On the parallel and perpendicular propagating motions visible in polar plumes: an incubator for (fast) solar wind acceleration?

Jiajia Liu; Scott W. McIntosh; Ineke De Moortel; Yuming Wang

doi:10.1088/0004-637X/806/2/273

On the parallel and perpendicular propagating motions visible in polar plumes: an incubator for (fast) solar wind acceleration?

Jiajia Liu^*, Scott W. McIntosh, Ineke De Moortel, Yuming Wang

^*Corresponding author for this work

Applied Mathematics

Research output: Contribution to journal › Article › peer-review

Abstract

We combine observations of the Coronal Multi-channel Polarimeter and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km s(-1) (in both the 171 and 193 angstrom passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km s(-1), a phase speed of 830 km s(-1), and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic turbulence required to accelerate the fast solar wind.

Original language	English
Article number	273
Number of pages	7
Journal	Astrophysical Journal
Volume	806
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/806/2/273
Publication status	Published - 20 Jun 2015

Keywords

Sun: corona
Waves
Coronal loops
Alfven waves
Turbulance-driven
Energy content
Chromosphere
Holes
Macrospicules
Oscillations
Seismology
Region

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10.1088/0004-637X/806/2/273

Moortel_2015_TAJ_Parallel
© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/0004-637X/806/2/273
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Plasma Theory: Solar and Magnetospheric Plasma Theory
Hood, A. W. (PI), Mackay, D. H. (CoI), Neukirch, T. (CoI), Parnell, C. E. (CoI), Priest, E. (CoI), Archontis, V. (Researcher), Cargill, P. (Researcher), De Moortel, I. (Researcher) & Wright, A. N. (Researcher)
Science & Technology Facilities Council
1/04/13 → 31/03/16
Project: Standard
EU FP7 Marie Curie IRSES SOLSPANET: EU FP7 Marie Curie IRSES SOLSPANET
De Moortel, I. (PI) & Hood, A. W. (CoI)
European Commission
1/09/11 → 31/08/17
Project: Standard

Cite this

@article{a2809f745cc3447db90d8326a7fc1f77,

title = "On the parallel and perpendicular propagating motions visible in polar plumes: an incubator for (fast) solar wind acceleration?",

abstract = "We combine observations of the Coronal Multi-channel Polarimeter and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km s(-1) (in both the 171 and 193 angstrom passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km s(-1), a phase speed of 830 km s(-1), and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic turbulence required to accelerate the fast solar wind.",

keywords = "Sun: corona, Waves, Coronal loops, Alfven waves, Turbulance-driven, Energy content, Chromosphere, Holes, Macrospicules, Oscillations, Seismology, Region",

author = "Jiajia Liu and McIntosh, {Scott W.} and {De Moortel}, Ineke and Yuming Wang",

note = "J.L. was a student visitor at HAO. J.L. acknowledges the financial support for his visit to HAO from the Chinese Scholarship Council (CSC). The authors acknowledge support from NSFC 41131065, 41121003, 973 Key Project 2011CB811403, and CAS Key Research Program KZZD-EW-01-4. We also acknowledge support from NASA contracts NNX08BA99G, NNX11AN98G, NNM12AB40P, NNG09FA40C (IRIS), and NNM07AA01C (Hinode). The research leading to these results has also received funding from the European Commission Seventh Framework Programme (FP7/ 2007-2013) under the grant agreement SOLSPANET (project No. 269299, www.solspanet.eu/solspanet) Date of Acceptance: 25/05/2015",

year = "2015",

month = jun,

day = "20",

doi = "10.1088/0004-637X/806/2/273",

language = "English",

volume = "806",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

TY - JOUR

T1 - On the parallel and perpendicular propagating motions visible in polar plumes

T2 - an incubator for (fast) solar wind acceleration?

AU - Liu, Jiajia

AU - McIntosh, Scott W.

AU - De Moortel, Ineke

AU - Wang, Yuming

N1 - J.L. was a student visitor at HAO. J.L. acknowledges the financial support for his visit to HAO from the Chinese Scholarship Council (CSC). The authors acknowledge support from NSFC 41131065, 41121003, 973 Key Project 2011CB811403, and CAS Key Research Program KZZD-EW-01-4. We also acknowledge support from NASA contracts NNX08BA99G, NNX11AN98G, NNM12AB40P, NNG09FA40C (IRIS), and NNM07AA01C (Hinode). The research leading to these results has also received funding from the European Commission Seventh Framework Programme (FP7/ 2007-2013) under the grant agreement SOLSPANET (project No. 269299, www.solspanet.eu/solspanet) Date of Acceptance: 25/05/2015

PY - 2015/6/20

Y1 - 2015/6/20

N2 - We combine observations of the Coronal Multi-channel Polarimeter and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km s(-1) (in both the 171 and 193 angstrom passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km s(-1), a phase speed of 830 km s(-1), and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic turbulence required to accelerate the fast solar wind.

AB - We combine observations of the Coronal Multi-channel Polarimeter and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km s(-1) (in both the 171 and 193 angstrom passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km s(-1), a phase speed of 830 km s(-1), and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic turbulence required to accelerate the fast solar wind.

KW - Sun: corona

KW - Waves

KW - Coronal loops

KW - Alfven waves

KW - Turbulance-driven

KW - Energy content

KW - Chromosphere

KW - Holes

KW - Macrospicules

KW - Oscillations

KW - Seismology

KW - Region

U2 - 10.1088/0004-637X/806/2/273

DO - 10.1088/0004-637X/806/2/273

M3 - Article

SN - 0004-637X

VL - 806

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 273

ER -

On the parallel and perpendicular propagating motions visible in polar plumes: an incubator for (fast) solar wind acceleration?

Abstract

Keywords

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Projects

Plasma Theory: Solar and Magnetospheric Plasma Theory

EU FP7 Marie Curie IRSES SOLSPANET: EU FP7 Marie Curie IRSES SOLSPANET

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