Observations of high-energy jets in the corona above the quiet sun, the heating of the corona, and the acceleration of the solar wind

Brueckner, G. E.; Bartoe, J. D. F.

doi:10.1086/161297

Cited by 332 publications

(187 citation statements)

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“…Already in the 80s of the last century, Brueckner and Bartoe (1983) reported observations of high-energy supersonic jets in quiet-Sun areas. They found that the associated shock waves reached to heights of about 4 to 16 Mm.…”

Section: Jetsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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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.

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Section: Jetsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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“…The main characteristics of the explosive events were studied by Brueckner & Bartoe (1983), Dere et al (1989), Porter & Dere (1991), Innes et al (1997Innes et al ( , 2001), Chae et al (1998), Pérez et al (1999), Teriaca et al (2001), and Teriaca et al (2002).…”

Section: Introductionmentioning

confidence: 99%

Simultaneous observations of solar transition region blinkers and explosive events by SUMER, CDS and BBSO

Madjarska¹,

Doyle²

2003

A&A

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Abstract. The SoHO discovery of the new "blinker" phenomena focused our study on the search of its relation to already known phenomena such as explosive events and spicules. The study was performed using a specially planned joint observing program involving the Coronal Diagnostic Spectrometer (CDS), Solar Ultraviolet Measurements of Emitted Radiation spectrograph (SUMER) and Big Bear Solar Observatory (BBSO) magnetograph. Within each blinker, the SUMER data reveal the presence of small-scale (3 -5 ), short-lived (2-3 min) bright features not seen in the CDS data which has sometimes being interpreted as oscillations in SUMER data. With this data we have clearly identified UV explosive events in CDS data. The explosive events show a size close to the small-scale brightenings forming the blinker core. However, they appear in the SUMER data with their typical strong blue and red wings while the blinker shows at best only a small increase in the emission of the blue and red wings and in most instances the typical transition region red-shift in the center of the line. In all cases the explosive events cover one pixel in CDS corresponding to a size of 4 × 4 −6 . All identified explosive events were located at the border of the bright network i.e. the blinker, in the network or even in the internetwork. From this data, we believe that blinkers and explosive events are two separate phenomena not directly related or triggering each other. In this study, the Doppler shift was derived in a blinker phenomenon for the first time. It ranges from -5 to 25 km s −1 and is predominantly red-shifted. The observed magnetic flux increase during the blinker phenomena seems to play a crucial role in the development of this event. We suggest that "blinkers" maybe the on-disk signature of spicules.

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“…They have a typical lifetime of 60 s, sizes of 2000 km and flow velocities of about 100 km s −1 . They were discovered in high resolution ultraviolet spectra of the Sun (Brueckner and Bartoe, 1983;Dere, Bartoe and Brueckner, 1989). They appear as small sites with large red and/or blue Doppler shifted emission lines of species which are formed at electron temperatures in the range 5 × 10 4 − 5 × 10 5 K. Recent observations have revealed several examples where the spatial and temporal evolution of the line profiles clearly indicate bidirectional flows (Innes et al, 1997;Wilhelm et al, 1998).…”

Section: Introductionmentioning

confidence: 99%

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Innes

Tóth

1999

Solar Physics

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Abstract. Small-scale explosive events or microflares occur throughout the chromospheric network of the Sun. They are seen as sudden bursts of highly Doppler shifted spectral lines of ions formed at temperatures in the range 2 × 10 4 − 5 × 10 5 K. They tend to occur near regions of cancelling photospheric magnetic fields and are thought to be directly associated with magnetic field reconnection. Recent observations have revealed that they have a bi-directional jet structure reminiscent of Petschek reconnection. In this paper compressible MHD simulations of the evolution of a current sheet to a steady Petschek, jet-like configuration are computed using the Versatile Advection Code. We obtain velocity profiles that can be compared with recent ultraviolet line profile observations. By choosing initial conditions representative of magnetic loops in the solar corona and chromosphere, it is possible to explain the fact that jets flowing outward into the corona are more extended and appear before jets flowing towards the chromosphere. This model can reproduce the high Doppler shifted components of the line profiles but the brightening at low velocities, near the centre of the bi-directional jet, cannot be explained by this simple MHD model.

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Observations of high-energy jets in the corona above the quiet sun, the heating of the corona, and the acceleration of the solar wind

Cited by 332 publications

References 0 publications

The magnetic field in the solar atmosphere

The magnetic field in the solar atmosphere

Simultaneous observations of solar transition region blinkers and explosive events by SUMER, CDS and BBSO

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