Diff for "BxByBzTransform"

Differences between revisions 8 and 9

HMI Pipeline Module - Module_Name_Here

Transform vector magnetic field from image coordinates to heliocentric ecliptic coordinates. A projection method, Lambert's Azimuthal equivalent, will be used for this transformation. Vector transformation will base on the formulae specified by Hagyard (1987). This method preserves area. The module will be applied to ARPs only. Uncertainties will be estimated based on variance and covariance from the Inversion code.

Module Inputs

Inputs: B_total, Filling Factor (under condition), inclination, azimuth and their uncertainties in image coordinates.

Module Outputs

Output: Bxyz field components with uncertainties in heliocentric ecliptic coordinates (a.k.a. Stonyhurst).

Cadence

6 hours?

Options

Indicate if there are any options when running the code

Overall Status of Module

Status of Code

Project.c from Rick.

Status of DRMS module

Indicate status of DRMS module version of module

Issues needing resolution

List issues that still need to be resolved
Describe as many as you like

Responsible scientist

Give name of local coordinator for development of this module

Y. Liu

Remarks

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-  ⇤ ← Revision 8 as of 2009-04-28 08:52:48 → 
  Size: 1404
  Editor: filament
  Comment:
+   ← Revision 9 as of 2009-05-02 01:43:39 → ⇥
  Size: 1441
  Editor: l4-m0
  Comment:
-Deletions are marked like this.
+Additions are marked like this.
 Line 3:
-Transform vector magnetic field from image coordinates to heliographic central eclipse coordinates. A project method, Lambert's Azimuthal equivalent, will be used for this transformation. Vector transformation will base on the formulae specified by Hagyard (1987). This method preserves area. The module will be applied to ARPs only. Uncertanties will be estimated based on variance and covariance from the Inversion  code.
+Transform vector magnetic field from image coordinates to heliocentric ecliptic coordinates. A projection method, Lambert's Azimuthal equivalent, will be used for this transformation. Vector transformation will base on the formulae specified by Hagyard (1987). This method preserves area. The module will be applied to ARPs only. Uncertainties will be estimated based on variance and covariance from the Inversion  code.
 Line 6:
- . Inputs: B_total, Filling Factor (under condition), inclination, azimuth and their uncertaities on image coordinates.
+ . Inputs: B_total, Filling Factor (under condition), inclination, azimuth and their uncertainties in image coordinates.
 Line 9:
- . Output: Bxyz with uncertaities on heliographic central coordinates.
+ . Output: Bxyz field components with uncertainties in heliocentric ecliptic coordinates (a.k.a. Stonyhurst).