Coronal Magnetic Structures Observing Campaign. 3: Coronal plasma and magnetic field diagnostics derived from multiwaveband active region observations

Schmelz, J. T.; Holman, Gordon D.; Brosius, J. W.; Willson, R. F.

doi:10.1086/174781

Cited by 48 publications

(21 citation statements)

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“…Because they are produced only in specific circumstances when electrons are guided by a magnetic field, they allow the reconstruction of the magnetic field strength in the corona (White et al 1991;Schmelz et al 1994;White and Kundu 1997;Brosius et al 1997;Lee et al 1998Lee et al , 1999. Note that hard X-ray emission often goes hand in hand with radio emission since the efficient emission of both requires electron energies of 10 keV (see Fig.…”

Section: Coronal Magnetic Field Measurements At Radio Wavelengthsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

183

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: Coronal Magnetic Field Measurements At Radio Wavelengthsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

183

125

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“…Main efforts have been connected with application of radio methods based on gyroresonant emission (e.g. Schmelz et al 1994;Brosius et al 1997;Lee et al 1999). However, the radio methods are mainly used for the detection of super-strong, few hundred Gauss magnetic fields over active regions.…”

Section: Introductionmentioning

confidence: 99%

Determination of the coronal magnetic field by coronal loop oscillations

Nakariakov

Ofman²

2001

A&A

489

444

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Abstract. We develop a new method for the determination of the absolute value of the magnetic field strength in coronal closed magnetic structures, based on the analysis of flare-generated oscillations of coronal loops. Interpretation of the oscillations observed in terms of global standing kink waves allows to connect the period of the oscillations and the loops length with the magnetic field strength in the loops. For loop oscillations observed with TRACE on 14th July 1998 and 4th July 1999, we estimate the magnetic field strength as 4-30 G. Using TRACE 171Å and 195Å images of the loop, taken on 4th July 1999 to determine the plasma density, we estimate the magnetic field in the loop as 13 ± 9 G. Improved diagnostic of the loop length, the oscillation period, and the plasma density in the loop will significantly improve the method's precision.

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“…Similarly, Schmelz et al (1994) found that the field strengths deduced from microwave observations in parts of an active region were well reproduced by potential field extrapolations from the photosphere. At least in some active regions, however, microwave observations are providing evidence for significant currents, i.e.…”

Section: Coronal Manifestationsmentioning

confidence: 66%