Heating and Acceleration of Protons and Minor Ions by Fast Shocks in the Solar Corona

Lee, L. C.; Wu, B. H.

doi:10.1086/308879

Cited by 78 publications

(71 citation statements)

References 72 publications

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“…However, the observational data are also consistent with a polar region where the oxygen temperature across the magnetic field at maximum is 10-20 times larger than that along the field lines (Lee & Wu 2000;Vocks & Marsch 2002;Cranmer & van Ballegooijen 2003;Antonucci et al 2000Antonucci et al , 2004Hellinger et al 2005;Li & Habbal 2005).…”

Section: Introductionsupporting

confidence: 70%

“…An alternative theory to the dissipation of ion cyclotron resonant Alfvén waves was proposed by Lee & Wu (2000): the fast shock heating. A fast shock mechanism for heating the heavy ions is able to reproduce satisfactorily the observed outflow velocity of the oxygen component of the fast solar wind and the evolution of the ion temperature anisotropy.…”

Section: Discussionmentioning

confidence: 99%

“…Hybrid fluidkinetic models by Li & Habbal (2005) and Hellinger et al (2005), based on cyclotron resonant heating of the oxygen ions, predict that the decrease of the anisotropy ratio starts when the system crosses the threshold of the oxygen cyclotron instability generated by the temperature anisotropy itself and thus when the oxygen ion cyclotron resonance saturates. On the other hand, the model proposed by Lee & Wu (2000), based on a fast shock mechanism for heating the O +5 ions, predicts that in a low beta plasma filled by quasi-parallel subcritical shocks the reversal of the anisotropy ratio evolution takes place when the Alfvén speed crosses its maximum value and the heating perpendicular to the magnetic field hence becomes less efficient.…”

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Oxygen temperature anisotropy and solar wind heating above coronal holes out to 5R$_\odot$

Telloni¹,

Antonucci²,

Dodero

2007

A&A

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Section: Introductionsupporting

confidence: 70%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Oxygen temperature anisotropy and solar wind heating above coronal holes out to 5R$_\odot$

Telloni¹,

Antonucci²,

Dodero

2007

A&A

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“…Small-scale reconnection events and spicules also predict the generation of fast shock waves (Lee & Wu 2000;Lee 2001;Hollweg 1982), although we have concentrated on the role of the N-waves (slow shocks along the magnetic field line) excited by those events in this paper. The dissipation length of the fast shocks must be larger than that of N-waves with an identical period, since their phase speed is ev A , which is much larger than that of the N-waves ($c s ) for lowcoronal plasma.…”

Section: Summary and Discussionmentioning

confidence: 99%

On the Heating of the Solar Corona and the Acceleration of the Low‐Speed Solar Wind by Acoustic Waves Generated in the Corona

Suzuki¹

2002

ApJ

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We investigate possibilities of solar coronal heating by acoustic waves generated not in the photosphere but in the corona, focusing on heating in the mid-to low-latitude corona, where the low-speed wind is expected to come from. Acoustic waves of period $ 100 s are triggered by chromospheric reconnection, one model of small-scale magnetic reconnection events recently proposed by Sturrock. These waves, having a finite amplitude, eventually form shocks to shape sawtooth waves (N-waves) and directly heat the surrounding corona by dissipation of their wave energy. Outward propagation of the N-waves is treated based on weak-shock theory, so that the heating rate can be evaluated consistently with physical properties of the background coronal plasma without setting a dissipation length in an ad hoc manner. We construct coronal structures from the upper chromosphere to outside 1 AU for various acoustic wave inputs, with a range of energy flux of F w;0 ¼ ð1 20Þ Â 10 5 ergs cm À2 s À1 and a period of ¼ 60-300 s. The heating by the N-wave dissipation works effectively in the inner corona, and we find that waves of F w;0 ! 2 Â 10 5 ergs cm À2 s À1 and ! 60 s could maintain the peak coronal temperature, T max > 10 6 K. The model could also reproduce the density profile observed in the streamer region. However, due to its short dissipation length, the location of T max is closer to the surface than in observation, and the resulting flow velocity of the solar wind is lower than the observed profile of the low-speed wind. Cooperation with other heating and acceleration sources with larger dissipation lengths are inevitably needed to reproduce the real solar corona.

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“…Ion cyclotron heating has been considered as a possible explanation (e.g., Marsch et al 1982;Hollweg & Isenberg 2002), but many details are not clear. Another possibility is that the more effective heating of heavy ions is due to shock waves in the corona (Lee & Wu 2000;Zimbardo , 2011. Indeed, those models show that quasi-perpendicular shocks are able to heat heavy ions more than protons, and preferential heating of heavy ions is actually observed in the solar wind on occasion of interplanetary shock crossings (Zastenker & Borodkova 1984;Berdichevsky et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Preferential acceleration of heavy ions in the reconnection outflow region

Artemyev

Zimbardo

Ukhorskiy

et al. 2014

A&A

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Context. Many observations show that heating in the solar corona should be more effective for heavy ions than for protons. Moreover, the efficiency of particle heating also seems to be larger for a larger particle electric charge. The transient magnetic reconnection is one of the most natural mechanisms of charged particle acceleration in the solar corona. However, the role of this process in preferential acceleration of heavy ions has still yet to be investigated. Aims. In this paper, we consider charged particle acceleration in the reconnection outflow region. We investigate the dependence of efficiency of various mechanisms of particle acceleration on particle charge and mass. Methods. We take into account recent in situ spacecraft observations of the nonlinear magnetic waves that have originated in the magnetic reconnection. We use analytical estimates and test-particle trajectories to study resonant and nonresonant particle acceleration by these nonlinear waves. Results. We show that resonant acceleration of heavy ions by nonlinear magnetic waves in the reconnection outflow region is more effective for heavy ions and/or for ions with a larger electric charge. Nonresonant acceleration can be considered as a combination of particle reflections from the front of the nonlinear waves. Energy gain for a single reflection is proportional to the particle mass, while the maximum possible gain of energy corresponds to the classical betatron heating. Conclusions. Small-scale transient magnetic reconnections produce nonlinear magnetic waves propagating away from the reconnection region. These waves can effectively accelerate heavy ions in the solar corona via resonant and nonresonnat regimes of interactions. This mechanism of acceleration is more effective for ions with a larger mass and/or with a larger electric charge.

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Heating and Acceleration of Protons and Minor Ions by Fast Shocks in the Solar Corona

Cited by 78 publications

References 72 publications

Oxygen temperature anisotropy and solar wind heating above coronal holes out to 5R$_\odot$

Oxygen temperature anisotropy and solar wind heating above coronal holes out to 5R$_\odot$

On the Heating of the Solar Corona and the Acceleration of the Low‐Speed Solar Wind by Acoustic Waves Generated in the Corona

Preferential acceleration of heavy ions in the reconnection outflow region

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