Dataset Identification:
Resource Abstract:
- description: A solar flare is a short-lived sudden increase in the intensity of radiation emitted in the neighborhood of sunspots.
For many years it was best monitored in the H-alpha wavelength and occurs in the chromosphere, though occasionally white light
flares are seen in the photosphere. In modern times the solar X-ray wavelengths are monitored via satellite for solar flares.
Flares are characterized by a rise time of the order of minutes and a decay time of the order of tens of minutes. The total
energy expended in a typical flare is about 1030 ergs; the magnetic field is extraordinarily high reaching values of 100 to
10,000 gauss. Optical flares in H-alpha are usually accompanied by radio and X-ray bursts and occasionally by high-energy
particle emissions. The optical brightness and size of the flare are indicated by a two-character code called "importance."
The first character, a number from 1 to 4, indicates the apparent area. For areas of less than 1, an "S" is used
to designate a subflare. The second character indicates relative brilliance: B for bright, N for normal and F for faint. A
general discussion of solar flares is found in Svestka [1976]. The NOAA National Centers for Environmental Information (formerly
NGDC) holds archives for about 80 stations, covering the period 1938 to the present. Currently 5 stations send their data
to NGDC Boulder on a routine monthly basis -- the current main observing emphasis for Space Weather has transitioned to Coronal
Mass Ejections (CMEs) which directly impact the Earth's geomagnetic field. Solar flares impact the Earth's upper
atmosphere and can eject high energy particles that can cause satellite failures. The flare reports were processed and published
in the monthly report "Solar-Geophysical Data" and in a different format in the IAU "Quarterly Bulletin on
Solar Activity."; abstract: A solar flare is a short-lived sudden increase in the intensity of radiation emitted in the
neighborhood of sunspots. For many years it was best monitored in the H-alpha wavelength and occurs in the chromosphere, though
occasionally white light flares are seen in the photosphere. In modern times the solar X-ray wavelengths are monitored via
satellite for solar flares. Flares are characterized by a rise time of the order of minutes and a decay time of the order
of tens of minutes. The total energy expended in a typical flare is about 1030 ergs; the magnetic field is extraordinarily
high reaching values of 100 to 10,000 gauss. Optical flares in H-alpha are usually accompanied by radio and X-ray bursts and
occasionally by high-energy particle emissions. The optical brightness and size of the flare are indicated by a two-character
code called "importance." The first character, a number from 1 to 4, indicates the apparent area. For areas of less
than 1, an "S" is used to designate a subflare. The second character indicates relative brilliance: B for bright,
N for normal and F for faint. A general discussion of solar flares is found in Svestka [1976]. The NOAA National Centers for
Environmental Information (formerly NGDC) holds archives for about 80 stations, covering the period 1938 to the present. Currently
5 stations send their data to NGDC Boulder on a routine monthly basis -- the current main observing emphasis for Space Weather
has transitioned to Coronal Mass Ejections (CMEs) which directly impact the Earth's geomagnetic field. Solar flares impact
the Earth's upper atmosphere and can eject high energy particles that can cause satellite failures. The flare reports
were processed and published in the monthly report "Solar-Geophysical Data" and in a different format in the IAU
"Quarterly Bulletin on Solar Activity."
Citation
- Title Solar Features - Solar Flares.
-
- creation Date
2017-02-07T06:21:02.195922
Resource language:
Processing environment:
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Metadata data stamp:
2018-08-06T21:05:32Z
Resource Maintenance Information
- maintenance or update frequency:
- notes: This metadata record was generated by an xslt transformation from a dc metadata record; Transform by Stephen M. Richard, based
on a transform by Damian Ulbricht. Run on 2018-08-06T21:05:32Z
Metadata contact
-
pointOfContact
- organisation Name
CINERGI Metadata catalog
-
- Contact information
-
-
- Address
-
- electronic Mail Address cinergi@sdsc.edu
Metadata language
eng
Metadata character set encoding:
utf8
Metadata standard for this record:
ISO 19139 Geographic Information - Metadata - Implementation Specification
standard version:
2007
Metadata record identifier:
urn:dciso:metadataabout:7f5b4ac6-7e67-4f5a-b3c3-fc94108400ea
Metadata record format is ISO19139 XML (MD_Metadata)