The Horizontal Magnetic Flux of the Quiet‐Sun Internetwork as Observed with theHinodeSpectro‐Polarimeter

2008 ◽  
Vol 672 (2) ◽  
pp. 1237-1253 ◽  
Author(s):  
B. W. Lites ◽  
M. Kubo ◽  
H. Socas‐Navarro ◽  
T. Berger ◽  
Z. Frank ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Quiet Sun

scholarly journals Evolution of Stokes V area asymmetry related to a quiet Sun cancellation observed with GRIS/IFU

2020 ◽  
Vol 634 ◽  
pp. A131
Author(s):  
A. J. Kaithakkal ◽  
J. M. Borrero ◽  
C. E. Fischer ◽  
C. Dominguez-Tagle ◽  
M. Collados
Keyword(s):  
Magnetic Flux ◽  
Opposite Polarity ◽  
Disk Center ◽  
Significant Rise ◽  
Polarity Inversion ◽  
Quiet Sun ◽  
Additional Information ◽  
Line Core ◽  
Polarity Inversion Line ◽  
Field Unit

A quiet Sun magnetic flux cancellation event at the disk center was recorded using the Integral Field Unit (IFU) mounted on the GREGOR Infrared Spectrograph (GRIS). The GRIS instrument sampled the event in the photospheric Si I 10827 Å spectral line. The cancellation was preceded by a significant rise in line core intensity and excitation temperature, which is inferred from Stokes inversions under local thermodynamic equilibrium (LTE). The opposite polarity features seem to undergo reconnection above the photosphere. We also found that the border pixels neighboring the polarity inversion line of one of the polarities exhibit a systematic variation of area asymmetry. Area asymmetry peaks right after the line core intensity enhancement and gradually declines thereafter. Analyzing Stokes profiles recorded from either side of the polarity inversion line could therefore potentially provide additional information on the reconnection process related to magnetic flux cancellation. Further analysis without assuming LTE will be required to fully characterize this event.

scholarly journals Emergence of small-scale magnetic flux in the quiet Sun

2020 ◽  
Vol 633 ◽  
pp. A67 ◽  
Author(s):  
I. Kontogiannis ◽  
G. Tsiropoula ◽  
K. Tziotziou ◽  
C. Gontikakis ◽  
C. Kuckein ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Morphological Characteristics ◽  
Small Scale ◽  
X Rays ◽  
Coronal Emission ◽  
Quiet Sun ◽  
Temperature Regimes ◽  
Multi Wavelength ◽  
Modelling Studies

Context. We study the evolution of a small-scale emerging flux region (EFR) in the quiet Sun, from its emergence in the photosphere to its appearance in the corona and its decay. Aims. We track processes and phenomena that take place across all atmospheric layers; we explore their interrelations and compare our findings with those from recent numerical modelling studies. Methods. We used imaging as well as spectral and spectropolarimetric observations from a suite of space-borne and ground-based instruments. Results. The EFR appears in the quiet Sun next to the chromospheric network and shows all morphological characteristics predicted by numerical simulations. The total magnetic flux of the region exhibits distinct evolutionary phases, namely an initial subtle increase, a fast increase with a Co-temporal fast expansion of the region area, a more gradual increase, and a slow decay. During the initial stages, fine-scale G-band and Ca II H bright points coalesce, forming clusters of positive- and negative-polarity in a largely bipolar configuration. During the fast expansion, flux tubes make their way to the chromosphere, pushing aside the ambient magnetic field and producing pressure-driven absorption fronts that are visible as blueshifted chromospheric features. The connectivity of the quiet-Sun network gradually changes and part of the existing network forms new connections with the newly emerged bipole. A few minutes after the bipole has reached its maximum magnetic flux, the bipole brightens in soft X-rays forming a coronal bright point. The coronal emission exhibits episodic brightenings on top of a long smooth increase. These coronal brightenings are also associated with surge-like chromospheric features visible in Hα, which can be attributed to reconnection with adjacent small-scale magnetic fields and the ambient quiet-Sun magnetic field. Conclusions. The emergence of magnetic flux even at the smallest scales can be the driver of a series of energetic phenomena visible at various atmospheric heights and temperature regimes. Multi-wavelength observations reveal a wealth of mechanisms which produce diverse observable effects during the different evolutionary stages of these small-scale structures.

The magnetic flux in the quiet sun network

Solar Physics ◽  
1982 ◽  
Vol 80 (1) ◽  
pp. 15-19 ◽  
Author(s):  
Barry J. Labonte ◽  
Robert Howard
Keyword(s):  
Magnetic Flux ◽  
Quiet Sun

scholarly journals Estimation of the Magnetic Flux Emergence Rate in the Quiet Sun from Sunrise Data

2017 ◽  
Vol 229 (1) ◽  
pp. 17 ◽  
Author(s):  
H. N. Smitha ◽  
L. S. Anusha ◽  
S. K. Solanki ◽  
T. L. Riethmüller
Keyword(s):  
Magnetic Flux ◽  
Flux Emergence ◽  
Quiet Sun ◽  
Emergence Rate

Characterization of Magnetic Flux in the Quiet Sun

2002 ◽  
Vol 573 (1) ◽  
pp. 431-444 ◽  
Author(s):  
B. W. Lites
Keyword(s):  
Magnetic Flux ◽  
Quiet Sun

scholarly journals Wave Heating in Magnetic Flux Tubes

1990 ◽  
Vol 138 ◽  
pp. 185-188
Author(s):  
Wolfgang Kalkofen
Keyword(s):  
Magnetic Flux ◽  
Solar Chromosphere ◽  
Flux Tubes ◽  
Quiet Sun ◽  
Long Period ◽  
Wave Heating ◽  
Magnetic Flux Tubes

The solar chromosphere is identified with the atmosphere inside magnetic flux tubes. In the quiet sun, the layers of the low and middle chromosphere are heated by compressive waves with periods mainly between 2 min and 4 min. These long-period waves probably supply all the energy required for the heating of the quiet solar chromosphere.

scholarly journals Irradiance Models Based on Solar Magnetic Fields

1994 ◽  
Vol 143 ◽  
pp. 217-225 ◽  
Author(s):  
Karen L. Harvey
Keyword(s):  
Active Region ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Coronal Holes ◽  
Active Regions ◽  
Spectral Irradiance ◽  
Solar Magnetic Fields ◽  
Quiet Sun ◽  
Possible Cause

A method to separate the active region and quiet network components of the magnetic fields in the photosphere is described and compared with the corresponding measurements of the He I λ 10830 absorption. The relation between the total He I absorption and total magnetic flux in active regions is roughly linear and differs between cycles 21 and 22. There appears to no relation between these two quantities in areas outside of active regions. The total He I absorption in the quiet Sun (comprised of network, filaments, and coronal holes) exceeds that in active regions at all times during the cycle. As a whole, active regions of cycle 22 appear to be less complex than the active regions of cycle 21, hinting at one possible cause for a differing relation between spectral-irradiance variations and the underlying magnetic flux for these two cycles.

scholarly journals Are the umbral dots, penumbral grains, and G band bright points formed by the same type of magnetic flux tubes?

2010 ◽  
Vol 6 (S273) ◽  
pp. 426-429
Author(s):  
Isroil Sattarov
Keyword(s):  
Magnetic Flux ◽  
Solar Atmosphere ◽  
Solar Physics ◽  
Common Type ◽  
Present Evidence ◽  
Flux Tubes ◽  
Quiet Sun ◽  
Magnetic Flux Tubes ◽  
Fine Structures ◽  
Umbral Dots

AbstractToday's Solar Physics comes across of different type of fine structures in solar atmosphere including umbral dots and penumbral grains in sunspots, and G-band bright points in quiet Sun. In this report, we present evidence that umbral dots, penumbral grains, and, possibly, G band bright points are related to a common type of features in solar atmosphere magnetic flux tubes.

scholarly journals Small-Scale Magnetic Features Observed in the Photosphere

1990 ◽  
Vol 138 ◽  
pp. 129-146 ◽  
Author(s):  
Sara F. Martin
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Active Regions ◽  
Line Of Sight ◽  
Small Scale ◽  
Quiet Sun ◽  
Magnetic Features

Small-scale solar features identifiable on the quiet sun in magnetograms of the line-of-sight component consist of network, intranetwork, ephemeral region magnetic fields, and the elementary bipoles of ephemeral active regions. Network fields are frequently observed to split into smaller fragments and equally often, small fragments are observed to merge or coalesce into larger clumps; this splitting and merging is generally confined to the borders and vertices of the convection cells known as supergranules. Intranetwork magnetic fields originate near the centers of the supergranule convection cells and appear to increase in magnetic flux as they flow in approximate radial patterns towards the boundaries of the cells.

Sign in / Sign up

Export Citation Format

Share Document