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1 Jul, 2008 :
HOPs are being accepted once again, since we have developed sufficient
confidence in operating the spacecraft and the three instruments in this
new slower, data-downlink mode. Hinode data are now transmitted
through a back-up transmitter that has a considerably lower
transmission rate. To compensate for the lower rate we
have, over the last four months, increased the level of data compression
without significantly affecting the quality of the data and improved our
operational efficiency. For more details, see the
data and data policy page.
1 Mar, 2008 :
The Hinode Solar Observatory is currently experiencing technical difficulties that have resulted in a reduction in the rate at which scientific data can be transmitted to the ground from the on-board recorder. One of the near term impacts is the ability to accommodate observations by non-team members through the HOP (Hinode Operation Plan) process. Consequently we have imposed a one month moratorium on all HOPs that will extend through March 31, 2008. For more details, see our data page.
30 Nov, 2007 :
Research using Hinode data by NASA/MSFC's Dr. Jonathan Cirtain (and others) will be featured in the Dec 7 issue of Science. See the special issue.
5 Nov, 2007 :
Data from the Solar Optical Telescope on Hinode is freely available to the community following the mission's open data policy. Many scientists have begun to analyze photospheric and chromospheric observations of unprecedented quality from SOT's Broadband Filter Imager and Spectro-Polarimeter. Recently a larger variety of data has become available from the third instrument channel, the Narrowband Filter Imager (NFI). The NFI has observed in all of its spectral bands and collected filtergrams, longitudinal magnetograms, Dopplergrams and Stokes IQUV images at various wavelengths. Several Fe I lines formed in the photosphere, Na D1 and Mg b2 in the low chromosphere, and H-alpha are all being observed. Na D1 is the default line for longitudinal magnetic and Doppler observations, due to its higher light level and more robust prefilter. The Solarsoft routine fg_prep is being updated to handle the additional observation types.
Specific questions about NFI images and their processing may be sent to:
sot_nfi (at) lmsal (dot) com.
More information about the SOT can be found at either of:
Data is available from the following:
Requests for observations should follow the procedure described at:
Hinode Observation Proposals.
(This news from Hinode/SOT Narrow Band Filter Imager by T. Tarbell in Solar News)
30 Aug, 2007
:
The XRT CCD has experienced some degradation due to contamination
that appeared after a short CCD bake-out in July. The contamination
is manifest by small (~5 pixel diameter) spots on the detector.
The spots cover somewhat less than 4% of the CCD area.They are seen
in G-band images and in the thinner x-ray filters (Al_mesh, Al_poly,
Ti_poly, C_poly and Be_thin, with decreasing effect in the order listed).
The origin of the contamination is not understood at this time.
For more details, see the data page or the XRT data-users' email list
29 Aug, 2007
:
AGU Special Session SH11:Coronal Jets, X-ray Bright Points and the Fast Solar Wind
Recent observations of the solar corona have revealed that x-ray jets occur with far more frequency than previously reported. These jets eminate from multi-polar x-ray bright points, with not all bright points producing jets. To discuss the status of the studies using these observations, the American Geophysical Union Fall meeting will feature a special session that highlights observations from both Hinode and STEREO. For more information, visit the AGU Session Page.
27 May, 2007
:
All Hinode data have now been released. See the Data Policy page for more details.
14 March, 2007
:
A NASA Science Update at 1 p.m. EDT Wednesday, March 21 will be held to discuss never-before-seen observations from an international mission studying the sun.
Learn More
9 February, 2007
:
Hinode data will be released for the first time, at the Solar Physics Division Meeting to be held in
Hawaii, May 27-31. A workshop will follow immediately to explain how data
are to be accessed and analyzed.
10-15 December, 2006
:
Images recorded during the engineering phase and a preliminary
discussion of the results will be presented at the fall meeting of the
American Geophysical Union in San Francisco, California.
4-10 December, 2006
:
NOAA active region 10926 has been tracked until 5 December. As AR 10930 appeared on the east limb (a re-appearance of AR 10923), it emitted an X9.0 flare (the 15th largest GOES flare since 1976) at 10:18 UT. Hinode has been redirected to track this Active Region.
27 November, 2006
:
A Press Conference was held in Japan. For the full story, see Hinode Initial Results.
20-24 November, 2006
:
Hinode continues to track NOAA active region 10923 to the Sun's west limb.
After west limb passage of AR 10923, Hinode is observing quiet Sun and
the northern polar
region.
16 November, 2006
:
UK scientists are invited to propose observations with Hinode's EUV Imaging
Spectrometer (EIS). For more information click here
10 November, 2006
:
Spacecraft pointing was adjusted to observe
NOAA active region 10923.
7 November, 2006
:
All instruments continue to study NOAA active region number 10921. The spacecraft was pointed to the limb as a test for the observation of the transit of Mercury on November 8 (for observation information in your local area, see Science at NASA). High resolution movies of spicules are being made in the light of Ca II.
1-3 November, 2006
:
The image stabilization system of the Solar Optical Telescope has been tested and the tracking stability is better than 0.01" rms. From now on, the SOT will be operated with the image stablization system engaged. Line-of-sight magnetic field data using the Narrow-band Filter Imager have been obtained, yielding a time series of magnetograms. These data reveal the evolution of magnetic elements everywhere in the quiet Sun. The tentative target for 4 November, is the active region NOAA 10921.
30 October, 2006
:
Data from all three instruments are being evaluated. From the spectra obtained with the EIS in the 17 nm - 21 nm and 25 nm - 39 nm wavelength ranges, hot iron lines are detected, even in the quiet Sun. The EIS is performing as expected, with high spectral resolution and sensitivity. The signal to noise ratio of the spectral polarimeter (SP) of the SOT has been confirmed at 0.1% and fluctuation of the SOT image is 0.01", allowing for high accuracy magnetic field measurements.
28 October, 2006
:
The rear door of the EIS was opened and the instrument successfully obtained fine Extreme UltraViolet spectra using the narrow 1" slit and an overlappogram using the 266" wide slot. The EIS is functioning normally.
27 October, 2006
:
The front door of Extreme Ultra-Violet Imaging Spectrometer (EIS) has been opened successfully. One of the two doors which protected the prefilter of the EIS during the launch was opened. The other door of the EIS is tentatively expected to be opened on 28 October.
26 October, 2006
:
The SOT continues to perform well. The four optical systems, the broadband filter imager, the narrowband filter imager, the spectropolarimeter, and the correlation tracker are working. An engineering image in the Na I D line, shows granule patterns well. A one-hour movie in the G-band, has been downlinked to the European Space Agency's Svalvard Station in Norway, but has not yet arrived at the Sagamihara Operation Center in Japan.
25 October, 2006
:
The SOT captured its first image! The top door was opened at about 17:00 JST and the telescope almost immediately began taking high-quality engineering test images in several wavelengths, using the broadband filter imager. See the STATUS page for more details.
24 October, 2006
:
XRT took a good-quality, visible-light image. The SOT is ready for the opening of its top door (tentatively scheduled for 25 October) and an observation table has been
uploaded.
23 October, 2006
:
The Solar Optical Telescope (SOT) is doing fine and "dark" images are being taken. The Extreme Ultraviolet Imaging Spectrometer (EIS) is being tested with an internal LED light source and the CCDs show good response. The XRT is successfully taking engineering test images and has obtained a good-quality, X-ray image.
16 October, 2006
:
Major elements of the spacecraft checkout have been completed, including the "safe-hold" tests. Japan has not reported any significant issues or concerns with any of the spacecraft subsystems. Subsequently, the Mission Data Processor was turned on last Thursday and the instruments powered on shortly thereafter.
EIS has been turned on successfully. The SOT has begun its initialization processes. The OTA side-door (which dumps extra heat from the telescope) has been deployed. The XRT has been powered on and the XRT door is open. Later this week, a series of "through focus" images will be made.
13 October, 2006
:
The X-Ray Telescope (XRT) was successfully turned on early this
morning (approximately 3:57 am EDT).
All of the sensors (temperature, voltage, currents) are in the
"green". Switches are in expected positions and
all equipment is operating as expected.
Based on the success to date, "first light" has been
scheduled for October 19.
22 September, 2006
:
LAUNCH occurred at 21:36 UT. For a replay of the launch, click HERE for RealVideo or HERE for Windows Media. (Video courtesy of JAXA -- download time may be a minute or two.)
19 September, 2006
:
Beginning at 9:32 UT, a rehearsal of launch operations will commence. This rehearsal will include functional tests of the satellite and data flow tests.
1 August, 2006
:
On July 30, the Solar-B spacecraft left ISAS' building C in Sagamihara and arrived at the
Uchinoura Space Center in the early morning of August 1. Throughout August, the spacecraft
will undergo post-shipment checks and
tests of launch-site/spacecraft systems and operations.
July 26, 2006
NAOJ Solar-B Homepage:
Under approval of the Space Activity Commission, JAXA announced the official
Solar-B launch schedule at 16:00 JST. Solar-B is scheduled for launch
on 2006 September 23, 06:00-07:00 JST (September 22, 21:00-22:00 UT)
on a M-V-7 rocket.
A backup launch window extends from September 24-30.
June 25-30, 2006
Solar Physics Division of the AAS 2006 Meeting:
The Solar Physics Division of the American Astronomical Society held its 37th meeting on the campus of
the University of New Hampshire in Durham. Topics of discussion included the solar wind and heliosphere, the active corona, coronal magnetic fields, the chromosphere, solar eruptions and conditions, the solar interior, the magnetic photosphere, and a special session on Solar-B. The special session included:
an Overview of the Solar-B Mission by Dr. John Davis, a discussion of The Focal Plane Package of the Solar Optical Telescope on Solar-B by Dr. Theodore Tarbell,
a description of The X-ray Telescope for Solar-B by Dr. Edward DeLuca,
and a survey of
The Extreme Ultraviolet Imaging Spectrometer (EIS) on Solar-B
by George A. Doschek.
November 15, 2005 Solar-B/STEREO Science Planning Workshop: This meeting was focused on science planning for the STEREO and Solar-B missions, which will both be launched in 2006. The purpose of the conference was to discuss the possibility of complementary science operations and data analysis and interpretation activities in order to maximize the science outputs from these missions. Discussion on how to make mutually productive partnerships, both with coexisting solar and heliospheric missions including SOHO, ACE, WIND, and Ulysses, with ground based solar observatories, especially those including magnetographs, and with overlapping activities and campaigns such as VSO, VHO and IHY, will also be a primary goal.
(Turtle Bay, Oahu, Hawaii)
November 8-11, 2005 Sixth Solar-B Science Meeting:
The sixth Solar-B science meeting was organized by Kwasan and Hida Observatories of Kyoto University
and sponsored by a Grant-in-Aid for the 21st Century COE "Center for Diversity and Universality in Physics",
Yukawa Institute for Theoretical Physics of Kyoto University, and Solar Terrestrial Environment Laboratory
of Nagoya University. The main objective of the meeting was to discuss science objectives and programs to
sponsor observing programs. (Kyoto, Japan)
December 14, 2001: Yohkoh (Solar-A) suffered a spacecraft failure that put an end to this mission. During the solar eclipse of December 14th the spacecraft lost pointing. Since the spacecraft operators were unable to command the satellite to point toward the sun, the batteries discharged.
April 3, 2001 Beyond Solar-B, The Marshall Space Flight Center Solar Physics Symposium: The MSFC solar physics group was active in the definition and promotion of the Japan/US/UK Solar-B Mission. Now that Solar-B is "under construction" it is time to begin to think about the science problems that the next high-resolution magnetography mission should address. The Huntsville solar group, with the encouragement of NASA Headquarters, undertook the initiative to organize a Workshop that brought together solar scientists who represent this segment of the solar physics community. Our chief aim was to reach consensus on the main science goals for space-based high-resolution solar magnetography beyond 2010. This process was begun by NASA's Sun-Earth Connection Roadmap exercise last year, but much more needs to be done. The topic needed to be revisited in light of NASA's new initiative, Living With a Star (LWS), and in light of the Advanced Technology Solar Telescope (ATST) being spearheaded by NSO.
The title of the Workshop was
High-Resolution Solar Magnetography from Space: Beyond Solar-B." The focus was on the interplay between solar convection and the magnetic field in and near the photosphere. The basic purpose was to identify (1) the science problems that will likely remain unsolved at the end of the decade, and (2) the improvements in high-resolution measurements of magnetic fields and magnetoconvection that are needed to open inroads into these problems. The purpose of the Workshop was not to define the next
high-resolution solar magnetography mission, but rather to define the scientific questions that such a mission will have to address.
Thus the outcome of the Workshop lays the foundation for the mission study,
which will come later.
MORE ITEMS August 30, 1991 - January 20, 2001
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