currently in operation can be seen in Figure 1: INAF-IAPS manages the radar pair of
Dome C East (DCE) and Dome C North (DCN) located at the Concordia station, in
Antarctica, whose fields of view are shaded in green in the figure.
The SuperDARN concept is described in detail in [2]. A SuperDARN radar is a bistatic
**Providers**:
apparatus (i.e. the same antennae and the same electronics are used to both transmit
and receive signals to/from the ionosphere), which works in the 8-20 MHz frequency
- **SupeDARN radars British Antarctic Survey repository** - sources:
range: coded sequences of radio pulses are steered through a field of view several tens
degrees wide along a number of “beams” (directions), so that the whole field of view
- https://www.bas.ac.uk/project/superdarn/
is covered in one or two minutes, depending on the operating mode. Along each beam,
-
the pulse sequence defines from 75 to 100 range gates, from 180 km up to 3000 km
-
from the radar site, where the radio signals encounter plasma density irregularities in
the ionosphere, which cause such signals to be scattered back along the same direction.
As ionospheric irregularities are dragged in the large scale convection at high latitudes, the measure of the Doppler phase shift between the emitted and backscattered waves
| **Product Type**: data
allows to infer the velocity of the ambient plasma with respect to the sounded direction
[2] Greenwald, R.A., Baker, K.B., Dudeney, J.R. et al., DARN/SuperDARN, A global
view of the dynamics of high-latitude convection, Space Sci Rev, 71, 761–796 (1995).
https://doi.org/10.1007/BF00751350
| **Sample**: SuperDARN_CPCP
[3] Ruohoniemi, J.M., and K.B. Baker, Large-scale imaging of high-latitude
Capabilities
convection with Super Dual Auroral Radar Network HF radar observations, J. Geophys. Res., Space Physics, 103, 20797-20811 (1998).https://doi.org/10.1029/98JA01288
~~~~~~~~~~~~
[4] Thomas, E. G., and S. G. Shepherd, Statistical Patterns of Ionospheric Convection
- int2130.1: Product ingestion
Derived From Mid-latitude, High-Latitude, and Polar SuperDARN HF Radar
- int2320.1: Data conversion
Observations, J. Geophys. Res., Space Physics, 123(4), 3196-3216 (2018).
- 2320.2 meta data mapping: meta data mapping (MANCA NELLA TENDINA)
https://doi.org/10.1002/2018JA025280
- ext2220.1: Standard Visualisation: Web GUI
- ext2220.2: Standard Query: Web GUI
[5] Baker, K. B., and S. Wing, A new coordinate system for conjugate studies at high latitudes, J. Geophys. Res., 94(A7), 9139 (1989).https://doi.org/10.1029/JA094iA07p09139
- ext2220.3: Download: Web GUI
[6] Shepherd, S. G., Altitude-Adjusted Corrected Geomagnetic Coordinates: Definition
- ext2230.1: Advanced Visualisation: ASPIS.py
and Functional Approximations, J. Geophys. Res., Space Physics, 119(9), 7501-7521
- ext2230.2: Advanced Query: ASPIS.py
(2014). https://doi.org/10.1002/2014JA020264
- ext2230.3: Download: ASPIS.py
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_cpcp_superdarn_datacube
* - **publisher:**
- INAF
* - **alph_code:**
- 31
* - **id_tmp:**
- 71
* - **short_name:**
- SuperDARN CPCP
* - **identifier:**
- aspis://inaf/cpcp_superdarn_datacube
* - **dynamic:**
- static
* - **size:**
- 200MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 1515672
* - **time_start:**
- 2015-06-21
* - **time_stop:**
- 2017-09-11
* - **spatial:**
- IONO
* - **messenger:**
- electrons,
* - **spectral_min:**
- 0
* - **spectral_max:**
- 1
* - **spectral_units:**
- dimensionless
* - **observable:**
- IMF,GEOINDEX
* - **latest update:**
- 2024-04-04 01:53:25
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- Time representation ISO8601: YYYY-MO-DYTHR:MN:SC
* - 2
- hem
-
- string
- Flag identifying the hemisphere where data are taken for a given record. “N”=North; “S”=South
* - 3
- ndata
- counts
- int
- Number of velocity vectors actually measured by the radars in the given time interval
* - 4
- minlat
- deg
- int
- Low latitude limit for the convection: it is the 0 described in Section 2.
* - 5
- latpole
- deg
- float
- Geographic latitude of the AACGM pole (North or South). It can be useful for coordinate transformations.
* - 6
- lonpole
- deg
- float
- Geographic longitude of the AACGM pole (North or South). It can be useful for coordinate transformations.
* - 7
- radpole
- Earth radii (Re=6371.2 km)
- float
- Distance from the centre of the Earth of the AACGM pole.
* - 8
- imfbx
- nT
- float
- GSM* x component of the interplanetary magnetic field. Data are taken from DSCOVR spacecraft, ballistically propagated to the centre of the Earth, median filtered and averaged in the 2 minutes time intervals of the radar scans. IMF is used to select the model patterns to be added to the measured vectors in order to reconstruct convection in the whole polar cap.
* - 9
- imfby
- nT
- float
- GSM* y component of the interplanetary magnetic field.
* - 10
- imfbz
- nT
- float
- GSM* z component of the interplanetary magnetic field.
* - 11
- imfbt
- nT
- float
- IMF strength. Btot = sqrt(Bx^2 + By^2 + Bz^2)
* - 12
- kpr
-
- string
- Range of geomagnetic Kp index during the given time interval. This parameter is used to select the model patterns to be added to the measured vectors in order to reconstruct convection in the whole polar cap. This field represents an information useful to be reported in the convection maps.
* - 13
- cpcp
- V
- float
- Cross Polar Cap Potential: Maximum potential difference through the polar cap.
* - 14
- maxpot
- V
- float
- Maximum positive value of the electric potential.
* - 15
- minpot
- V
- float
- Minimum negative value of the electric potential.
* - 16
- l
- counts
- int
- l-order of the harmonic expansion of the potential.
* - 17
- m
- counts
- int
- m-order of the harmonic expansion of the potential. -l ≤ m ≤ l
* - 18
- coef
- V
- float
- Alm coefficient of the harmonic expansion of the potential. If m<0, then the coefficient is the Blm in Eq. 2.
The product contains density N, speed vector V, pressure tensor P, temperature components (Tx, Ty, Tz), and the velocity of the satellite V_solo, computed using the data collected by the Proton-Alpha Sensor (PAS) onboard Solar Orbiter.
The product contains density N, speed vector V, pressure tensor P, temperature components (Tx, Ty, Tz), and the velocity of the satellite V_solo, computed using the data collected by the Proton-Alpha Sensor (PAS) onboard Solar Orbiter.
PAS measures the 3D distribution functions of the dominant ions of the solar wind, from 200 eV to 20 KeV, without mass and charge selection. In practice, this concerns mostly the proton and alfa populations (unseparated). At full resolution, PAS collects the 3D ion distribution function in about 1 second, even though the moments have a cadence of 4 seconds, while in “snapshot” mode the phase space sampling is reduced, allowing a greater cadence for the moments.
PAS measures the 3D distribution functions of the dominant ions of the solar wind, from 200 eV to 20 KeV, without mass and charge selection. In practice, this concerns mostly the proton and alfa populations (unseparated). At full resolution, PAS collects the 3D ion distribution function in about 1 second, even though the moments have a cadence of 4 seconds, while in “snapshot” mode the phase space sampling is reduced, allowing a greater cadence for the moments.
Data is hosted on http://soar.esac.esa.int/soar/
Data is hosted on http://soar.esac.esa.int/soar/
**References**
References
~~~~~~~~~~
R. D’Amicis et al, Astronomy &Astrophysics 656, A21 (2021)
B. Lavraud et al, Astronomy &Astrophysics 656, A37 (2021)
D. Perrone et al, Astronomy &Astrophysics 668, A189 (2022)
R. D’Amicis et al, Astronomy &Astrophysics 656, A21 (2021)
B. Lavraud et al, Astronomy &Astrophysics 656, A37 (2021)
D. Perrone et al, Astronomy &Astrophysics 668, A189 (2022)
R. De Marco et al, Astronomy &Astrophysics, 669, A108 (2023)
R. De Marco et al, Astronomy &Astrophysics, 669, A108 (2023)
**Providers**:
Dataset summary
~~~~~~~~~~~~~~~
- **Solar Orbiter** - source:
.. list-table::
- SWA-PAS
* - **internal_name:**
- inaf_data_solopas_timeseries
| **Product Type**: data
* - **publisher:**
- INAF-IAPS, Plasma & Space Weather Group
| **Status**: Active
* - **alph_code:**
- 14
| **Creation date**: 2022-04-20T19:10:47+02:00
* - **id_tmp:**
- 72
| **Last Update**: 2023-10-01T12:00:00+02:00
* - **short_name:**
- SolO-PAS_data
Data Description
* - **identifier:**
~~~~~~~~~~~~~~~~
- aspis://inaf/data_solopas_timeseries
* - **dynamic:**
| **Data type**: timeseries
- a file each day (file size between 3 and 4 Mb). As a general rule, one month of data is uploaded each month, generally relating to 3 months before the upload date
The model is based on the code by Mura et al., described in doi:10.1016/j.icarus.2008.11.014, doi:10.1016/j.pss.2006.11.028 and integrated in doi: 10.1016/j.pss.2011.08.012
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes.
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 1h. Average intensity of January-February 1997 = 100%
- % - Normalized Intensity of the cosmic ray secondary nucleonic component measured by the Rome neutron monitor. The counting rates have been normalized to the reference value of January-February 1997 (= 100%).
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 1min
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 5min
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 5min Average intensity of January-February 1997 = 100%
Counting rate of the neutron monitor operating at the Testa Grigia Station (3480 m, Cervinia, Italy). The aim is to study the cosmic ray intensity variations in correlation with solar activity and space weather phenomena.
Quasi 3-d magnetic field maps of magnetic field configuration within magnetic clouds for geoeffective target SWE events. Such maps will be estimated through the Grad-Shafranov reconstruction from single-spacecraft plasma and magnetic field data.
Quasi 3-d magnetic field maps of magnetic field configuration within magnetic clouds for geoeffective target SWE events. Such maps will be estimated through the Grad-Shafranov reconstruction from single-spacecraft plasma and magnetic field data.
**Providers**:
References
~~~~~~~~~~
- **Wind** - sources:
- MFI
- SWE
Dataset summary
- **Solar Orbiter** - sources:
~~~~~~~~~~~~~~~
- SWA
.. list-table::
- MAG
- **Small Scale Magnetic Flux Rope Database** - source:
* - **internal_name:**
- inaf_gsmaps_datacube
- http://fluxrope.info/
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
The catalogue will contain the > M2 Soft X- Ray (SXR) flares from 1995 to 2017. The columns in the table are defined as follows: (1) event number; (2) date of the SXR flare; (3) peak time of SXR flare; (4) peak SXR classification (saturated events flagged with an S in which case (3) refers to the onset of saturation); (5) flare location; (6) time-integrated SXR intensity (nominally between the 1/3 power points on rise and fall); (7) time-integrated 1 MHz Wind/WAVES intensity from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak; (8) Waves frequency used.
The catalogue will contain the > M2 Soft X- Ray (SXR) flares from 1995 to 2017. The columns in the table are defined as follows: (1) event number (2) date of the SXR flare (3) peak time of SXR flare (4) peak SXR classification (saturated events flagged with an S in which case (3) refers to the onset of saturation), (5) flare location, (6) time-integrated SXR intensity (nominally between the 1/3 power points on rise and fall), (7) time-integrated 1 MHz Wind/WAVES intensity from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak, (8) Waves frequency used.
- Classification of SXR bursts according to their peak intensities
* - 5
- SXR Class Label
-
- string
- Letter indicating the Peak SXR flux range, according to the standard SXR classification
* - 6
- SXR Class Intensity
- <unit>
- float
- Number indicating the factor for the flare within the class
* - 7
- Location Halpha-line
-
- string
- Averaged heliographic position of flare central region from observations on the H-alpha spectral line
* - 8
- HGS lat
- deg
- float
- Averaged heliographic latitude of flare central region from observations on the H-alpha spectral line
* - 9
- HGS lon
- deg
- float
- Averaged heliographic longitude of flare central region from observations on the H-alpha spectral line
* - 10
- SXR Fluence
- J/m^2
- float
- Time integrated SXR intensity between the 1/3 power points on rise and fall (J m^2)
* - 11
- Wind/Waves Fluence
- sfu*min
- float
- 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 (sfu x min)
Dataset of observations of Mercury's exosphere in the sodium D lines. Data are taken from the ground-based solar telescope THEMIS (years 2009-2013). They have been produced in both D1 and D2 lines (when both available) and converted into bi-dimensional maps of Rayleigh emission. Estimation of the “seeing” parameter is included in the jpeg files. Here the original fits files are given too for the whole database (2007-2014), and it may be expanded to the most recent data from 2021 and 2022 (TBC). Data can be provided both uncalibrated and/or calibrated (TBD).
Dataset of observations of Mercury's exosphere in the sodium D lines. Data are taken from the ground-based solar telescope THEMIS (years 2009-2013). They have been produced in both D1 and D2 lines (when both available) and converted into bi-dimensional maps of Rayleigh emission. Estimation of the “seeing” parameter is included in the jpeg files. Here the original fits files are given too for the whole data base (2007-2014), and it may be expanded to the most recent data from 2021 and 2022 (TBC). Data can be provided both uncalibrated and/or calibrated (TBD).
**Providers**:
References
~~~~~~~~~~
- **THEMIS solar telescope**
Leblanc, F., Doressoundiram, A., Schneider, N., Mangano, V., López Ariste, A., Lemen, C., Gelly, B., Barbieri, C. and Cremonese, G., 2008. High latitude peaks in Mercury's sodium exosphere: Spectral signature using THEMIS solar telescope. Geophysical Research Letters, 35(18).
| **Product Type**: data
Leblanc, F., Doressoundiram, A., Schneider, N., Massetti, S., Wedlund, M., López Ariste, A., Barbieri, C., Mangano, V. and Cremonese, G., 2009. Short‐term variations of Mercury's Na exosphere observed with very high spectral resolution. Geophysical research letters, 36(7).
| **Status**: Active
Mangano, V., Massetti, S., Milillo, A., Mura, A., Orsini, S. and Leblanc, F., 2013. Dynamical evolution of sodium anisotropies in the exosphere of Mercury. Planetary and Space Science, 82, pp.1-10.
| **Creation date**: 2022-04-29T17:15:42+02:00
Mangano, V., Massetti, S., Milillo, A., Plainaki, C., Orsini, S., Rispoli, R. and Leblanc, F., 2015. THEMIS Na exosphere observations of Mercury and their correlation with in-situ magnetic field measurements by MESSENGER. Planetary and Space Science, 115, pp.102-109.
| **Last Update**: 2023-10-01T12:00:00+02:00
Massetti, S., Mangano, V., Milillo, A., Mura, A., Orsini, S. and Plainaki, C., 2017. Short‐term observations of double‐peaked Na emission from Mercury's exosphere. Geophysical Research Letters, 44(7), pp.2970-2977.
Data Description
Orsini, S., Mangano, V., Milillo, A., Plainaki, C., Mura, A., Raines, J.M., De Angelis, E., Rispoli, R., Lazzarotto, F. and Aronica, A., 2018. Mercury sodium exospheric emission as a proxy for solar perturbations transit. Scientific reports, 8(1), p.928.
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.
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.
- 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.
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.
- 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.
Simulated flux maps of SW precipitating onto the surface of Mercury for a subset of IMF condition, with surface resolution of 1° (LAT/LON) and IMF binning of 5 nT (from -20 to 20 nT)
**Providers**:
Missing providers
| **Product Type**: data
| **Status**: Active
| **Creation date**: 2022-05-04T16:00:00+02:00
| **Last Update**: 2023-10-01T12:00:00+02:00
Data Description
~~~~~~~~~~~~~~~~
| **Data type**: image
| **Data formats**: - PNG
| **Sample**: Simulated_SW_Flux
Capabilities
~~~~~~~~~~~~
- int2130.1: Product ingestion
- int2320.1: Data conversion
- 2320.2 meta data mapping: meta data mapping (MANCA NELLA TENDINA)
- ext2220.1: Standard Visualisation: Web GUI
- ext2220.2: Standard Query: Web GUI
- ext2220.3: Download: Web GUI
- ext2230.1: Advanced Visualisation: ASPIS.py
- ext2230.2: Advanced Query: ASPIS.py
- ext2230.3: Download: ASPIS.py
- ext 2330.1 MANCA DALLA LISTA A TENDINA: MANCA DALLA LISTA A TENDINA???
Galactic cosmic ray intensity variations associated to the passage of magnetic clouds. The particle intensity variation is estimated through a dedicated full-orbit test-particle simulation.
Galactic cosmic ray intensity variations associated to the passage of magnetic clouds. The particle intensity variation is estimated through a dedicated full-orbit test-particle simulation.
The velocity - magnetic field (v-b) correlation coefficient unables to identify Alfvénic solar wind intervals (along with almost constant magnetic field magnitude and proton number density). It is derived as the ratio between the covariance of velocity and magnetic field (in Alfvén units) components and the product of their standard deviations, in a time window ranging between tens of minutes to hours. In principle, this formula should be applied to every component of the velocity (V_i) and magnetic fields (B_i) (with i = R, T, N in RTN coordinate system or i = X, Y, Z in GSE coordinate system). The total correlation coefficient is then derived as the average from the three components. However, for the sake of simplicity, we consider only the N component since more Alfvénic than the other two.
**Providers**:
- **Parker Solar Probe** - sources:
- Solar Wind Electrons Alphas and Protons investigation (SWEAP)
Stefano Scardigli authoreda6f0273f
Valerio Formato authored