Statistical Properties of Solar Coronal Bright Points

Alipour, Nasibe; Safari, Hossein

doi:10.1088/0004-637x/807/2/175

Cited by 63 publications

(75 citation statements)

References 35 publications

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“…With the ground-based and space telescopes, photospheric BPs are often studied to investigate the condition of the convective flows in and below the photosphere (Feng et al 2013;Jafarzadeh et al 2014;Yang et al 2015Yang et al , 2016Ji et al 2016a,b). These flows are widely accepted to be the ultimate source of the energy; coronal BPs as well as coronal loops are also frequently discussed (Li et al 2013;Zhang et al 2014;Alipour & Safari 2015;Chesny et al 2015;Mou et al 2016) as they were thought to be the most potential candidates for coronal heating.…”

Section: Introductionmentioning

confidence: 99%

Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Zhao

Schmieder

et al. 2017

ApJ

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Section: Introductionmentioning

confidence: 99%

Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Zhao

Schmieder

et al. 2017

ApJ

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“…Coronal jets are often associated with coronal bright points (CBPs) at their bottom (Krieger et al, 1971;Golub et al, 1974;Habbal & Withbroe, 1981;Zhang et al, 2012a;Hong et al, 2014;Alipour & Safari, 2015). As one type of longlived (2−48 hr), small-scale (10 ′′ −40 ′′ ) activities with temperature (1−4 MK; Kariyappa et al, 2011) and density (10 9 −10 10 cm −3 ; Ugarte- Urra et al, 2005) enhancements, CBPs are also believed to be heated by magnetic reconnection in the lower corona (e.g.…”

Section: Introductionmentioning

confidence: 99%

Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Zhang

2016

Sol Phys

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Coronal bright points (CBPs) and jets are ubiquitous small-scale brightenings that are often associated with each other. In this paper, we report our multiwavelength observations of two groups of homologous jets. The first group was observed by the Extreme-Ultraviolet Imager (EUVI) aboard the behind Solar TErrestrial RElations Observatory (STEREO) spacecraft in 171Å and 304Å on 2014 September 10, from a location where data from the Solar Dynamic Observatory (SDO) could not observe. The jets (J1−J6) recurred for six times with intervals of 5−15 minutes. They originated from the same primary CBP (BP1) and propagated in the northeast direction along large-scale, closed coronal loops. Two of the jets (J3 and J6) produced sympathetic CBPs (BP2 and BP3) after reaching the remote footpoints of the loops. The time delays between the peak times of BP1 and BP2 (BP3) are 240±75 s (300±75 s). The jets were not coherent. Instead, they were composed of bright and compact blobs. The sizes and apparent velocities of the blobs are 4.5−9 Mm and 140−380 km s −1 , respectively. The arrival times of the multiple blobs in the jets at the far-end of the loops indicate that the sympathetic CBPs are caused by jet flows rather than thermal conduction fronts. The second group was observed by the Atmospheric Imaging Assembly aboard SDO in various wavelengths on 2010 August 3. Similar to the first group, the jets originated from a short-lived bright point (BP) at the boundary of active region 11092 and propagated along a small-scale, closed loop before flowing into the active region. Several tiny blobs with sizes of ∼1.7 Mm and apparent velocity of ∼238 km s −1 were identified in the jets. We carried out the differential emission measure (DEM) inversions to investigate the temperatures of the blobs, finding that the blobs were multithermal with average temperature of 1.8−3.1 MK. The estimated number densities of the blobs were (1.7−2.8)×10 9 cm −3 .

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“…This Carrington rotation covers the period studied by DeForest et al (2018), and we hence try to provide a representation of the global magnetic field configuration around the Sun at the time of that study. We furthermore made both the heating duration and recurrence interval random, with mean values inspired on the results reported by Alipour & Safari (2015) and Madjarska (2019) for the same time period. our 1-D reference case (as a function of height above the solar surface).…”

Section: Simulation Setupmentioning

confidence: 99%

“…The statistical analysis of CBPs by Alipour & Safari (2015) reveals that, in April 2014, when the deep-field campaign of DeForest et al (2018) took place, the av-erage daily number of CBPs observed on the entire visible solar disk was around 550. If one extrapolates this number to the full photosphere, covering 41253 deg 2 in total, we can infer that in April 2014 there were about 0.02 CBP per deg 2 per day.…”

Section: Introductionmentioning

confidence: 99%

Coronal Bright Points as Possible Sources of Density Variations in the Solar Corona

Griton

Pinto

Poirier

et al. 2020

ApJ

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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 an ubiquitous manner in the solar wind. The present study investigates whether these density fluctuations could originate from the transient heating of the low corona observed during Coronal Bright Points (CBPs). We assume that part of the intense heating measured during CBPs occurs at the coronal base of open magnetic fields that channel the forming solar wind. We employ the solar wind model MULTI-VP to quantify the plasma compression induced by transient heating and investigate how the induced perturbation propagates to the upper corona. We show that for heating rates with statistics comparable to those observed during CBPs the compressive wave initially increases the local plasma density by a factor of up to 50% at 5 R . The wave expands rapidly beyond 30 solar radii and the local enhancement in density decreases beyond. Based on the occurrence rates of CBPs measured in previous studies, we impose transient heating events at the base of thousands of open magnetic field lines to study the response of the entire 3-D corona. The simulated density cubes are then converted into synthetic white-light imagery. We show that the resulting brightness variations occupy all position angles in the images on timescales of hours. We conclude that a significant part of the ubiquitous brightness variability of the solar corona could originate in the strong transient heating of flux tubes induced by CBPs.

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Statistical Properties of Solar Coronal Bright Points

Cited by 63 publications

References 35 publications

Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations

Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

Coronal Bright Points as Possible Sources of Density Variations in the Solar Corona

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