Temperature variability in X-ray bright points observed with Hinode/XRT

Kariyappa, R.; DeLuca, E. E.; Saar, S. H.; Golub, L.; Damé, Luc; Pevtsov, Alexei A.; Varghese, B. A.

doi:10.1051/0004-6361/201014878

Cited by 28 publications

(24 citation statements)

References 31 publications

(40 reference statements)

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“…The observations indicate that the heating rate of CBPs is highly variable on short time scales, which supports the models involving the magnetic reconnection as the origin of CBPs (see discussion in Kariyappa et al 2011). Recent observations (e.g., Cirtain et al 2007) associate (at least, some) CBPs with the coronal jets which may accelerate the material from low corona and to form a basis for the slow solar wind.…”

Section: Introductionsupporting

confidence: 81%

What SDO tells us about structure and evolution of coronal bright points

et al. 2014

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Using magnetograms and coronal images from two instruments on board the Solar Dynamics Observatory (SDO), we study structure and evolution of a limited number of coronal bright points (CBPs). Our results show that the relation between CBPs and their magnetic footpoints is not simple. In some cases, CBP may appear as a bright portion of a larger loop (with clearly identifiable footpoints), and in some cases, an isolated CBP may develop between magnetic poles, which might not be the closest ones to each other or which might not be involved in the magnetic flux cancellation. We suggest that the magnetic connectivity responsible for formation of isolated coronal bright points is governed by the orientation of the large-scale magnetic field.

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Section: Introductionsupporting

confidence: 81%

What SDO tells us about structure and evolution of coronal bright points

et al. 2014

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“…Brightness fluctuation of BPs can result from either the BP area changing with time, and/or because the BP undergoes a variation in temperature (Kariyappa et al 2011). In actuality, area and temperature changes may be related and naturally result from magnetic field emergence/submergence/reconnection as the agent responsible for the observed modifications.…”

Section: Resultsmentioning

confidence: 99%

Solar Polar X-Ray Jets and Multiple Bright Points: Evidence for Sympathetic Activity

Pucci

Poletto

Sterling

et al. 2012

ApJ

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We present an analysis of X-ray bright points (BPs) and X-ray jets observed by Hinode/X-Ray Telescope on 2007 November 2-4, within the solar northern polar coronal hole. After selecting small subregions that include several BPs, we followed their brightness evolution over a time interval of a few hours, when several jets were observed. We find that most of the jets occurred in close temporal association with brightness maxima in multiple BPs: more precisely, most jets are closely correlated with the brightening of at least two BPs. We suggest that the jets result from magnetic connectivity changes that also induce the BP variability. We surmise that the jets and implied magnetic connectivity we describe are small-scale versions of the active-region-scale phenomenon, whereby flares and eruptions are triggered by interacting bipoles.

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“…The method has been questioned as the filter wavelength bands cover spectral lines formed over a wide range of temperatures that contribute to the signal in each filter (e.g., Martens et al 2002;. The temporal variability of temperature was investigated by Kariyappa et al (2011) using the Hinode/XRT Ti_poly and Al_mesh filter ratio. The temperatures of seven BPs were found to range from 1.11 to 2.31 MK with one CBP reaching as high as 3.44 MK.…”

Section: Temperaturesmentioning

confidence: 99%

Coronal bright points

Madjarska

2019

Living Rev Sol Phys

105

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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 active regions. Most importantly, their simple structure and short lifetimes of less than 20 h that allow to follow their full lifetime evolution present a unique opportunity to investigate outstanding questions in solar physics including coronal heating. The present Living Review is the first review of this essential class of solar phenomena and aims to give an overview of the current knowledge about the CBP general, plasma and magnetic properties. Several transient dynamic phenomena associated with CBPs are also briefly introduced. The observationally derived energetics and the theoretical modelling that aims at explaining the CBP formation and eruptive behaviour are reviewed.

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Temperature variability in X-ray bright points observed with Hinode/XRT

Cited by 28 publications

References 31 publications

What SDO tells us about structure and evolution of coronal bright points

What SDO tells us about structure and evolution of coronal bright points

Solar Polar X-Ray Jets and Multiple Bright Points: Evidence for Sympathetic Activity

Coronal bright points

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