Alfvénic waves with sufficient energy to power the quiet solar corona and fast solar wind

McIntosh, Scott W.; Pontieu, Bart De; Carlsson, Mats; Hansteen, V. H.; Boerner, P.; Goossens, Marcel

doi:10.1038/nature10235

Cited by 537 publications

(530 citation statements)

References 21 publications

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“…This process transmitting energy from the (convectively active) PNS to the much less dense surrounding medium bears a strong similarity to the proposed mechanism for heating the solar corona by Alfvén waves emerging from the solar surface (e.g. McIntosh et al 2011). …”

Section: Introductionmentioning

confidence: 88%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

101

117

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We study the amplification of magnetic fields in the collapse and the post-bounce evolution of the core of a non-rotating star of 15 M in axisymmetry. To this end, we solve the coupled equations of magnetohydrodynamics and neutrino transport in the two-moment approximation. The pre-collapse magnetic field is strongly amplified by compression in the infall. Initial fields of the order of 10 10 G translate into proto-neutron star fields similar to the ones observed in pulsars, while stronger initial fields yield magnetar-like final field strengths. After core bounce, the field is advected through the hydrodynamically unstable neutrino-heating layer, where non-radial flows due to convection and the standing accretion shock instability amplify the field further. Consequently, the resulting amplification factor of order five is the result of the number of small-eddy turnovers taking place within the time scale of advection through the post-shock layer. Due to this limit, most of our models do not reach equipartition between kinetic and magnetic energy and, consequently, evolve similarly to the non-magnetic case, exploding after about 800 ms when a single or few highentropy bubbles persist over several dynamical time scales. In the model with the strongest initial field we studied, 10 12 G, for which equipartition between flow and field is achieved, the magnetic tension favours a much earlier development of such long-lived high-entropy bubbles and enforces a fairly ordered large-scale flow pattern. Consequently, this model, after exhibiting very regular shock oscillations, explodes much earlier than non-magnetic ones.

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Section: Introductionmentioning

confidence: 88%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

101

117

View full text Add to dashboard Cite

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“…In conclusion, it looks unlikely that blowouts can significantly contribute to the wind. Still, this estimate may change, if type II spicules were proved to accompany blowouts: it is well known (see, e.g., McIntosh et al, 2011) that the type II spicular mass flux can easily balance the wind mass loss. Here we are on a still unknown territory.…”

Section: Do Plumes Contribute To Solar Wind?mentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL) images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV) and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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“…Throughout the last decade, a number of authors, including Walsh and Ireland (2003), Aschwanden (2005), McIntosh et al (2011), Wedemeyer-Böhm et al (2012, Winebarger et al (2013), demonstrated that one of the several mechanisms, involving small-scale X-ray jets, bright points, micro-and nanoflares as well as Alfvén and MHD turbulence and waves, are able to provide partial explanations for the extreme heating of coronal plasma. Mass and energytransport between the lower atmosphere (photosphere and chromosphere) and the outer atmosphere (corona) is, in general, a challenging concern.…”

Section: Role Of Magnetic Fields In Coronal and Chromospheric Heatingmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

172

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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Alfvénic waves with sufficient energy to power the quiet solar corona and fast solar wind

Cited by 537 publications

References 21 publications

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Solar Coronal Plumes

The magnetic field in the solar atmosphere

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