Science Objective: Understanding Energy Transport by Alfvénic Waves in Solar Flares

Jeffrey W. Reep, Harry P. Warren, James E. Leake, Lucas A. Tarr, Alexander J. B. Russell, Graham S. Kerr, Hugh S. Hudson

Research output: Other contribution

Abstract

Solar flares are driven by the release of magnetic energy from reconnection events in the solar corona, whereafter energy is transported to the chromosphere, heating the plasma and causing the characteristic radiative losses. In the collisional thick-target model, electrons accelerated to energies exceeding 10 keV traverse the corona and impact the chromosphere, where they deposit their energy through collisions with the much denser plasma in the lower atmosphere. While there are undoubtedly high energy non-thermal electrons accelerated in flares, it is unclear whether these electron beams are the sole mechanism of energy transport, or whether they only dominate in certain phases of the flare's evolution. Alfv\'enic waves are generated during the post-reconnection relaxation of magnetic field lines, so it is important to examine their role in energy transport.
Original languageEnglish
TypeNext Generation Solar Physics Mission White Paper
PublisherCornell University
Number of pages4
Publication statusPublished - 6 Feb 2017

Fingerprint

solar flares
chromosphere
energy
flares
lower atmosphere
solar corona
dense plasmas
coronas
electrons
deposits
electron beams
heating
collisions
magnetic fields

Keywords

  • astro-ph.SR

Cite this

Reep, J. W., Warren, H. P., Leake, J. E., Tarr, L. A., Russell, A. J. B., Kerr, G. S., & Hudson, H. S. (2017, Feb 6). Science Objective: Understanding Energy Transport by Alfvénic Waves in Solar Flares. Cornell University.
Reep, Jeffrey W. ; Warren, Harry P. ; Leake, James E. ; Tarr, Lucas A. ; Russell, Alexander J. B. ; Kerr, Graham S. ; Hudson, Hugh S. . / Science Objective : Understanding Energy Transport by Alfvénic Waves in Solar Flares. 2017. Cornell University. 4 p.
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abstract = "Solar flares are driven by the release of magnetic energy from reconnection events in the solar corona, whereafter energy is transported to the chromosphere, heating the plasma and causing the characteristic radiative losses. In the collisional thick-target model, electrons accelerated to energies exceeding 10 keV traverse the corona and impact the chromosphere, where they deposit their energy through collisions with the much denser plasma in the lower atmosphere. While there are undoubtedly high energy non-thermal electrons accelerated in flares, it is unclear whether these electron beams are the sole mechanism of energy transport, or whether they only dominate in certain phases of the flare's evolution. Alfv\'enic waves are generated during the post-reconnection relaxation of magnetic field lines, so it is important to examine their role in energy transport.",
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author = "Reep, {Jeffrey W.} and Warren, {Harry P.} and Leake, {James E.} and Tarr, {Lucas A.} and Russell, {Alexander J. B.} and Kerr, {Graham S.} and Hudson, {Hugh S.}",
note = "Next Generation Solar Physics Mission White paper, 4 pages, 2 figures",
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Reep, JW, Warren, HP, Leake, JE, Tarr, LA, Russell, AJB, Kerr, GS & Hudson, HS 2017, Science Objective: Understanding Energy Transport by Alfvénic Waves in Solar Flares. Cornell University.

Science Objective : Understanding Energy Transport by Alfvénic Waves in Solar Flares. / Reep, Jeffrey W.; Warren, Harry P.; Leake, James E.; Tarr, Lucas A.; Russell, Alexander J. B.; Kerr, Graham S.; Hudson, Hugh S. .

4 p. Cornell University. 2017, Next Generation Solar Physics Mission White Paper.

Research output: Other contribution

TY - GEN

T1 - Science Objective

T2 - Understanding Energy Transport by Alfvénic Waves in Solar Flares

AU - Reep, Jeffrey W.

AU - Warren, Harry P.

AU - Leake, James E.

AU - Tarr, Lucas A.

AU - Russell, Alexander J. B.

AU - Kerr, Graham S.

AU - Hudson, Hugh S.

N1 - Next Generation Solar Physics Mission White paper, 4 pages, 2 figures

PY - 2017/2/6

Y1 - 2017/2/6

N2 - Solar flares are driven by the release of magnetic energy from reconnection events in the solar corona, whereafter energy is transported to the chromosphere, heating the plasma and causing the characteristic radiative losses. In the collisional thick-target model, electrons accelerated to energies exceeding 10 keV traverse the corona and impact the chromosphere, where they deposit their energy through collisions with the much denser plasma in the lower atmosphere. While there are undoubtedly high energy non-thermal electrons accelerated in flares, it is unclear whether these electron beams are the sole mechanism of energy transport, or whether they only dominate in certain phases of the flare's evolution. Alfv\'enic waves are generated during the post-reconnection relaxation of magnetic field lines, so it is important to examine their role in energy transport.

AB - Solar flares are driven by the release of magnetic energy from reconnection events in the solar corona, whereafter energy is transported to the chromosphere, heating the plasma and causing the characteristic radiative losses. In the collisional thick-target model, electrons accelerated to energies exceeding 10 keV traverse the corona and impact the chromosphere, where they deposit their energy through collisions with the much denser plasma in the lower atmosphere. While there are undoubtedly high energy non-thermal electrons accelerated in flares, it is unclear whether these electron beams are the sole mechanism of energy transport, or whether they only dominate in certain phases of the flare's evolution. Alfv\'enic waves are generated during the post-reconnection relaxation of magnetic field lines, so it is important to examine their role in energy transport.

KW - astro-ph.SR

M3 - Other contribution

PB - Cornell University

ER -

Reep JW, Warren HP, Leake JE, Tarr LA, Russell AJB, Kerr GS et al. Science Objective: Understanding Energy Transport by Alfvénic Waves in Solar Flares. 2017. 4 p.