IMAGE Extreme UltraViolet (EUV) Imager, Modified Data 2 (M2), 10 min Data

https://doi.org/10.48322/xsb1-nc45

2023-07-30 12:34:56.789

The IMAGE extreme ultraviolet (EUV) imager detects resonantly scattered solar EUV photons with a wavelength of 30.4 nm that have been resonantly scattered by singly ionized helium (Sandel et al., 2000). The sizeable database of IMAGE global snapshots from the extreme ultraviolet (EUV) imager provides revolutionary observations of spatial and temporal plasma distributions throughout the plasmasphere. In this study, the IMAGE EUV data have been mapped to the equator using the approach detailed in Gallagher et al. (2005). IMAGE EUV data have been used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient in order to identify the magnetic local time, MLT, dependent plasmapause position as a function of time. This description has been adapted from text appearing in Katus et al. (2015).

Please acknowledge the Principal Investigator R.M. Katus for use of the Data

spase://VSPO/NumericalData/IMAGE/EUV/EquatorialMappedImages/ModifiedData/PT10M

Online

Open

CDF

None

Please acknowledge the Principal Investigator R.M. Katus. Please acknowledge the Data Providers and CDAWeb when using these Data.

Online

Open

CSV

Please acknowledge the Principal Investigator R.M. Katus. Please acknowledge the Data Providers and CDAWeb when using these Data.

PT10M

Epoch Time, TT2000

Epoch

Epoch Time Tags in Terrestrial Time 2000, TT2000

PT10M

ns

1.0e-9>s

1999-12-31T23:59:58.999995365

2006-01-01T00:00:00.000000000

9999-12-31T23:59:59.999999999

Plasmapause L-shell gradient, spectrogram

Time series defined by using: EPOCH

Plasmapause_MLTbin

Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, 48 MLT half hour bins, spectrogram format

PT10M

Re

6.3712e6>m

0.0001

20.0

-1.0e+31

Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, MLT noon down, dawn right

Time series defined by using: EPOCH

Mapped_Plasmapause_Grid

Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, MLT noon to the bottom, dawn to the right

PT10M

-32768

Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, MLT noon down, dawn left

Time series defined by using: EPOCH

Mapped_Plasmapause_Grid_flip_vert

Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left

This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Mapped_Plasmapause_Grid.

PT10M

-32768

Plasmapause L-shell gradient, from equatorial IMAGE EUV ion images, Movie

Time series defined by using: EPOCH

Mapped_Plasmapause_Grid_Movie

Plasmapause L-shell, sharpest gradient from IMAGE EUV ion image data mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left, Movie format

This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Mapped_Plasmapause_Grid.

PT10M

-32768

Plasmapause data quality index

Time series defined by using: EPOCH

Quality_Flag

Plasmapause data quality rating index: 1=Low, 2=Medium, 3=High

PT10M

1

3

-32768

Magnetic Local Time bins

MLTbin

Magnetic Local Time, MLT, 48 half hour bins

PT10M

h

3600>s

0.0

100.0

-1.0e+31

X-axis coordinates on the equatorial plane

X_Axis

X-axis coordinates on the equatorial plane, used to define the dependent grid

PT10M

Re

6.3712e6>m

-1.0e+31

Y-axis coordinates on the equatorial plane

Y_Axis

Y-axis coordinates on the equatorial plane, used to define the dependent grid

PT10M

Re

6.3712e6>m

-1.0e+31

IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn right

Time series defined by using: EPOCH

Equatorial_EUV_Grid

IMAGE EUV images mapped to the equatorial plane, MLT noon to the bottom, dawn to the right

PT10M

cm^-3

1.0e6>m^-3

-1.0e+31

IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn left

Time series defined by using: EPOCH

Equatorial_EUV_Grid_flip_vert

IMAGE EUV images mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left

This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.

PT10M

cm^-3

1.0e6>m^-3

-1.0e+31

IMAGE EUV images mapped to the equatorial plane, MLT noon down, dawn left, Movie

Time series defined by using: EPOCH

Equatorial_EUV_Grid_Movie

IMAGE EUV images mapped to the equatorial plane, flipped, MLT noon to the bottom, dawn to the left, Movie format

This parameter is virtual. It is calculated by calling the function ALTERNATE_VIEW_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.

PT10M

cm^-3

1.0e6>m^-3

-1.0e+31

IMAGE EUV images mapped to the equatorial plane, log scale, MLT noon down, dawn left

Time series defined by using: EPOCH

Equatorial_EUV_Grid_log

IMAGE EUV images mapped to the equatorial plane, log scale, flipped, MLT noon to the bottom, dawn to the left

This parameter is virtual. It is calculated by calling the function CONVERT_LOG10_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.

PT10M

log(cm^-3)

(log(cm^-3)+6)>log(m^-3)

-1.0e+31

IMAGE EUV images mapped to the equatorial plane, log scale, MLT noon down, dawn left, Movie

Time series defined by using: EPOCH

Equatorial_EUV_Grid_log_Movie

IMAGE EUV images mapped to the equatorial plane, log scale, flipped, MLT noon to the bottom, dawn to the left, Movie format

This parameter is virtual. It is calculated by calling the function CONVERT_LOG10_FLIP_VERT with the following input parameters: Equatorial_EUV_Grid.

PT10M

log(cm^-3)

(log(cm^-3)+6)>log(m^-3)

-1.0e+31