Rotation of the magnetic elements in polar regions on the Sun

2007 ◽  
Vol 328 (10) ◽  
pp. 1016-1019 ◽  
Author(s):  
E.E. Benevolenskaya
Keyword(s):  
Polar Regions ◽  
The Sun ◽  
Magnetic Elements

scholarly journals Ulysses COSPIN observations of cosmic rays and solar energetic particles from the South Pole to the North Pole of the Sun during solar maximum

2003 ◽  
Vol 21 (6) ◽  
pp. 1217-1228 ◽  
Author(s):  
R. B. McKibben ◽  
J. J. Connell ◽  
C. Lopate ◽  
M. Zhang ◽  
J. D. Anglin ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Solar Maximum ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Polar Regions ◽  
The Sun ◽  
The South ◽  
The North ◽  
Inner Heliosphere

Abstract. In 2000–2001 Ulysses passed from the south to the north polar regions of the Sun in the inner heliosphere, providing a snapshot of the latitudinal structure of cosmic ray modulation and solar energetic particle populations during a period near solar maximum.  Observations from the COSPIN suite of energetic charged particle telescopes show that latitude variations in the cosmic ray intensity in the inner heliosphere are nearly non-existent near solar maximum, whereas small but clear latitude gradients were observed during the similar phase of Ulysses’ orbit near the 1994–95 solar minimum. At proton energies above ~10 MeV and extending up to >70 MeV, the intensities are often dominated by Solar Energetic Particles (SEPs) accelerated near the Sun in association with intense solar flares and large Coronal Mass Ejections (CMEs). At lower energies the particle intensities are almost constantly enhanced above background, most likely as a result of a mix of SEPs and particles accelerated by interplanetary shocks. Simultaneous high-latitude Ulysses and near-Earth observations show that most events that produce large flux increases near Earth also produce flux increases at Ulysses, even at the highest latitudes attained. Particle anisotropies during particle onsets at Ulysses are typically directed outwards from the Sun, suggesting either acceleration extending to high latitudes or efficient cross-field propagation somewhere inside the orbit of Ulysses. Both cosmic ray and SEP observations are consistent with highly efficient transport of energetic charged particles between the equatorial and polar regions and across the mean interplanetary magnetic fields in the inner heliosphere.Key words. Interplanetary physics (cosmic rays) – Solar physics, astrophysics and astronomy (energetic particles; flares and mass ejections)

scholarly journals II. On a supposed periodicity in the elements of terrestrial mag­netism, with a period of 26 1/3 days

1872 ◽  
Vol 20 (130-138) ◽  
pp. 308-312 ◽  
Keyword(s):  
The Sun ◽  
Horizontal Force ◽  
Magnetic Elements ◽  
Royal Observatory ◽  
Imperial Academy ◽  
Meteorological Observations ◽  
Academy Of Sciences ◽  
Periodical Change

In a paper published in the ‘Proceedings of the Imperial Academy of Sciences of Vienna,’ vol. lxiv., Dr. Karl Hornstein has exhibited the results of a series of observations which appeared to show that the earths magnetism undergoes a periodical change in successive periods of 26 1/3 days, which might with great plausibility be referred to the rotation of the sun. It appeared to me that the deductions from the magnetic observations made at the Royal Observatory of Greenwich, and which are printed annually in the Greenwich Observations,’ or in the detached copies of ‘Results of Magnetical and Meteorological Observations made at the Royal Observatory of Greenwich, would afford good materials for testing the accuracy of this law, as applicable to a series of years. The mew results of the measured hourly ordinates of the terrestrial magnetic elements are given for every day, and it is certain that there has been no change of adjustments of the declination and horizontal-force instruments in the course of each year. For the horizontal-force instrument the temperature of the room has been maintained in a generally equable state, and in later years it has been remarkably uniform.

scholarly journals XV. Results of magnetical observations made in Little Namaqualand during a part of the months of April and May, 1874

1875 ◽  
Vol 23 (156-163) ◽  
pp. 553-563
Keyword(s):  
The Sun ◽  
Magnetic Elements ◽  
Made In

An eclipse of the sun was to occur on April 16, 1874, which would be total throughout Little Namaqualand. I made arrangements for a visit to this country to observe the eclipse. The country is one rarely visited. I was not aware that any determinations of the magnetic elements had been made there, except a few of the variation by the Admiralty surveyors at one or two points along the coast. It appeared to me desirable that the opportunity afforded by my visit to observe the eclipse should not be lost of securing magnetical observations at several stations in Namaqualand.

scholarly journals Solar and stellar magnetic flux tubes

1996 ◽  
Vol 176 ◽  
pp. 201-216
Author(s):  
Sami K. Solanki
Keyword(s):  
Magnetic Field ◽  
Magnetic Properties ◽  
Magnetic Flux ◽  
Large Range ◽  
The Sun ◽  
Flux Tubes ◽  
Magnetic Elements ◽  
Turbulent Pressure ◽  
Magnetic Flux Tubes ◽  
The Magnetic Field

The magnetic field of the Sun is mainly concentrated into intense magnetic flux tubes having field strengths of the order of 1 kG. In this paper an overview is given of the thermal and magnetic properties of these flux tubes, which are known to exhibit a large range in size, from the smallest magnetic elements to sunspots. Differences and similarities between the largest and smallest features are stressed. Some thoughts are also presented on how the properties of magnetic flux tubes are expected to scale from the solar case to that of solar-like stars. For example, it is pointed out that on giants and supergiants turbulent pressure may dominate over gas pressure as the main confining agent of the magnetic field. Arguments are also presented in favour of a highly complex magnetic geometry on very active stars. Thus the very large starspots seen in Doppler images probably are conglomerates of smaller (but possibly still sizable) spots.

scholarly journals 1.1.13 A Temporal Study of the Radiance of the F-Corona Close to the Sun

1976 ◽  
Vol 31 ◽  
pp. 65-65
Author(s):  
R.H. Munro
Keyword(s):  
Temporal Variations ◽  
Stray Light ◽  
Polar Regions ◽  
The Sun ◽  
Photometric Calibration ◽  
Temporal Study ◽  
Single Region ◽  
Solar Eruptions ◽  
The Individual ◽  
Source Of Error

During the Skylab mission – May 1973 through February 1974 – the High Altitude Observatory’s white light coronagraph observed the sum of the F-corona, electron scattered K-corona, and instrumental stray light between 0.4 and 1.6 degrees from the sun. In searching for temporal variations in the F-corona, measurements were confined to the solar polar regions to minimize the effects of the K-coronal component. Changes in instrumental stray light were eliminated by restricting measurements to a single region within the instruments’ field of view. The largest source of error is the photometric calibration of the individual rolls of film. Frames were specifically selected to encompass periods of time ranging from a few days to eight months. Generally no variation in the total radiance greater than three percent was detected for intervals on the order of a few weeks. This level of stability holds for most of the eight-month period, excepting a few instances when deviations of up to eight percent were observed where the calibration is most uncertain. A preliminary study of the asymmetry in the F-corona close to the sun and the possible effect of solar eruptions (e.g., flares and prominences) upon the F-corona will be discussed.

The Solar Orbiter mission – Exploring the Sun and heliosphere

2021 ◽  
Author(s):  
Daniel Mueller ◽  
Yannis Zouganelis ◽  
Teresa Nieves-Chinchilla ◽  
Chris St. Cyr
Keyword(s):  
High Spatial Resolution ◽  
Ecliptic Plane ◽  
Space Mission ◽  
Polar Regions ◽  
The Sun ◽  
Very High Spatial Resolution ◽  
New Perspective ◽  
Orbiter Mission ◽  
Very High

<p>Solar Orbiter, launched on 10 February 2020, is a space mission of international collaboration between ESA and NASA. It is exploring the linkage between the Sun and the heliosphere and has started to collect unique data at solar distances down to 0.49 AU. By ultimately approaching as close as 0.28 AU, Solar Orbiter will view the Sun with very high spatial resolution and combine this with in-situ measurements of the surrounding heliosphere. Over the course of the mission, the highly elliptical orbit will get progressively more inclined to the ecliptic plane. Thanks to this new perspective, Solar Orbiter will deliver images and comprehensive data of the unexplored Sun’s polar regions and the side of the Sun not visible from Earth. This talk will highlight first science results from Solar Orbiter and provide a mission status update.</p>

Solar Orbiter: Europe's mission to the Sun

2020 ◽  
Author(s):  
Yannis Zouganelis ◽  
Daniel Mueller ◽  
Chris St Cyr ◽  
Holly Gilbert ◽  
Teresa Nieves-Chinchilla
Keyword(s):  
High Spatial Resolution ◽  
Solar Wind Plasma ◽  
Ecliptic Plane ◽  
Current Status ◽  
Polar Regions ◽  
The Sun ◽  
Physical Processes ◽  
New Perspective ◽  
Orbiter Mission

<p><span>ESA’s Solar Orbiter mission is scheduled for launch in February 2020, and will focus on exploring the linkage between the Sun and the heliosphere. It is a collaborative mission with NASA that will collect unique data that will allow us to study, e.g., the coupling between macroscopic physical processes to those on kinetic scales, the generation of solar energetic particles and their propagation into the heliosphere, and the origin and acceleration of solar wind plasma. By approaching as close as 0.28 AU, Solar Orbiter will view the Sun with high spatial resolution and combine this with in-situ measurements of the surrounding heliosphere. Over the course of the mission, the highly elliptical orbit will get progressively more inclined to the ecliptic plane. Thanks to this new perspective, Solar Orbiter will deliver images and comprehensive data of the unexplored Sun’s polar regions and the side of the Sun not visible from Earth. This talk will provide a mission overview, highlight synergies with NASA’s Parker Solar Probe and summarise current status.</span></p>

The increase in the magnetic flux from the polar regions of the Sun over the last 120 years

2001 ◽  
Vol 45 (9) ◽  
pp. 746-750 ◽  
Author(s):  
V. I. Makarov ◽  
V. N. Obridko ◽  
A. G. Tlatov
Keyword(s):  
Magnetic Flux ◽  
Polar Regions ◽  
The Sun

scholarly journals Solar Differential Rotation of Compact Magnetic Elements and Polarity Reversal of the Sun

2008 ◽  
Vol 4 (S257) ◽  
pp. 173-176 ◽  
Author(s):  
Darejan Japaridze ◽  
Marina Gigolashvili ◽  
Vasili Kukhianidze
Keyword(s):  
Differential Rotation ◽  
Rotation Rate ◽  
Temporal Variability ◽  
Large Scale ◽  
Opposite Polarity ◽  
Polarity Reversal ◽  
The Sun ◽  
Solar Differential Rotation ◽  
Spatially Resolved ◽  
Magnetic Elements

AbstractThe differential rotation of the compact elements of the large-scale magnetic fields is studied using Solar Synoptic Charts (1966–1986). It is revealed that compact magnetic elements with the similar polarity of the polar magnetic field of the Sun have a larger rotation rate than the elements with the opposite polarity at all stages in the cycle.From the comparison of the experimental measuring data of the solar magnetic elements there are received the results: a) The differential rotations of the compact magnetic elements with negative and positive polarities have the similar behavior for the solar 20 and 21 cycles; b) It is established that in the rotation rate of compact magnetic elements there are present some variations at the time of polarity reversal of the Sun.There is assumed that the physical understanding of the connections of differential rotation of compact magnetic elements and polarity reversal of the Sun depends upon establishing a connection between the temporal variability of spatially resolved solar magnetic elements and polar reversals.

scholarly journals DETECTION OF SUPERGRANULATION ALIGNMENT IN POLAR REGIONS OF THE SUN BY HELIOSEISMOLOGY

2010 ◽  
Vol 726 (2) ◽  
pp. L17 ◽  
Author(s):  
Kaori Nagashima ◽  
Junwei Zhao ◽  
Alexander G. Kosovichev ◽  
Takashi Sekii
Keyword(s):  
Polar Regions ◽  
The Sun
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