Hinode Featured in Science
2007 December 7
National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NAOJ/NINS)
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA)
National Aeronautics and Space Administration (NASA)
Science and Technology Facilities Council (STFC)
European Space Agency (ESA)
Hinode (SOLAR-B) has brought us a new perspective
of solar physics since its launch on September 22, 2006.
Sience magazine, one of the leading journals of
scientific research, features Hinode discoveries.
An impressive picture obtained with Hinode appears in
the front page of the journal.
This press release highlights two of nine articles published
in the special issue.
- Continuous Plasma Outflows from the Edge of a Solar Active Region as a Possible Source of Solar Wind
T. Sakao1, R. Kano2, N. Narukage,1,
J. Kotoku2, T. Bando2, E. E. DeLuca3
L. L. Lundquist3, S. Tsuneta2, L. K. Harra4,
Y. Katsukawa2, M. Kubo5, H. Hara2,
K. Matsuzaki1, M. Shimojo2, J. A. Bookbinder3
L. Golub3, K. E. Korreck3, Y. Su3,
K. Shibasaki2, T. Shimizu1, and I. Nakatani1
1Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA)
2National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NAOJ/NINS)
3Harvard-Smithsonian Center for Astrophysics
4Mullard Space Science Laboratory (MSSL)
5High Altitude Observatory, The National Center for Atmospheric Research (HAO/NCAR)
Figure 1 presents an active region corona adjacent to an equatorial
coronal hole observed
The sequence of images display continuous plasma outflow from
the edge of the active region (white curcle in Fig. 1).
Apparent velocity of the outflow is 140 km/s.
Magnetic field extrapolartion from full disk magnetogram suggests
that roots of the open magnetic field are co-spatial with
the plasma outflow region.
Hinode allowed us to identify the source region of the low
speed solar wind for the first time.
This discovery will contribute to the study of solar wind which
affects terrestrial environment.
Figure 1. The corona of active region adjacent to a coronal hole, seen
A circle in the bottom indicates the size of the Earth.
- Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence
T. Okamoto1, S. Tsuneta1, T. E. Berger2,
K. Ichimoto1, Y. Katsukawa1,B. W. Lites3,
S. Nagata4, K. Shibata4, T. Shimizu5,
R. A. Shine2, Y. Suematsu1, T. D. Tarbell2,
and A. M. Title2
1National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NAOJ/NINS)
2Lockheed Martin Solar and Astrophysics Laboratory (LMSAL)
3High Altitude Observatory, The National Center for Atmospheric Research (HAO/NCAR)
4Kwasan and Hida Observatories, Kyoto University
5Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA)
Figure 2 displays a limb prominence above an active region observed
Prominences are floating cool plasma in the hot corona.
High resolution images in Ca II H spectral line revealed
waving motion of the prominence.
Detailed analysis proved that the motion is attributed to
Alfvén wave in the corona.
This observational result holds vital clues
for understanding the coronal heating.
Figure 2. Alfvén wave in the active region
prominence observed by SOT/Hinode.
A circle in the left indicates the size of the Earth.
Contact: press (at) solar-b.nao.ac.jp