Coronal bright points

@article{Madjarska2019CoronalBP,
  title={Coronal bright points},
  author={Maria S. Madjarska},
  journal={Living Reviews in Solar Physics},
  year={2019},
  volume={16},
  pages={1-79}
}
  • M. Madjarska
  • Published 2019
  • Physics
  • Living Reviews in Solar Physics
Coronal bright points (CBPs) are a fundamental class of solar activity. They represent a set of low-corona small-scale loops with enhanced emission in the extreme-ultraviolet and X-ray spectrum that connect magnetic flux concentrations of opposite polarities. CBPs are one of the main building blocks of the solar atmosphere outside active regions uniformly populating the solar atmosphere including active region latitudes and coronal holes. Their plasma properties classify them as downscaled… Expand
Coronal Bright Points as Possible Sources of Density Variations in the Solar Corona
Recent analysis of high-cadence white-light images taken by the Solar-Terrestrial RElations Observatory (STEREO) near solar maximum has revealed that outflowing density structures are released in anExpand
Observations of the Quiet Sun during the Deepest Solar Minimum of the Past Century with Chandrayaan-2 XSM: Sub-A-class Microflares outside Active Regions
Solar flares, with energies ranging over several orders of magnitude, result from impulsive release of energy due to magnetic reconnection in the corona. Barring a handful, almost all microflaresExpand
Population of Bright Plume Threads in Solar Polar Coronal Holes
Coronal holes are well accepted to be source regions of the fast solar wind. As one of the common structures in coronal holes, coronal plumes might contribute to the origin of the nascent solar wind.Expand
Latitudinal distribution of solar coronal active regions
Abstract We studied the cyclic evolution of the latitudinal distribution of solar coronal active regions based on daily images from SOHO EIT for the period 1995-2017. Fully automated software wasExpand
How Rotating Solar Atmospheric Jets Become Kelvin–Helmholtz Unstable
Recent observations support the propagation of a number of magnetohydrodynamic (MHD) modes which, under some conditions, can become unstable and the developing instability is the Kelvin--HelmholtzExpand
A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response
Inspired by recent observations suggesting that photospheric magnetic flux cancellation occurs much more frequently than previously thought, we analytically estimated the energy released fromExpand
Rossby Waves in Astrophysics
Rossby waves are a pervasive feature of the large-scale motions of the Earth’s atmosphere and oceans. These waves (also known as planetary waves and r-modes) also play an important role in theExpand
Solar Wind Helium Abundance Heralds Solar Cycle Onset
We study the solar wind helium-to-hydrogen abundance's ($A_\mathrm{He}$) relationship to solar cycle onset. Using OMNI/Lo data, we show that $A_\mathrm{He}$ increases prior to sunspot number (SSN)Expand
Solar Wind Helium Abundance Heralds Solar Cycle Onset
We study the solar wind helium-to-hydrogen abundance’s ( $A_{ {\mathrm {He}}}$ ) relationship to solar cycle onset. Using OMNI/Lo data, we show that $A_{ {\mathrm {He}}}$ increases prior toExpand
On the Nature of Propagating Intensity Disturbances in Polar Plumes during the 2017 Total Solar Eclipse
The propagating intensity disturbances (PIDs) in plumes are still poorly understood, and their identity (magnetoacoustic waves or flows) remains an open question. We investigate PIDs in five plumesExpand
...
1
2
...

References

SHOWING 1-10 OF 199 REFERENCES
Coronal Bright Points Associated with Minifilament Eruptions
Coronal bright points (CBPs) are small-scale, long-lived coronal brightenings that always correspond to photospheric network magnetic features of opposite polarity. In this paper, we subjectivelyExpand
Emission heights of coronal bright points on Fe XII radiance map
Abstract The study of coronal bright points (BPs) is important for understanding coronal heating and the origin of the solar wind. Previous studies indicated that coronal BPs have a highlyExpand
Signature of oscillations in coronal bright points
A detailed study of two consecutive bright points observed simultaneously with the Coronal Diagnostic Spectrometer (CDS), the Extreme ultraviolet Imaging Telescope (EIT) and the Michelson DopplerExpand
BRIGHT POINTS: MULTITHERMAL ANALYSIS AS A TEST OF STEADY HEATING MODELS
X-ray bright points are small, million-degree features in the solar atmosphere composed of short coronal loops. They are magnetically driven structures associated with photospheric magnetic bipoles.Expand
X-ray observations of characteristic structures and time variations from the solar corona: preliminary results from Skylab
Examples taken from the S-054 X-ray telescope observations made during the first Skylab mission show the hot coronal plasma tracing the configuration of the magnetic fields. The high spectralExpand
The correspondence between x-ray bright points and evolving magnetic features in the quiet sun
Coronal bright points, first identified as X-ray Bright Points (XBPs), are compact, short-lived and associated with small-scale, opposite polarity magnetic flux features. Previous studies haveExpand
TWO TYPES OF MAGNETIC RECONNECTION IN CORONAL BRIGHT POINTS AND THE CORRESPONDING MAGNETIC CONFIGURATION
Coronal bright points (CBPs) are long-lived small-scale brightenings in the solar corona. They are generally explained by magnetic reconnection. However, the corresponding magnetic configurations areExpand
Coronal hole boundaries evolution at small scales - II. XRT view. Can small-scale outflows at CHBs be a source of the slow solar wind?
Aims. We aim to further explore the small-scale evolution of coronal hole boundaries using X-ray high-resolution and high-cadence images. We intend to determine the fine structure and dynamics of theExpand
Network boundary origins of fast solar wind seen in the low transition region
We present a study of a high spatial resolution raster acquired on-disk with the SUMER (Solar Ultraviolet Measurements of Emitted Radiation) grating spectrograph on SoHO (the Solar and HeliosphericExpand
A comparison between bright points in a coronal hole and a quiet-sun region
A comparison is made of the morphological structure and temporal behavior of the emission from coronal bright points in a coronal hole and a quiet region, using data from the Harvard EUV experimentExpand
...
1
2
3
4
5
...