FG: Metrics and Validation - Revision history

Tguild: /* Models */

2015-01-26T18:54:42Z

Models

2015-01-26T18:50:02Z

Coordination / short term progress

2015-01-26T18:49:53Z

Coordination / short term progress

2015-01-26T18:49:42Z

ULF Wave Modeling Challenge

2015-01-26T18:48:19Z

Observations

2014-12-02T17:58:30Z

2014-12-02T17:56:19Z

2014-12-02T17:50:27Z

2014-09-30T14:16:03Z

ULF Wave Modeling Challenge

2014-09-30T14:13:05Z

ULF Wave Modeling Challenge

@@ Line 30: / Line 30: @@
 * LFM (Claudepierre)
 * BATS-R-US (Hartinger)
-* OpenGGCM (Raeder)
+* OpenGGCM (CCMC)
 * Empirical Magnetic field models
 * ...

@@ Line 38: / Line 38: @@
 * CCMC for runs/analysis (Lutz with Claudepierre & Hartinger tools)
 * What should we compare first?
-  * Idealized runs at CCMC with Alberta empirical PSD?
+ * Idealized runs at CCMC with Alberta empirical PSD?
-  * March 1-15 runs at CCMC with which data?
+ * March 1-15 runs at CCMC with which data?

@@ Line 38: / Line 38: @@
 * CCMC for runs/analysis (Lutz with Claudepierre & Hartinger tools)
 * What should we compare first?
-   * Idealized runs at CCMC with Alberta empirical PSD?
+  * Idealized runs at CCMC with Alberta empirical PSD?
-   * March 1-15 runs at CCMC with which data?
+  * March 1-15 runs at CCMC with which data?

← Older revision		Revision as of 18:49, 26 January 2015
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	* Empirical Magnetic field models		* Empirical Magnetic field models
	* ...		* ...
		+
		+	=== Coordination / short term progress ===
		+
		+	* CCMC for runs/analysis (Lutz with Claudepierre & Hartinger tools)
		+	* What should we compare first?
		+	* Idealized runs at CCMC with Alberta empirical PSD?
		+	* March 1-15 runs at CCMC with which data?

@@ Line 21: / Line 21: @@
 === Observations ===
 * Remotely sensed ULF wave fields from magnetometers (U. Alberta)
 * ...

@@ Line 3: / Line 3: @@
 == ULF Wave Modeling Challenge ==
-We're organizing a modeling challenge to investigate the ability of global models to reproduce ULF wave fields in the magnetosphere, and ultimately if those ULF fields can radially diffuse an existing electron population from L~5.5 to L~4.5 in two weeks.
+We're organizing a modeling challenge to investigate the ability of global models to reproduce ULF wave fields in the magnetosphere, and ultimately if those ULF fields can radially diffuse an existing electron population from L~5.5 to L~4.5 in two weeks.  To get there, we can split the question into two distinct ones:
-. Can global models of the magnetosphere reproduce the observed persistent, solar wind driven, low mode number ULF wave fields in the magnetosphere?
+. Can global models of the magnetosphere reproduce the observed persistent, solar wind driven, low mode number ULF wave fields in the magnetosphere? and...
 . Are those waves capable of producing  the observed energetic radiation belt population evolution observed during the first two weeks of March 2013 as observed by Van Allen Probes?
@@ Line 23: / Line 23: @@
 * EMFISIS wave fields from Van Allen Probes
 * Remotely sensed ULF wave fields from magnetometers (U. Alberta)
 === Models ===
@@ Line 30: / Line 31: @@
 * OpenGGCM (Raeder)
 * Empirical Magnetic field models

← Older revision		Revision as of 17:56, 2 December 2014
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	The figure above is the REPT flux from http://www.rbsp-ect.lanl.gov/science/LTPlots/RBSP-ECT_LT_Mission_plot.pdf with the interval I mentioned circled in pink. Tick marks in time (x-axis) are one month in duration. The modest electron belt which starts out at L~5.5 seems to diffuse inward a whole L in two weeks. I would think that a key aspect of that question which MHD models could uniquely constrain is the fraction of the diffusion which is accomplished by solar wind driving alone.		The figure above is the REPT flux from http://www.rbsp-ect.lanl.gov/science/LTPlots/RBSP-ECT_LT_Mission_plot.pdf with the interval I mentioned circled in pink. Tick marks in time (x-axis) are one month in duration. The modest electron belt which starts out at L~5.5 seems to diffuse inward a whole L in two weeks. I would think that a key aspect of that question which MHD models could uniquely constrain is the fraction of the diffusion which is accomplished by solar wind driving alone.
		+
		+
		+	The 1st question above may be divided into two basic ULF wave challenges dealing with (Level 0) a idealized continuum of solar wind frequencies [Claudepierre et al., 2010, Paragraph 12] and (Level 1) the real solar wind input from 1-16 March 2013.
		+

	=== Observations ===		=== Observations ===

← Older revision		Revision as of 14:13, 30 September 2014
Line 14:		Line 14:

	The figure above is the REPT flux from http://www.rbsp-ect.lanl.gov/science/LTPlots/RBSP-ECT_LT_Mission_plot.pdf with the interval I mentioned circled in pink. Tick marks in time (x-axis) are one month in duration. The modest electron belt which starts out at L~5.5 seems to diffuse inward a whole L in two weeks. I would think that a key aspect of that question which MHD models could uniquely constrain is the fraction of the diffusion which is accomplished by solar wind driving alone.		The figure above is the REPT flux from http://www.rbsp-ect.lanl.gov/science/LTPlots/RBSP-ECT_LT_Mission_plot.pdf with the interval I mentioned circled in pink. Tick marks in time (x-axis) are one month in duration. The modest electron belt which starts out at L~5.5 seems to diffuse inward a whole L in two weeks. I would think that a key aspect of that question which MHD models could uniquely constrain is the fraction of the diffusion which is accomplished by solar wind driving alone.
		+
		+	=== Observations ===
		+
		+	- EMFISIS wave fields from Van Allen Probes
		+	- Remotely sensed ULF wave fields from magnetometers (U. Alberta)
		+
		+	=== Models ===
		+
		+	- LFM (Claudepierre)
		+	- BATS-R-US (Hartinger)
		+	- OpenGGCM (Raeder)
		+	- Empirical Magnetic field models
		+

	Paragraph 12 of Claudepierre et al., 2010 discusses "continuum" of solar wind frequencies		Paragraph 12 of Claudepierre et al., 2010 discusses "continuum" of solar wind frequencies