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
Data description
~~~~~~~~~~~~~~~~
**internal_name:** infn_iss_ams_flux_timeseries
**publisher:** not available in DBF
**alphanumeric_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
- UTC - datetime - Acquisition time of the associated image
* - 2
- S_index
- index
- int
- index of the Sunspot
* - 3
- Width of Contour
- arcsec
- float
- Width of contoured Sunspot in arcseconds
* - 4
- Height of Contour
- arcsec
- float
- Height of contoured Sunspot in arcseconds
* - 5
- HGS_Lon
- deg
- float
- Latitude of contoured Sunspot in Stonyhurst Heliographic Coordinates
* - 6
- HGS_Lat
- deg
- float
- Longitude of contoured Sunspot in Stonyhurst Heliographic Coordinates
* - 7
- Area of Contour
- arcsec**2
- float
- Area of contoured Sunspot in arcseconds squared
* - 8
- HMI_HGS_Lon
- deg
- float
- Latitude of contoured HMI magnetic field element in Stonyhurst Helio- graphic Coordinates
* - 9
- HMI_HGS_Lat
- deg
- float
- Longitude of contoured HMI magnetic field element in Stonyhurst Helio- graphic Coordinates
* - 10
- Average Magnetic Field
- Gauss
- float
- Average Magnetic Field in Gauss
* - 11
- Lat_Distance_sunspot
- arcsec
- float
- Latitude difference between the contoured Sunspot and HMI magnetic field element
* - 12
- Lon_Distance_sunspot
- arcsec
- float
- Longitude difference between the contoured Sunspot and HMI magnetic field element
* - 13
- NOAA number
- index
- int
- NOAA number
* - 14
- Center Latitude_hmi
- deg
- int
- Sunspot group latitude in heliographic degrees (mea- sured in degrees north or south)
* - 15
- Center Longitude_hmi
- deg
- int
- Sunspot group longitude in heliographic degrees (mea- sured in degrees east or west). It provides the east-west position of the region on the Sun’s surface
* - 16
- Area
- uSun
- int
- Total estimated area of the sunspot group in millionths of the solar hemisphere. This field quantifies the size or area covered by the entire sunspot group
* - 17
- Z
- char
- string
- McIntosh classification of the sunspot group. The McIntosh classification is a system used to categorize sunspot groups based on their visual characteristics, including the arrangement and com- plexity of sunspots and magnetic fields. It provides informa
* - 18
- LL
- deg
- int
- Longitudinal extent of the sunspot group in he- liographic degrees. This field indicates the east-west extent of the sunspot group on the solar surface
* - 19
- NN
- index
- int
- Total number of individual sunspots visible in the sunspot group. This field specifies how many individual sunspots are part of the sunspot group
* - 20
- Mag Type
- char
- string
- Modified Mount Wil- son classification of the sunspot group. The Mount Wilson classification is a system used to categorize sunspot groups based on their magnetic prop- erties. The ”Modified” classification may indicate a variation or adapta- tion of the
* - 21
- Lon_Distance_hmi
- arcsec
- float
- Latitude difference between the HMI magnetic field element and Solar- monitor data
* - 22
- Lat_Distance_hmi
- arcsec
- float
- Longitude difference between the HMI magnetic field element and Solar- monitor data