again...

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INAF SuperDARN Cross Polar Cap Potential

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=============================

SuperDARN Polar Cap Potential

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.. contents:: The tiny table of contents

SuperDARN maximum potential difference measured across the polar caps.

The Super Dual Auroral Radar Network (SuperDARN) is an international network of

High Frequency coherent scatter radars. A map of the fields of view of the radars

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

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

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

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

allows to infer the velocity of the ambient plasma with respect to the sounded direction

and gate.

**References**

https://www.sciencedirect.com/science/article/abs/pii/S136468260600263X

[1] SuperDARN Data Analysis Working Group, Thomas, E. G., Reimer, A. S., Bland,

E. C., Burrell, A. G., Grocott, A., Ponomarenko, P. V., Schmidt, M. T., Shepherd, S. G.,

Sterne, K. T., and Walach, M.-T, SuperDARN Radar Software Toolkit (RST) 5.0 (v5.0).

Zenodo (2022). https://doi.org/10.5281/zenodo.7467337

[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

[3] Ruohoniemi, J.M., and K.B. Baker, Large-scale imaging of high-latitude

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

Derived From Mid-latitude, High-Latitude, and Polar SuperDARN HF Radar

Observations, J. Geophys. Res., Space Physics, 123(4), 3196-3216 (2018).

https://doi.org/10.1002/2018JA025280

[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

[6] Shepherd, S. G., Altitude-Adjusted Corrected Geomagnetic Coordinates: Definition

and Functional Approximations, J. Geophys. Res., Space Physics, 119(9), 7501-7521

(2014). https://doi.org/10.1002/2014JA020264

Data description

~~~~~~~~~~~~~~~~

:download:`Further readings (pdf) <../../private/inaf_cpcp_superdarn_datacube-SuperDARN_data_handling.pdf>`.

**internal_name:** inaf_cpcp_superdarn_datacube

**publisher:** INAF

**alphanumeric_code:** 31

**Providers**:

**id_tmp:** 71

- **SupeDARN radars British Antarctic Survey repository** - sources:

**short_name:** SuperDARN CPCP

  - https://www.bas.ac.uk/project/superdarn/

  - 

  - 

**identifier:** aspis://inaf/cpcp_superdarn_datacube

**dynamic:** static

| **Product Type**: data

**size:** 200MB

| **Status**: Active

**format:** csv

| **Creation date**: 2022-05-04T16:00:00+02:00

**type:** timeseries

| **Last Update**: 2023-10-01T12:00:00+02:00

**records_number:** 1515672

Data Description

~~~~~~~~~~~~~~~~

**time_start:** 2015-06-21

**time_stop:** 2017-09-11

| **Data type**: timeseries

**spatial:** IONO

| **Data formats**: - ASCII

**messenger:** electrons,

**spectral_min:** 0

| **Sample**: SuperDARN_CPCP

**spectral_max:** 1

Capabilities

~~~~~~~~~~~~

**spectral_units:** dimensionless

- 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

**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.

=====================================

INAF SuperDARN Convection Maps (data)

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.. contents:: The tiny table of contents

Ionospheric convection maps at high latitudes in both hemispheres derived from the raw SuperDARN data retrieved from the BAS repository.

**Providers**:

- **SupeDARN radars British Antarctic Survey repository** - sources:

  - https://www.bas.ac.uk/project/superdarn/

  - 

  - 

| **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**: SuperDARN_Maps_data

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

=========================================

INAF Solar Orbiter-PAS data

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INAF-IAPS Solar Orbiter-PAS data

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.. contents:: The tiny table of contents

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.

Data is hosted on http://soar.esac.esa.int/soar/

**References**

R. De Marco et al, Astronomy &Astrophysics, 669, A108 (2023)

**Providers**:

- **Solar Orbiter** - source:

  - SWA-PAS

| **Product Type**: data

| **Status**: Active

| **Creation date**: 2022-04-20T19:10:47+02:00

| **Last Update**: 2023-10-01T12:00:00+02:00

Data Description

Data description

~~~~~~~~~~~~~~~~

| **Data type**: timeseries

| **Data formats**: - cdf

| **Sample**: https://drive.google.com/file/d/1X_6RZeN72zjR11g2DYNoMTr6DP6vDg_t/view?usp=sharing

Capabilities

~~~~~~~~~~~~

- int2130.1: Product ingestion

- int2130.3: Mirroring: bulk static

- int2320.1: Data conversion

- 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

- 2330.1: wiki

- 2320.2: metadata mapping

- SAMP: Sul Solar Orbiter ARchive  questi dati possono essere condivisi via SAMP

**internal_name:** inaf_data_solopas_timeseries

**publisher:** INAF-IAPS, Plasma & Space Weather Group

**alphanumeric_code:** 14

**id_tmp:** 72

**short_name:** SolO-PAS_data

**identifier:** aspis://inaf/data_solopas_timeseries

**dynamic:** 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

**size:** 2GB

**format:** dsv

**type:** timeseries

**records_number:** 38653

**time_start:** 2020-07-06

**time_stop:** 2022-01-31

**spatial:** IP

**messenger:** Protons

**spectral_min:** 

**spectral_max:** 

**spectral_units:** 

**observable:** SW,SEP

**latest update:** 2024-04-04 01:54:59

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 [UTC ]

   * - 2

     - N

     - cm^-3

     - float

     - Protono Density [cm^-3]

   * - 3

     - VR

     - Km/s

     - float

     - Proton Velocity along the R direction [Km/s]

   * - 4

     - VT

     - Km/s

     - float

     - Proton Velocity along the T direction [Km/s]

   * - 5

     - VN

     - Km/s

     - float

     - Proton Velocity along the N direction [Km/s]

   * - 6

     - T

     - eV

     - float

     - Proton Temperature [eV]

   * - 7

     - VR_SolO

     - Km/s

     - float

     - Spacecraft Velocity along the R direction [Km/s]

   * - 8

     - VT_SolO

     - Km/s

     - float

     - Spacecraft Velocity along the T direction [Km/s]

   * - 9

     - VN_SolO

     - Km/s

     - float

     - Spacecraft Velocity along the N direction [Km/s]

============================================================

INAF Montecarlo, single particle exospheric model of Mercury

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.. contents:: The tiny table of contents

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

**Providers**:

INAF

| **Product Type**: software

| **Status**: Active

| **Creation date**: 2022-05-10T16:05:00+02:00

| **Last Update**: 2022-05-10T04:10:00+02:00

Data Description

~~~~~~~~~~~~~~~~

| **Data type**: ND

| **Data formats**: ND

| **Sample**: ND

Capabilities

~~~~~~~~~~~~

- ext2220.5: On demand computation

=========================================

INAF SVIRCO neutron monitor (1h)

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SVIRCO Observatory - the Rome neutron monitor

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.. contents:: The tiny table of contents

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%

Resolution: 1h. 

**References**

Average intensity of January-February 1997 = 100%

**Providers**:

- **SVIRCO neutron monitor**

Data description

~~~~~~~~~~~~~~~~

**internal_name:** inaf_flux1h_svirco_timeseries

| **Product Type**: data

**publisher:** INAF

| **Status**: Active

**alphanumeric_code:** 42C

| **Creation date**: 2022-04-28T13:31:08+02:00

**id_tmp:** 73

| **Last Update**: 2023-10-01T12:00:00+02:00

**short_name:** flux1h_SVIRCO

Data Description

~~~~~~~~~~~~~~~~

**identifier:** inaf_flux1h_svirco_timeseries

**dynamic:** Data collection grows in time.

**size:** 13MB

**format:** CSV

**type:** timeseries

**records_number:** 479976

**time_start:** 1966-04-01

**time_stop:** 2020-12-31

**spatial:** GROUND

**messenger:** Nucleons

**spectral_min:** 6.3

| **Data type**: timeseries

**spectral_max:** 9999

| **Data formats**: - ASCII

**spectral_units:** GeV

**observable:** GLE,GCR

| **Sample**: https://drive.google.com/file/d/17ahUkpirH-DUWnqBr731ExAgjMBGNeJ4/view?usp=sharing

**latest update:** 2024-03-28 05:08:05

Capabilities

~~~~~~~~~~~~

Columns specification

~~~~~~~~~~~~~~~~~~~~~

- int2130.3: Mirroring: bulk static

- 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

.. list-table:: 

   :widths: 7 20 15 10 48

   :align: right 

   :header-rows: 1

   * - progr

     - column

     - units

     - type

     - description

   * - 1

     - time

     - UTC

     - datetime

     - UTC - Time

   * - 2

     - I

     - %

     - float

     - % - 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%).