Solar X-Ray Bright Points

Golub, L.; Krieger, A. S.; Silk, J. K.; Timothy, A. F.; Vaiana, G. S.

doi:10.1086/181472

Cited by 287 publications

(185 citation statements)

References 0 publications

Supporting

Mentioning

179

Contrasting

Unclassified

Order By: Relevance

“…1.1.1) were also found to be centers of activity Harvey and Martin (1973). As in their active-region counterparts, the photospheric magnetic field in the ephemeral regions drives activity, such as X-ray bright points, (Golub et al 1974(Golub et al , 1977Priest 1994) in the upper solar atmosphere. The color-coded background resembles the cotemporal WIND/WAVES frequency-time radio spectra.…”

Section: Quiet-sun Magnetic Fieldsmentioning

confidence: 92%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

172

125

View full text Add to dashboard Cite

This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

show abstract

Section: Quiet-sun Magnetic Fieldsmentioning

confidence: 92%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

172

125

View full text Add to dashboard Cite

show abstract

“…They have been studied in detail by Golub et al (1974Golub et al ( , 1977 and Golub (1980), who found that bright points had a mean lifetime of 8 h in X rays and were associated with emerging magnetic flux. The spacing between the magnetic poles increased with time.…”

Section: Bright Pointsmentioning

confidence: 99%

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

et al. 2007

View full text Add to dashboard Cite

In Part I of this review, the concepts of solar vacuum-ultraviolet (VUV) observations were outlined together with a discussion of the space instrumentation used for the investigations. A section on spectroradiometry provided some quantitative results on the solar VUV radiation without considering any details of the solar phenomena leading to the radiation. Here, in Part II, we present solar VUV observations over the last decades and their interpretations in terms of the plasma processes and the parameters of the solar atmosphere, with emphasis on the spatial and thermal structures of the chromosphere, transition region and corona of the quiet Sun. In addition, observations of active regions, solar flares and prominences are included as well as of small-scale events. Special sections are devoted to the elemental composition of the solar atmosphere and theoretical considerations on the heating of the corona and the generation of the solar wind.

show abstract

“…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

View full text Add to dashboard Cite

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 .

show abstract

Solar X-Ray Bright Points

Cited by 287 publications

References 0 publications

The magnetic field in the solar atmosphere

The magnetic field in the solar atmosphere

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

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

Contact Info

Product

Resources

About