Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence

T. J. Okamoto; S. Tsuneta; T. E. Berger; K. Ichimoto; Y. Katsukawa; B. W. Lites; S. Nagata; K. Shibata; T. Shimizu; R. A. Shine; Y. Suematsu; T. D. Tarbell; A. M. Title

doi:10.1126/science.1145447

Special Reports

Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence

T. J. Okamoto1,2,*,
S. Tsuneta1,
T. E. Berger3,
K. Ichimoto1,
Y. Katsukawa1,
B. W. Lites4,
S. Nagata2,
K. Shibata2,
T. Shimizu5,
R. A. Shine3,
Y. Suematsu1,
T. D. Tarbell3,
A. M. Title3

¹ National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan.
² Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan.
³ Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304, USA.
⁴ High Altitude Observatory, National Center for Atmospheric Research, Post Office Box 3000, Boulder CO 80307–3000, USA.
⁵ Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Kanagawa 229-8510, Japan.

↵* To whom correspondence should be addressed. E-mail: joten.okamoto{at}nao.ac.jp

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Science 07 Dec 2007:
Vol. 318, Issue 5856, pp. 1577-1580
DOI: 10.1126/science.1145447

T. J. Okamoto

National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan.

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S. Tsuneta

National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan.

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T. E. Berger

Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304, USA.

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K. Ichimoto

National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan.

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Y. Katsukawa

National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan.

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B. W. Lites

High Altitude Observatory, National Center for Atmospheric Research, Post Office Box 3000, Boulder CO 80307–3000, USA.

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S. Nagata

Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan.

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K. Shibata

Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan.

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T. Shimizu

Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Kanagawa 229-8510, Japan.

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R. A. Shine

Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304, USA.

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Y. Suematsu

National Astronomical Observatory (NAOJ), Mitaka, Tokyo 181-8588, Japan.

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T. D. Tarbell

Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304, USA.

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A. M. Title

Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover Street, Palo Alto, CA 94304, USA.

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Abstract

Solar prominences are cool 10⁴ kelvin plasma clouds supported in the surrounding 10⁶ kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role in heating the corona.

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Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence

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