style for some files

Elena.Budnik
1 parent dbb05891
Showing 3 changed files with 22 additions and 4 deletions Show diff stats
Instrument/AMDA/ACE/MAG.xml
NumericalData/AMDA/Cluster/Cluster1/PEACE/clust1-pea-mom.xml
NumericalData/AMDA/Juno/JEDI/juno-jedi-e090.xml
@@ -11,7 +11,25 @@
       <AlternateName>ACE MFI</AlternateName>
       <AlternateName>1997-045A-09</AlternateName>
       <ReleaseDate>2016-11-18T16:00:05Z</ReleaseDate>
-      <Description>The ACE Magnetometer (MAG) experiment consists of two triaxial fluxgate magnetometers mounted remotely on booms extending beyond the spacecraft solar panels at four meters from the spacecraft center. Each identical sensor (M1, M2) has a wide dynamic range of sensitivity at +- 0.004 to +- 65536 nT and measures the three vector components of the magnetic field. Usage of twin magnetometer sensors for measurements of weak interplanetary magnetic fields is a proven approach based on experience from many past space missions. The MAG sensors were originally built as spares for the MFI instrument on the Wind spacecraft and have been given minor modifications for inclusion on ACE. Readout of MAG data includes three data types: (1) average magnetic field vectors from the primary and secondary sensors, (2) "Snap-Shot Memory" data, and (3) Fast Fourier Transform (FFT) data. The average vector readout includes 216 bps corresponding to six vectors per second. These vector readouts can be split between M1 and M2 in the ratios of 3:3, 5:1, or 6:0. The "Snap-Shot Memory" stores field vectors at the maximum sampling rate of 30 vectors per second and is read out at 48 bps. The FFT readout includes 17 seconds accumulation of vector data transformed into spectral matrices of the components and total magnitude at a transmission rate of 32 bps. Prof. Norman F. Ness of the Bartol Research Institute at the University of Delaware is the MAG Experiment Manager.</Description>
+      <Description>The ACE Magnetometer (MAG) experiment consists of two triaxial fluxgate magnetometers mounted remotely on booms extending 
+        beyond the spacecraft solar panels at four meters from the spacecraft center. 
+        Each identical sensor (M1, M2) has a wide dynamic range of sensitivity at +- 0.004 to +- 65536 nT and measures the three vector components of 
+        the magnetic field. Usage of twin magnetometer sensors for measurements of weak interplanetary magnetic fields is a proven approach based on 
+        experience from many past space missions. The MAG sensors were originally built as spares for the MFI instrument on the Wind spacecraft and 
+        have been given minor modifications for inclusion on ACE. 
+        
+        Readout of MAG data includes three data types: 
+        * average magnetic field vectors from the primary and secondary sensors,
+        * "Snap-Shot Memory" data,  
+        * Fast Fourier Transform (FFT) data. 
+        
+        The average vector readout includes 216 bps 
+        corresponding to six vectors per second. These vector readouts can be split between M1 and M2 in the ratios of 3:3, 5:1, or 6:0. 
+        The "Snap-Shot Memory" stores field vectors at the maximum sampling rate of 30 vectors per second and is read out at 48 bps. 
+        The FFT readout includes 17 seconds accumulation of vector data transformed into spectral matrices of the components and total magnitude at 
+        a transmission rate of 32 bps. 
+        
+        Prof. Norman F. Ness of the Bartol Research Institute at the University of Delaware is the MAG Experiment Manager.</Description>
       <Acknowledgement>Please acknowledge the ACE/MAG instrument team and the ACE Science Center</Acknowledgement>
       <Contact>
         <!-- N. Ness -->
@@ -22,6 +22,7 @@
             are used instead for the MOMENTS  production (see  Mode_DataOrigin_HEEA/LEEA).  Choices  on  the  best  way  to  combine  data  from  the  two 
             sensors can be made in the moments production software; in the first release the moments are made using LEEA data in the 
             energy overlap region. 
+            
             In some situations, use of both sensors together may be a better choice, for example in case
             s where the  distribution  changes 
             during  a  spin  as  the  method  can  resolve  time  aliasing  errors.  If  resources  allow,  the  Moments 
@@ -33,6 +34,7 @@
             using  default  values  to  control  the  approach  to 
             potential correction and photoelectron removal, and has not been systematically human
             - validated, so some errors may exist. 
+            
             Specifically, the spacecraft potential, Vsc, is set to be 1 V greater than the
             measured probe - spacecraft potential provided by 
             the electric field experiment (EFW) and the lower energy cutoff for the  moments
@@ -41,6 +43,7 @@
             may  also  contain  counts  due  to  spacecraft electrons). 
             Sometimes cold electrons are present which can appear in the same energy bin as the spacecraft photoelectrons, 
             therefore  both the  cold electrons and spacecraft photoelectrons are  removed resulting in underestimated electron densities. 
+            
             Recent  work
             by  the  EFW  team  suggests  a  more  accurate  determination  of  from  would  be  a  term  that  increases  linearly 
             above  ~10  V  (Cully  et  al.,  2007)  but  this  has  not  yet  been  
@@ -105,9 +105,6 @@
             <RenderingHints>
                 <DisplayType>TimeSeries</DisplayType>
             </RenderingHints>
-            <Structure>
-                <Size/>               
-            </Structure>
         </Parameter>
     </NumericalData>
 </Spase>