a radial speed of about 0.3 km
s. These local inward-moving enhancements of the LOS component of the
magnetic fields appear to be relatively common. They are associated with dark
structures and tend to display downflows relatively to the penumbral
background. Possible explanations are discussed.Comment: 4 pages, 4 figures, submitted to ApJ Letter
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