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INAF PSP velocity-magnetic field correlation coefficient data of solar wind streams
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.. contents:: The tiny table of contents

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)
  - FIELDS


| **Product Type**: data

| **Status**: Active

| **Creation date**: 2022-05-06T10:39:35+02:00

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

Data Description
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| **Data type**: timeseries

| **Data formats**: - ascii


| **Sample**: https://drive.google.com/file/d/1C7lxF193kgoyLwgAU_3UzE29kWigLTQ9/view?usp=sharing

Capabilities
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- int2130.1: Product ingestion
- int2320.1: Data conversion
- int2320.2: metadata mapping
- 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

