About this Dataset

Solar Flares From RHESSI Mission

Context

Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI, originally High Energy Solar Spectroscopic Imager or HESSI) is a NASA solar flare observatory. It is the sixth mission in the Small Explorer program, selected in October 1997 and launched on 5 February 2002. Its primary mission is to explore the physics of particle acceleration and energy release in solar flares.
HESSI was renamed to RHESSI on 29 March 2002 in honor of Reuven Ramaty, a pioneer in the area of high energy solar physics. RHESSI is the first space mission named after a NASA scientist. RHESSI was built by Spectrum Astro for Goddard Space Flight Center and is operated by the Space Sciences Laboratory in Berkeley, California. The principal investigator from 2002 to 2012 was Robert Lin, who was succeeded by Säm Krucker.

useful links:
https://en.wikipedia.org/wiki/Reuven_Ramaty_High_Energy_Solar_Spectroscopic_Imager
https://hesperia.gsfc.nasa.gov/hessi/objectives.htm

Content

Ramaty High Energy Solar Spectroscopic Imager (RHESSI)

Notes:
Note that only events with non-zero position and energy range not equal to 3-6 keV are confirmed as solar sources.
Events which have no position and show up mostly in the front detectors, but were not able to be imaged
are flagged as "PS".

Events which do not have valid position are only confirmed to be non-solar if the NS flag is set.

Peak Rate: peak counts/second in energy range 6-12 keV, averaged over active collimators, including background.

Total Counts: counts in energy range 6-12 keV integrated over duration of flare summed over all subcollimators,
including background.

Energy: the highest energy band in which the flare was observed. Electron Kev (kilo electron volt)
https://en.wikipedia.org/wiki/Electronvolt

Radial Distance: distance from Sun center

Quality Codes: Qn, where n is the total number of data gap, SAA, particle, eclipse or decimation flags set for event.
n ranges from 0 to 11. Use care when analyzing the data when the quality is not zero.

Active_Region: A number for the closest active region, if available

radial_offset: the offset of the flare position from the spin axis of the spacecraft in arcsec. This is used i
spectroscopy.

peak_c/s: peak count rate in corrected counts.

Flare Flag Codes:
a0 - In attenuator state 0 (None) sometime during flare
a1 - In attenuator state 1 (Thin) sometime during flare
a2 - In attenuator state 2 (Thick) sometime during flare
a3 - In attenuator state 3 (Both) sometime during flare
An - Attenuator state (0=None, 1=Thin, 2=Thick, 3=Both) at peak of flare
DF - Front segment counts were decimated sometime during flare
DR - Rear segment counts were decimated sometime during flare
ED - Spacecraft eclipse (night) sometime during flare
EE - Flare ended in spacecraft eclipse (night)
ES - Flare started in spacecraft eclipse (night)
FE - Flare ongoing at end of file
FR - In Fast Rate Mode
FS - Flare ongoing at start of file
GD - Data gap during flare
GE - Flare ended in data gap
GS - Flare started in data gap
MR - Spacecraft in high-latitude zone during flare
NS - Non-solar event
PE - Particle event: Particles are present
PS - Possible Solar Flare; in front detectors, but no position
Pn - Position Quality: P0 = Position is NOT valid, P1 = Position is valid
Qn - Data Quality: Q0 = Highest Quality, Q11 = Lowest Quality
SD - Spacecraft was in SAA sometime during flare
SE - Flare ended when spacecraft was in SAA
SS - Flare started when spacecraft was in SAA

Acknowledgements

What is a solar flare?

A Solar flare is the rapid release of a large amount of energy stored in the solar atmosphere. During a flare, gas is heated to 10 to 20 million degrees Kelvin (K) and radiates soft X rays and longer-wavelength emission. Unable to penetrate the Earth's atmosphere, the X rays can only be detected from space. Instruments on Skylab, SMM, the Japanese/US Yohkoh mission and other spacecraft have recorded many flares in X rays over the last twenty years or so. Ground-based observatories have recorded the visible and radio outputs. These data form the basis of our current understanding of a solar flare. But there are many possible mechanisms for heating the gas, and observations to date have not been able to differentiate between them.

HESSI's new approach

Researchers believe that much of the energy released during a flare is used to accelerate, to very high energies, electrons (emitting primarily X-rays) and protons and other ions (emitting primarily gamma rays). The new approach of the HESSI mission is to combine, for the first time, high-resolution imaging in hard X-rays and gamma rays with high-resolution spectroscopy, so that a detailed energy spectrum can be obtained at each point of the image.

This new approach will enable researchers to find out where these particles are accelerated and to what energies. Such information will advance understanding of the fundamental high-energy processes at the core of the solar flare problem.
https://hesperia.gsfc.nasa.gov/hessi/objectives.htm

Inspiration

Explore,
Know something new,
Predict the solar flare,
Respect the Sun and value it and
Take care of the environments.

Thanks

Tables

Hessi Solar Flare 2002to2016

@kaggle.khsamaha_solar_flares_rhessi.hessi_solar_flare_2002to2016

3.19 MB
113942 rows
18 columns


CREATE TABLE hessi_solar_flare_2002to2016 (
  "flare" BIGINT,
  "start_date" TIMESTAMP,
  "start_time" VARCHAR,
  "peak" VARCHAR,
  "end" VARCHAR,
  "duration_s" BIGINT,
  "peak_c_s" BIGINT,
  "total_counts" BIGINT,
  "energy_kev" VARCHAR,
  "x_pos_asec" BIGINT,
  "y_pos_asec" BIGINT,
  "radial" BIGINT,
  "active_region_ar" BIGINT,
  "flag_1" VARCHAR,
  "flag_2" VARCHAR,
  "flag_3" VARCHAR,
  "flag_4" VARCHAR,
  "flag_5" VARCHAR
);

Hessi Solar Flare Up To 2018

@kaggle.khsamaha_solar_flares_rhessi.hessi_solar_flare_up_to_2018

3.27 MB
116143 rows
18 columns


CREATE TABLE hessi_solar_flare_up_to_2018 (
  "flare" BIGINT,
  "start_date" TIMESTAMP,
  "start_time" VARCHAR,
  "peak" VARCHAR,
  "end" VARCHAR,
  "duration_s" BIGINT,
  "peak_c_s" BIGINT,
  "total_counts" DOUBLE,
  "energy_kev" VARCHAR,
  "x_pos_asec" BIGINT,
  "y_pos_asec" BIGINT,
  "radial" BIGINT,
  "active_region_ar" BIGINT,
  "flag_1" VARCHAR,
  "flag_2" VARCHAR,
  "flag_3" VARCHAR,
  "flag_4" VARCHAR,
  "flag_5" VARCHAR
);