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GYŐRI, L.: 2003, Compiling sunspot catalogue: the principles, Proc. SIRW Meeting, (Oct. 23-24, 2003, Royal Observatory of Belgium), CD-ROM,
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Publ. Debrecen Obs. Heliogr. Ser.: The volumes of DPD published here are the electronic publications of the volumes of
Publications of Debrecen Heliophysical Observatory Heliographic Series.
At the Debrecen Observatory there are no magnetic observations. However, we can complete the white-light observations with magnetic observations by courtesy of several observatories
(see Acknowledgements).
If any of these magnetograms are used in publications, the original source of files should be referred to.
For further information and more data see the original sites of the observatories.
The origins of the magnetic observations are indicated in the file names:
*KittPeak*: full-disk magnetic observations copied from the archive of
NSO Kitt Peak Observatory (Z UNIX compressed fits files),
*HMI*:
SDO/HMI research group at Stanford University (fits files),
*MDI*:
SOHO/MDI research group at Stanford University (fits files),
*GONG*:
Global Oscillation Network Group (GONG) (fits files),
*MWIL*:
Mount Wilson Observatory (*MWIL* fits magnetograms , *MWIL_drawing* sunspot polarity drawings),
*KANZ*:
Kanzelhoehe Observatory ( Na-D filtergrams),
*HSOS*:
Huairou Solar Observing Station (region observations),
*NAOJ*:
Solar Observatory of NAOJ (full-disk and region observations),
*SolnDann*: scanned sunspot polarity drawings (jpg images) from the Solnechnie Dannie solar data reports edited in the
Pulkovo Observatory,
*IMIS*: scanned sunspot polarity drawings of Institute of terrestrial magnetism and radiowave propagation of Siberian division of RAS (Irkutsk) (SibIZMIR), and
*KrAO*: scanned sunspot polarity drawings of Crimean Astrophysical Observatory, and
*UrAO*: scanned sunspot polarity drawings of Astronomical Observatory of Ural State University, and
*UsAO*: scanned sunspot polarity drawings of Ussurijsk Astrophysical Observatory copied from
Combined database of sunspot magnetic fields at Pulkovo Observatory
*YNAO*: scanned sunspot polarity drawings of
Yunnan Astronomical Observatory published in Publications of Yunnan Observatory
*Rome*:
Astronomical Observatory of Rome (region polarity drawings scanned from Solar Phenomena Monthly Bulletin),
*Mees*: vector magnetograms of
Mees Solar Observatory, University of Hawaii, with Haleakala Stokes Polarimeter (HSP) or Imaging Vector Magnetograph (IVM)
It is important to note that magnetic measurements of sunspot umbras made at Kitt Peak are underestimates of true field strengths by a factor of about 50%. That is, one should multiply the fields by a
factor of about 1.5 in umbras (Jack Harvey, 2004, personal communication).
To put a GONG fits image into "standard" orientation one first needs to rotate the image counter clock-wise by OFFSET
(
http://gong.nso.edu/data/DMAC_documentation/Vmbical/GONG_Image_Orientation.html).
This places Solar North at the top. Then one needs to flip the image right-for-left, thus placing Solar East on the left and Solar West on the right. If one does not have the camera offset angle one can assume on offset of 90 degrees.
Red and blue in the full-disk magnetic maps of NAOJ indicate positive (N-polarity) and negative (S-polarity) magnetic fields, respectively.
In the active region vector magnetograms red and blue contours indicate positive (N-polarity) and negative (S-polarity) magnetic fields along the line of sight, and green arrows indicate the strength and direction of transverse magnetic
fields. The image orientation is celestial north at the top and west to the right.
Information copied from the site of Mees Solar observatory:
HSP Magnetograms:
Each magnetogram is a 60 kbyte GIF image. Celestial north is at the top; east is at the left.
Continuum brightness: The underlying image shows a continuum image of the region observed.
Line-of-sight component of the magnetic field: The red and blue contours show the component of the vector magnetic field projected onto the line-of-sight. Red contours
indicate field towards the observer, and blue contours indicate field away from the observer.
Transverse component of the magnetic field: The short,green (or white) line segments show the direction and magnitude of the projection of the magnetic field vector into the plane perpendicular to the line of sight.
Solar Coordinates: The yellow contours show the solar coordinates of the observed region (solar latitude and central meridian distance) in degrees. Negative values indicate the eastern and southern hemispheres.
The Imaging Vector Magnetograph (IVM) at Mees Solar Observatory on Haleakala, Maui, Hawaii measures the polarization of an absorption line in the solar spectrum, and uses the polarization data to map the
vector magnetic field in the solar photosphere. The IVM observes a region about 203,000 km square on the sun.
We express our deepest gratitude to the colleagues at the collaborating observatories for participating in the daily routine observations and putting the necessary material at our disposal.
The contributing observatories taking white-light full disk observations were:
Abastumani Astrophysical Observatory (Georgia),
Ebro Observatory (Spain),
Helwan Observatory (Egypt),
Kanzelhoehe Solar Observatory (Austria),
Kiev University Observatory (Ukraine),
Kislovodsk Solar Observing Station of Pulkovo Observatory (Russia),
Ussuriysk Astrophysical Observatory, Far-Eastern Branch of the Russian Academy of Sciences (Russia),
Kodaikanal Solar Observatory (India),
Mauna Loa Solar Observatory (USA),
Mount Wilson Observatory (USA),
San Fernando Observatory (USA),
Solar Observatory of National Astronomical Observatory of Japan (Mitaka/Tokyo, Japan),
Rome Astronomical Observatory (Italy),
Tashkent Observatory (Uzbekistan),
Royal Observatory of Belgium (USET data/image of Uccle/Brussels, Belgium),
Royal Greenwich Observatory (Herstmonceux, UK),
Valasske Mezirici Observatory (Czech Republic).
We thank the
INAF-Catania Astrophysical Observatory for its full-disk photospheric observations.
The Mount Wilson white-light full disk scans are available thanks to the
Mt.Wilson Solar Photographic Archive Digitization Project
supported by the National Science Foundation under Grant No.0236682. The magnetic database includes data from the synoptic program at the
150-Foot Solar Tower of the
Mount Wilson Observatory. The Mt. Wilson150-Foot Solar Tower is operated by UCLA, with funding from NASA, ONR
and NSF, under agreement with the Mt. Wilson Institute.
The Na-D filtergrams of
Kanzelhoehe Solar Observatory are available by courtesy of the
CentralEuropean Solar ARchives (CESAR).
Space-born full disk quasi-continuum images and LOS magnetograms obtained by the Michelson Doppler Imager (MDI) on the board of Solar and Heliospheric Observatory (SOHO) are used by courtesy of the
SOHO/MDI research group at Stanford University. SOHO (Solar and Heliospheric Observatory) is a mission of international cooperation between ESA and NASA.
The SDO/HMI images are available by courtesy of NASA/SDO and the AIA, EVE, and HMI science teams.
We thank the
NSO/Kitt Peak Observatory for the full disk LOS magnetograms observed with the 512-Channel Magnetograph, Spectromagnetograph and SOLIS VSM.
NSO/Kitt Peak magnetic data used here are produced cooperatively by NSF/NOAO, NASA/GSFC and NOAA/SEL.
We acknowledge the courtesy of editors of Solnechnie Dannie solar catalogue, who permit the use of magnetic polarity drawings observed by several contributing observatories:
Crimean Astrophysical Observatory,
Sayan Observatory of Institute of Solar-Terrestrial Physics of Siberian Department of Russian Academy of Sciences,
Pulkovo Observatory
and its
Kislovodsk Solar Observing Station,
Ussuriysk Astrophysical Observatory (Ussurijsk Solar Service Station) ,
Astronomical Observatory of Ural State University,
Institute of Geophysics and Astronomy of Cuba.
This work utilizes data obtained by the
Global Oscillation Network Group (GONG) Program, managed by the National Solar Observatory, which
is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the
Big Bear Solar Observatory,
High Altitude Observatory,
Learmonth Solar Observatory,
Udaipur Solar Observatory,
Instituto de Astrofisica de Canarias,
and
Cerro Tololo Inter-American Observatory.
We thank the
Huairou Solar Observing Station of National Astronomical Observatories of Chinese Academy of Science for the magnetic observations of the HSOS archive.
We thank the
Solar Observatory of National Astronomical Observatory of Japan (NAOJ) for their full-disk white-light and magnetic observations as well as active region vector magnetograms.
We appreciate the long-term work of
NOAA's National Geophysical Data Center (NGDC) providing wide-range of scientific products and services for solar physics, and publishing the volumes of Solar-Geophysical Data (SGD).
Data used here from
Mees Solar Observatory, University of Hawaii, are produced with the support of NASA grant NNG06GE13G.
We acknowledge the courtesy of
Yunnan Astronomical Observatory (YNAO) for permitting the use of scans of magnetic polarity drawings published in Publications of Yunnan Observatory.
The images of Precision Solar Photometric Telescope (PSPT) at Mauna Loa Solar Observatory are available by courtesy of the
Mauna Loa Solar Observatory, operated by the
High Altitude Observatory, as part of the
National Center for Atmospheric Research (NCAR). NCAR is supported by the National Science Foundation.
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