The catalogue contains SEP events observed at the Earth of class S1, i.e. with flux in the range [10, 100) pfu, at >10 MeV from 1995 and their properties (onset, peak flux, fluence) as well as features of the associated flare (peak time, class, location), CME (lift off, position, angle width, speed) and radio burst (occurrence of type II or IV). The SEP events having flux >= 100 pfu at > 10 MeV are listed in the companion table S2 SEP Catalogue.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_s1sep_tableset
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 16A
* - **id_tmp:**
- 77
* - **short_name:**
- IAPS-S1 SEP events
* - **identifier:**
- aspis://inaf/s1sep_tableset
* - **dynamic:**
- static
* - **size:**
- 100kB
* - **format:**
- csv
* - **type:**
- tableset
* - **records_number:**
- 68
* - **time_start:**
- 1995-01-01
* - **time_stop:**
- 2014-09-10
* - **spatial:**
- Earth
* - **messenger:**
- Protons,Photons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- flare,CME,SEP
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- utc
- datetime
- UTC - Time of the peak of the SEP associated soft X -ray (SXR) flare. When the time coincides with that of the CME no information about the actual time was available.
* - 2
- SXR_class
- char
- char
- Char - Class of the SEP associated flare according to their peak intensities
* - 3
- Flare_Latitude
- deg
- float
- Degrees - Averaged heliographic latitude of the SEP associated flare central region from observations of the H-alpha spectral line
* - 4
- Flare_Longitude
- deg
- float
- Degrees - Averaged heliographic longitude of the SEP associated flare central region from observations of the H-alpha spectral line. The value 180 indicates longitudes >90, when it cannot be better determined. The value -180 indicates longitudes >90, when
* - 5
- CME_NOAA_date
- utc
- datetime
- UTC - Date and time of the associated CME from the NOAA list (https://umbra.nascom.nasa.gov/SEP/)
* - 6
- CME_SOHO_date
- utc
- datetime
- UTC - In case the CME NOAA Date was not present or not considered reliable in the previous column, the date and time of the associated CME from the SOHO list (https://cdaw.gsfc.nasa.gov/CME_list/UNIVERSAL_ver1/1998_05/univ1998_05.html) is given in this c
* - 7
- CME_central_PA
- deg
- float
- Degrees - CME position angle measured from Solar North in degrees (counter-clockwise). The value 360 indicates a halo CME.
* - 8
- Halo_CME_type
- char
- char
- Char - Halo CMEs are indicated in the 'CME_Central_PA' column with 360. In this column the letters ('S', 'BA', 'OA') in the brackets show type of halo CMEs. Halo CMEs can be symmetric (S) or asymmetric with respect to the occulting disk. Brightness asymme
* - 9
- CME_angular_width
- deg
- float
- Degrees - Angular width of the CME. For values =361 more information are available in the sOHO LASCO CME catalogue (https://cdaw.gsfc.nasa.gov/CME_list/).
* - 10
- CME_Speed_Art1
- km/s
- float
- km/s - CME speed from catalogue of article 1 (Art1) Papaioannou et a. 2016 (doi: 10.1051/swsc/2016035)
* - 11
- Radio_burst_type_II
- char
- int
- Int - Occurrence of type II radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 12
- Radio_burst_type_IV
- char
- int
- Int - Occurrence of type IV radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 13
- CME_Speed_Art2
- km/s
- float
- km/s - CME speed from catalogue of article2 (ART2) Gopalswamy et al. 2015 (doi: 10.48550/arXiv.1509.04216)
* - 14
- SOHO_CME_linear_speed
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through linear fit of height-time measurements
* - 15
- SOHO_CME_speed_2nd
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated at the time of final height measurement
* - 16
- SOHO_CME_speed_20_Rs
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated when the CME is at a height of 20 solar radii
* - 17
- CME_acceleration
- km/s^2
- float
- km/s^2 - Acceleration of the CME
* - 18
- SXR_Fluence
- J/m^2
- float
- J m^2 - Time integrated SXR intensity between the 1/3 power points on rise and fall (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 19
- Radio_Fluence
- sfu*min
- float
- sfu*min - Time integrated 1 MHz intensity from Wind/Waves from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 20
- Frequency
- kHz
- float
- kHz - Used Wind/Waves frequency close to 1 MHz in computing the Radio_Fluence in the previous column
* - 21
- SEP_onset
- utc
- datetime
- UTC - SEP onset time
* - 22
- SEP_threshold
- utc
- datetime
- UTC - Time at which the >10 MeV proton flux exceeds the 10 pfu threshold
* - 23
- SEP_Peak_time
- utc
- datetime
- UTC - Peak proton flux time at >10 MeV energies
* - 24
- SEP_end
- utc
- datetime
- UTC - Time at the end of the SEP event at >10 MeV energies
* - 25
- Peak_proton_flux
- pfu
- float
- pfu=1/(cm^2 s sr) - Peak proton flux at >10 MeV energies
* - 26
- Proton_fluence
- #/(cm^2*sr)
- float
- #/(cm^2 sr) - Time integrated proton flux in the onset-end time interval
* - 27
- GLE
- char
- char
- Char - YES or NO flag indicating the presence or the absence of a Ground Level Enhancement event, respectively.
The catalogue contains SEP events observed at the Earth of class S2, i.e. with flux >100 pfu, at >10 MeV from 1995 and their properties (onset, peak flux, fluence) as well as features of the associated flare (peak time, class, location), CME (lift off, position, angle width, speed) and radio burst (occurrence of type II or IV). The SEP events having flux in the interval [10, 100) pfu at > 10 MeV are listed in the companion table S1 SEP Catalogue.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_s2sep_tableset
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 16B
* - **id_tmp:**
- 78
* - **short_name:**
- IAPS-S2 SEP events
* - **identifier:**
- aspis://inaf/s1sep_tableset
* - **dynamic:**
- static
* - **size:**
- 100kB
* - **format:**
- csv
* - **type:**
- tableset
* - **records_number:**
- 60
* - **time_start:**
- 1995-01-01
* - **time_stop:**
- 2014-09-10
* - **spatial:**
- Earth
* - **messenger:**
- Protons,Photons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- flare,CME,SEP
* - **latest update:**
- 2024-03-28 05:08:06
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- utc
- datetime
- UTC - Time of the peak of the SEP associated soft X -ray (SXR) flare. When the time coincides with that of the CME no information about the actual time was available.
* - 2
- SXR_class
- char
- char
- Char - Class of the SEP associated flare according to their peak intensities
* - 3
- Flare_Latitude
- deg
- float
- Degrees - Averaged heliographic latitude of the SEP associated flare central region from observations of the H-alpha spectral line
* - 4
- Flare_Longitude
- deg
- float
- Degrees - Averaged heliographic longitude of the SEP associated flare central region from observations of the H-alpha spectral line. The value 91 indicates longitudes >90 the value 121 indicates longitudes >120 the value -91 indicates longitudes<-90.
* - 5
- CME_NOAA_date
- utc
- datetime
- UTC - Date and time of the associated CME from the NOAA list (https://umbra.nascom.nasa.gov/SEP/)
* - 6
- CME_SOHO_date
- utc
- datetime
- UTC - In case the CME NOAA Date was not present or not considered reliable in the previous column, the date and time of the associated CME from the SOHO list (https://cdaw.gsfc.nasa.gov/CME_list/UNIVERSAL_ver1/1998_05/univ1998_05.html) is given in this c
* - 7
- CME_central_PA
- deg
- float
- Degrees - CME position angle measured from Solar North in degrees (counter-clockwise). The value 360 indicates a halo CME.
* - 8
- Halo_CME_type
- char
- char
- Char - Halo CMEs are indicated in the 'CME_Central_PA' column with 360. In this column the letters ('S', 'BA', 'OA') in the brackets show type of halo CMEs. Halo CMEs can be symmetric (S) or asymmetric with respect to the occulting disk. Brightness asymme
* - 9
- CME_angular_width
- deg
- float
- Degrees - Angular width of the CME. For values =-361 more information are available in the sOHO LASCO CME catalogue (https://cdaw.gsfc.nasa.gov/CME_list/).
* - 10
- CME_Speed_Art1
- km/s
- float
- km/s - CME speed from catalogue of article 1 (Art1) Papaioannou et a. 2016 (doi: 10.1051/swsc/2016035)
* - 11
- Radio_burst_type_II
- char
- int
- Int - Occurrence of type II radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 12
- Radio_burst_type_IV
- char
- int
- Int - Occurrence of type IV radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 13
- CME_Speed_Art2
- km/s
- float
- km/s - CME speed from catalogue of article2 (ART2) Gopalswamy et al. 2015 (doi: 10.48550/arXiv.1509.04216)
* - 14
- SOHO_CME_linear_speed
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through linear fit of height-time measurements
* - 15
- SOHO_CME_speed_2nd
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated at the time of final height measurement
* - 16
- SOHO_CME_speed_20_Rs
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated when the CME is at a height of 20 solar radii
* - 17
- CME_acceleration
- km/s^2
- float
- km/s^2 - Acceleration of the CME
* - 18
- SXR_Fluence
- J/m^2
- float
- J m^2 - Time integrated SXR intensity between the 1/3 power points on rise and fall (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 19
- Radio_Fluence
- sfu*min
- float
- sfu*min - Time integrated 1 MHz intensity from Wind/Waves from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 20
- Frequency
- kHz
- float
- kHz - Used Wind/Waves frequency close to 1 MHz in computing the Radio_Fluence in the previous column
* - 21
- SEP_onset
- utc
- datetime
- UTC - SEP onset time
* - 22
- SEP_threshold
- utc
- datetime
- UTC - Time at which the >10 MeV proton flux exceeds the 10 pfu threshold
* - 23
- SEP_Peak_time
- utc
- datetime
- UTC - Peak proton flux time at >10 MeV energies
* - 24
- SEP_end
- utc
- datetime
- UTC - Time at the end of the SEP event at >10 MeV energies
* - 25
- Peak_proton_flux
- pfu
- float
- pfu=1/(cm^2 s sr) - Peak proton flux at >10 MeV energies
* - 26
- Proton_fluence
- #/(cm^2*sr)
- float
- #/(cm^2 sr) - Time integrated proton flux in the onset-end time interval
* - 27
- GLE
- char
- char
- Char - YES or NO flag indicating the presence or the absence of a Ground Level Enhancement event, respectively.
Daily proton fluxes in cosmic rays were measured with the Alpha Magnetic Spectrometer aboard the International Space Station, from May 20, 2011 to October 29, 2019 (a total of 2824 days or 114 Bartels rotations) in the rigidity interval from 1 to 100 GV, based on 5.5×10^9 protons collected. Several Forbush decreases were also observed during the whole period, in connection with transient magnetic perturbations. The product provides these data as time-profiles from May 20, 2011 to October 29 2019 as a function of rigidity. In particular the daily proton fluxes are measured in 30 bins from 1.00 to 100 GV. The errors include statistics, time-dependent systematic errors and the total systematic error.
References
~~~~~~~~~~
https://doi.org/10.1103/PhysRevLett.127.271102
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_iss_ams_flux_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 50A
* - **id_tmp:**
- 89
* - **short_name:**
- AMS_daily_H
* - **identifier:**
- aspis:///infn/ams_protons
* - **dynamic:**
- static
* - **size:**
- 4.1MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 83757
* - **time_start:**
- 2011-05-20
* - **time_stop:**
- 2019-10-29
* - **spatial:**
- GEOMAG
* - **messenger:**
- Protons
* - **spectral_min:**
- 1
* - **spectral_max:**
- 100
* - **spectral_units:**
- GV
* - **observable:**
- GCR
* - **latest update:**
- 2024-04-04 02:10:23
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime (2011-05-20T12:00:00) - time UTC of the data-taking
* - 2
- rigidity_min
- GV
- float
- GV (10.1) - lower edge of the rigidity interval
* - 3
- rigidity_max
- GV
- float
- GV (16.6) - upper edge of the rigidity interval
* - 4
- proton_flux
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (259.9) - daily proton flux
* - 5
- proton_flux_error_statistical
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.11) - total statistical error
* - 6
- proton_flux_error_timedependent
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.07) - systematic error from the trigger and reconstruction efficiencies
* - 7
- proton_flux_error_systematic_total
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.24) - total systematic error (sum in quadrature of the time-indep and the time-dep systematic errors)
Time-profiles of galactic cosmic-ray protons measured by the PAMELA detector in space during 4 Forbush Decreases from March 2012 to June 2015 in various rigidity intervals. Each profile is scaled for a suitable period of quiet Sun, estimated about 10 days before each Forbush Decrease
