The effect of plume/interplume lanes on ion-cyclotron resonance heating

AbstractThe effect of the Plume/Interplume Lane (PIPL) structure of the solar North Polar Coronal Hole (NPCH) on the ion-cyclotron resonance (ICR) process is investigated. The ICR process in the interplume lanes is much more effective than in the plumes, agreeing with the observations which show the source of fast solar wind is interplume lanes.

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Ion–Cyclotron Resonance Frequency Interval Dependence on the O VI Ion Number Density in the North Polar Coronal Hole 1.5R–3R Region

Journal of Astrophysics and Astronomy ◽

10.1007/s12036-013-9187-3 ◽

2013 ◽

Vol 34 (4) ◽

pp. 349-355

Author(s):

Özgür Gültekin ◽

Emine Rızaoǧlu ◽

K. Gediz Akdeniz

Keyword(s):

Resonance Frequency ◽

Coronal Hole ◽

Cyclotron Resonance ◽

Polar Coronal Hole ◽

Ion Cyclotron Resonance ◽

Frequency Interval ◽

Number Density ◽

The North ◽

Ion Cyclotron ◽

North Polar

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EVIDENCE OF THE ION CYCLOTRON RESONANCE AT PROTON KINETIC SCALES IN THE SOLAR WIND

The Astrophysical Journal ◽

10.1088/0004-637x/802/1/1 ◽

2015 ◽

Vol 802 (1) ◽

pp. 1 ◽

Cited By ~ 25

Author(s):

O. W. Roberts ◽

Xing Li

Keyword(s):

Solar Wind ◽

Cyclotron Resonance ◽

Ion Cyclotron Resonance ◽

Ion Cyclotron

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Spectroscopic Constraints on Models of Ion Cyclotron Resonance Heating in the Polar Solar Corona and High‐Speed Solar Wind

The Astrophysical Journal ◽

10.1086/307330 ◽

1999 ◽

Vol 518 (2) ◽

pp. 937-947 ◽

Cited By ~ 207

Author(s):

Steven R. Cranmer ◽

George B. Field ◽

John L. Kohl

Keyword(s):

Solar Wind ◽

Solar Corona ◽

Cyclotron Resonance ◽

High Speed ◽

Ion Cyclotron Resonance ◽

Ion Cyclotron ◽

Speed Solar Wind ◽

High Speed Solar Wind

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OBSERVATIONAL QUANTIFICATION OF THE ENERGY DISSIPATED BY ALFVÉN WAVES IN A POLAR CORONAL HOLE: EVIDENCE THAT WAVES DRIVE THE FAST SOLAR WIND

The Astrophysical Journal ◽

10.1088/0004-637x/776/2/78 ◽

2013 ◽

Vol 776 (2) ◽

pp. 78 ◽

Cited By ~ 36

Author(s):

M. Hahn ◽

D. W. Savin

Keyword(s):

Solar Wind ◽

Coronal Hole ◽

Alfven Waves ◽

Polar Coronal Hole ◽

Alfvén Waves ◽

Fast Solar Wind ◽

Energy Dissipated

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Drivers of the solar wind: then and now

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2005.1713 ◽

2005 ◽

Vol 364 (1839) ◽

pp. 505-527 ◽

Cited By ~ 24

Author(s):

Joseph V Hollweg

Keyword(s):

Solar Wind ◽

Pressure Gradient ◽

Cyclotron Resonance ◽

Coronal Holes ◽

Ion Cyclotron Resonance ◽

The Sun ◽

Principal Mechanism ◽

Fast Wind ◽

Ion Cyclotron ◽

Spacecraft Data

Early spacecraft data in the 1960s revealed solar wind properties, which could not be well explained by models in which the electron pressure gradient was the principal accelerating force. The Alfvén waves discovered around 1970 were thought for a while to provide additional energy and momentum, but they ultimately failed to explain the rapid acceleration of the fast wind close to the Sun. By the late 1970s, various data were suggesting the importance of the ion-cyclotron resonance far from the Sun. This notion was soon applied to the acceleration region close to the Sun. The models, which resulted, suggested that the fast wind could be driven mainly by the proton pressure gradient. Since the mid-1990s, Solar and Heliospheric Observatory has provided remarkable data, which have verified some of the predictions of these theories, and given impetus to studies of the ion-cyclotron resonance as the principal mechanism for heating the coronal holes, and ultimately driving the fast wind. After a historical review, we discuss the basic ideas behind current research, emphasizing the particle kinetics. We discuss remaining problems, especially the source of the ion-cyclotron resonant waves.

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