Energy Balance

Gilbert, H. R.

doi:10.1007/978-3-319-10416-4_7

Cited by 13 publications

(3 citation statements)

References 53 publications

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“…Reproduced from Labrosse et al (2022). Frontiers in Astronomy and Space Sciences frontiersin.org well understood under the prominence conditions (Gilbert, 2015). A reliable knowledge of the temperature distribution within the prominence fine structures and its temporal evolution will also help our understanding of the magnetothermal convection processes discussed in Berger et al (2011).…”

Section: Observations and Plasma Diagnosticsmentioning

confidence: 98%

Prominence observations with ALMA

Heinzel

Bárta²,

Gunár³

et al. 2022

Front. Astron. Space Sci.

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This review comes at the time when ALMA successfully obtained the first regular observations of both a prominence and a filament. These observations have a spatial resolution of 1-2 arcsec, far better than previous prominence observations in the mm/sub-mm radio domain. The achieved resolution is compatible with the cotemporal ground-based coronagraphic observations in the hydrogen Hα line that accompany the ALMA Band 3 prominence observations. A core part of this review is the description and analysis of these pioneering ALMA observations of a quiescent prominence, focusing on various physical and geometrical properties of the observed prominence fine structures. We also summarize the basic physical processes behind the formation of mm/sub-mm continua under prominence conditions and describe the plasma diagnostics potential of ALMA solar observations. Finally, we discuss future prospects of ALMA prominence observations and the value of coordinated optical and UV spectra and images.

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Section: Observations and Plasma Diagnosticsmentioning

confidence: 98%

Prominence observations with ALMA

Heinzel

Bárta²,

Gunár³

et al. 2022

Front. Astron. Space Sci.

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“…In order to exist, prominences need mechanical equilibrium as well as a detailed energy balance between heating and radiative cooling. Energy balance studies suggest that incident radiation provides most of the heating of prominence plasma (H. Gilbert, 2015), however, this radiative heating depends on the illumination from the surrounding atmosphere. Moreover, radiative equilibrium prominence models, constructed from a balance between incident radiation and cooling (Anzer & Heinzel, 1999; Heinzel & Anzer, 2012; Heinzel et al., 2010), as well as differential emission measures have pointed out that a further unknown heating is required in order to reproduce the observed temperatures in the prominence cores (Heinzel, 2015; Heinzel & Anzer, 2012; Labrosse et al., 2010) and to balance the radiative losses (Parenti, 2014; Parenti & Vial, 2007).…”

Section: Heating Of the Chromospherementioning

confidence: 99%

Chromospheric Heating by Magnetohydrodynamic Waves and Instabilities

et al. 2021

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The importance of the chromosphere in the mass and energy transport within the solar atmosphere is now widely recognised. This review discusses the physics of magnetohydrodynamic (MHD) waves and instabilities in large-scale chromospheric structures as well as in magnetic flux tubes. We highlight a number of key observational aspects that have helped our understanding of the role of the solar chromosphere in various dynamic processes and wave phenomena, and the heating scenario of the solar chromosphere is also discussed. The review focuses on the physics of waves and invokes the basics of plasma instabilities in the context of this important layer of the solar atmosphere. Potential implications, future trends and outstanding questions are also delineated.

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“…Regarding prominence heating, in order to exist, prominences need mechanical equilibrium as well as a detailed energy balance between heating and radiative cooling. Energy balance studies suggest that incident radiation provides most of the heating of the prominence plasma (Gilbert, 2015); however, this radiative heating depends on the illumination from the surrounding atmosphere. Moreover, radiative-equilibrium prominence models, constructed from a balance between incident radiation and cooling (Anzer and Heinzel, 1999;Heinzel, Anzer, and Gunár, 2010;Heinzel and Anzer, 2012), as well as differential emission measures have pointed out that a further unknown heating is required in order to reproduce the observed temperatures in the prominence cores (Labrosse et al, 2010;Heinzel and Anzer, 2012;Heinzel, 2015) and to balance radiative losses (Parenti and Vial, 2007;Parenti, 2014;Soler et al, 2016;Melis, Soler, and Ballester, 2021).…”

Section: Introductionmentioning

confidence: 99%

The Effect of Thermal Misbalance on Slow Magnetoacoustic Waves in a Partially Ionized Prominence-Like Plasma

Ibanez¹,

Ballester²

2022

Sol Phys

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Solar prominences are partially ionized plasma structures embedded in the solar corona. Ground- and space-based observations have confirmed the presence of oscillatory motions in prominences, which have been interpreted in terms of standing or propagating MHD waves. Some of these observations suggest that slow magnetoacoustic waves could be responsible for these oscillations and have provided us with evidence about their damping/amplification with very small ratios between damping/amplifying times and periods, which have been difficult to explain from a theoretical point of view. Here we investigate the temporal behavior of non-adiabatic, slow, magnetoacoustic waves when a heating–cooling misbalance is present. The influence of optically thin losses and of a general heating term, in which density and temperature dependence can be modified, as well as the effect of partial ionization have been considered. Furthermore, a tentative example of how, using observational data, the observed ratio between damping/amplifying times and periods could be matched with those theoretically obtained is shown. In summary, different combinations of radiative losses, heating mechanisms, and typical wavenumbers, together with the effect of partial ionization, could provide a theoretical tool able to reproduce observational results on small-amplitude oscillations in prominences.

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Energy Balance

Cited by 13 publications

References 53 publications

Prominence observations with ALMA

Prominence observations with ALMA

Chromospheric Heating by Magnetohydrodynamic Waves and Instabilities

The Effect of Thermal Misbalance on Slow Magnetoacoustic Waves in a Partially Ionized Prominence-Like Plasma

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