Wind Plasma and Radio Waves (WAVES) Time Domain Sampler (TDS) Dust Impact, Level 3, 1 s Data

https://doi.org/10.48322/635a-nc73

2021-05-31 12:34:56.789

Wind WAVES Time Domain Sampler, TDS, Dust Data File References: 1) Bougeret, J.-L., et al., WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Space Sci. Rev., 71, 231-263, 1995, doi:10.1007/BF00751331. 2) Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz, L.B. Wilson III, and K. Kersten, Interplanetary and Interstellar Dust observed by the Wind/WAVES Electric Field Instrument, Geophys. Res. Lett., 41, 266-272, 2014, doi:10.1002/2013GL058786. 3) Malaspina, D.M., and L.B. Wilson III, A Database of Interplanetary and Interstellar Dust Detected by the Wind Spacecraft, J. Geophys. Res., 121, 9369-9377, 2016, doi:10.1002/2016JA023209.

D.M. Malaspina, L.B. Wilson III, R.J. MacDowall, We would like to thank the Wind/WAVES team, especially Keith Goetz, Paul J. Kellogg, Kris Kersten, and Josh Lynch for their Support with Data Retrieval and Calibration. Please Cite or Reference the Wind WAVES Paper by J.-L. Bougeret et al., 1995 in Space Sci. Rev. and Work by D.M. Malaspina et al., 2014 in Geophys. Res. Lett., doi:10.1002/2013GL058786. We would also appreciate a Reference to the Wind Dust Impact Database Paper: D.M. Malaspina et al., 2016, in J. Geophys. Res., doi:10.1002/2016JA023209.

spase://VSPO/NumericalData/Wind/WAVES/DustImpact/PT1S

Online

Open

CDF

None

D.M. Malaspina, L.B. Wilson III, R.J. MacDowall, We would like to thank the Wind/WAVES team, especially Keith Goetz, Paul J. Kellogg, Kris Kersten, and Josh Lynch for their Support with Data Retrieval and Calibration. Please Cite or Reference the Wind WAVES Paper by J.-L. Bougeret et al., 1995 in Space Sci. Rev. and Work by D.M. Malaspina et al., 2014 in Geophys. Res. Lett., doi:10.1002/2013GL058786. We would also appreciate a Reference to the Wind Dust Impact Database Paper: D.M. Malaspina et al., 2016, in J. Geophys. Res., doi:10.1002/2016JA023209.. Please acknowledge the data providers and CDAWeb when using these data.

Online

Open

CSV

D.M. Malaspina, L.B. Wilson III, R.J. MacDowall, We would like to thank the Wind/WAVES team, especially Keith Goetz, Paul J. Kellogg, Kris Kersten, and Josh Lynch for their Support with Data Retrieval and Calibration. Please Cite or Reference the Wind WAVES Paper by J.-L. Bougeret et al., 1995 in Space Sci. Rev. and Work by D.M. Malaspina et al., 2014 in Geophys. Res. Lett., doi:10.1002/2013GL058786. We would also appreciate a Reference to the Wind Dust Impact Database Paper: D.M. Malaspina et al., 2016, in J. Geophys. Res., doi:10.1002/2016JA023209.. Please acknowledge the data providers and CDAWeb when using these data.

PT1S

Epoch, TT2000, Start of TDS Event

EPOCH

Epoch, Terrestrial Time 2000, TT2000, Start of Time Domain Sampler, TDS, Event

Time at Beginning of TDS Event as measured by the Minor Frame Clock. Thus, the Time Stamps have not been adjusted to correct for the Inherent Positive Definite Rounding Errors due to the Low Resolution of the Minor Frame Clock Times. This will be implemented in Future Versions when the Entire TDS Dataset is released on CDAWeb.

PT1S

ns

1e-9>s

1994-11-01T23:59:59.999999999

2044-11-01T23:59:59.999999999

9999-12-31T23:59:59.999999999

TDS Event Number

Time series defined by using: EPOCH

TDS_Event_Number

Time Domain Sampler, TDS, Event Number, Identifier for each Dust Impact

The TDS Event Number is a Unique Long Integer that identifies one Event from another. The Counter rolls over, so the Date and Event Number are required for Waveform Identification.

PT1S

0

99999999

-1

TDS Event Duration

Time series defined by using: EPOCH

TDS_Event_Duration

Time Domain Sampler, TDS, Event Duration

The Total Duration of each TDSF Event in Seconds. A single TDSF Event is defined as a Snapshot of two Electric Field Components with the same Event Number occurring on the Same Date. Most TDSF Events were sampled at 120000 Samples per Second, thus will have Durations of roughly 17 ms. However, the longest Duration Events can last upwards of about 1 s.

PT1S

s

0.015

1.3

-1.0e+31

Spacecraft Spin Rate

Time series defined by using: EPOCH

Wind_Spin_Rate

Spacecraft Spin Rate

The Spacecraft, SC, Spin Rate in '/s was determined by using the known Event Duration and Angle subtended during each TDS Event. This Value is accurate to much less than 1', where the Uncertainties arise from the Onboard Sample Rate Clock of the TDS Receiver and Sun Pulse Detector Time Accuracy. The Spin Period in Seconds was then determined by using 360' divided by the Spin Rate Value. Both Values assume that the Spin Rate and Spin Period are constant during the TDS Event, which should be an accurate Assumption for nearly all Events.

PT1S

°/s

0.0174532925>rad/s

0.0

360.0

-1.0e+31

Spacecraft Spin Period

Time series defined by using: EPOCH

Wind_Spin_Period

Spacecraft Spin Period

The Spacecraft, SC, Spin Rate in '/s was determined by using the known Event Duration and Angle subtended during each TDS Event. This Value is accurate to much less than 1', where the Uncertainties arise from the Onboard Sample Rate Clock of the TDS Receiver and Sun Pulse Detector Time Accuracy. The Spin Period in Seconds was then determined by using 360' divided by the Spin Rate Value. Both Values assume that the Spin Rate and Spin Period are constant during the TDS Event, which should be an accurate Assumption for nearly all Events.

PT1S

s

0.0

5.0

-1.0e+31

Peak Amplitude, Channel 1

Time series defined by using: EPOCH

Ch01___Peak_amplitude

Peak Amplitude, Channel 1

The Peak Amplitude of the Electric Field Component from the Dust Impact. This is the Peak Amplitude measured during a TDSF Event on both Antenna. This is a Signed Value, that is, Plus, +, or Minus, -. The X-Antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective Antenna Lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-Antenna, Y-Antenna, and Z-Antenna, respectively, for all Dust Impacts. We have removed these Antenna Length Dependencies, which is why the Amplitude Units are in mV.

PT1S

mV

1e-3>V

-20000.0

20000.0

-1.0e+31

Cross-Correlation Value, Channel 1

Time series defined by using: EPOCH

Ch01___cc_value

Cross-Correlation Value, Channel 1

The Cross-Correlation Value between the Channel 1 Waveform and the Normalized Median Waveform of a given Morphological Type, e.g., See Malaspina and Wilson, (2016) for Morphological Type Definitions.

PT1S

0.0

1.0

-1.0e+31

Cross-Correlation Threshold Value, Channel 1

Time series defined by using: EPOCH

Ch01___cc_threshold

Cross-Correlation Threshold Value, Channel 1

The Cross-Correlation Threshold Value for the Channel 1 Waveform used. The Overall Cross-Correlation Threshold is 0.8 but Morphological Types C, D, and M are required to exceed 0.9.

PT1S

0.0

1.0

-1.0e+31

Event Selection Threshold Amplitude, Channel 1

Time series defined by using: EPOCH

MinCh1_threshold

Event Selection Threshold Amplitude, Channel 1

The Minimum Channel 1 Absolute Amplitude required for Event Selection. The X-Antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the Effective Antenna Lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-Antenna, Y-Antenna, and Z-Antenna, respectively, for all Dust Impacts. We have removed these Antenna Length Dependencies, which is why the Amplitude Units are in mV.

PT1S

mV

1e-3>V

0.0

100.0

-1.0e+31

Average Clockwise Angle of the Closest Ex Antenna to the Dust Impact from the Earth-Sun Line

Time series defined by using: EPOCH

Ch1ImpAnt_E_S_Angle

Average Clockwise Angle of the Closest Ex Antenna to the Dust Impact on the Spacecraft Bus from Earth-Sun Line, roughly GSE +X, Channel 1

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

-360.0

360.0

-1.0e+31

Peak Amplitude, Channel 2

Time series defined by using: EPOCH

Ch02___Peak_amplitude

Peak Amplitude, Channel 2

The Peak Amplitude of the Electric Field Component from the Dust Impact. This is the Peak Amplitude measured during a TDSF Event on both Antenna. This is a Signed Value, that is, Plus, +, or Minus, -. The X-Antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective Antenna Lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-Antenna, Y-Antenna, and Z-Antenna, respectively, for all Dust Impacts. We have removed these Antenna Length Dependencies, which is why the Amplitude Units are in mV.

PT1S

mV

1e-3>V

-20000.0

20000.0

-1.0e+31

Cross-Correlation Value, Channel 2

Time series defined by using: EPOCH

Ch02___cc_value

Cross-Correlation Value, Channel 2

The Cross-Correlation Value between the Channel 2 Waveform and the Normalized Median Waveform of a given Morphological Type, e.g., See Malaspina and Wilson, (2016) for Morphological Type Definitions.

PT1S

0.0

1.0

-1.0e+31

Cross-Correlation Threshold Value, Channel 2

Time series defined by using: EPOCH

Ch02___cc_threshold

Cross-Correlation Threshold Value, Channel 2

The Cross-Correlation Threshold Value for the Channel 2 Waveform used. The Overall Cross-Correlation Threshold is 0.8 but Morphological Types C, D, and M are required to exceed 0.9.

PT1S

0.0

1.0

-1.0e+31

Event Selection Threshold Amplitude, Channel 2

Time series defined by using: EPOCH

MinCh2_threshold

Event Selection Threshold Amplitude, Channel 2

The Minimum Channel 2 Absolute Amplitude required for Event Selection. The X-Antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the Effective Antenna Lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-Antenna, Y-Antenna, and Z-Antenna, respectively, for all Dust Impacts. We have removed these Antenna Length Dependencies, which is why the Amplitude Units are in mV.

PT1S

mV

1e-3>V

0.0

100.0

-1.0e+31

Average Clockwise Angle of the Closest Ey Antenna to the Dust Impact from the Earth-Sun Line

Time series defined by using: EPOCH

Ch2ImpAnt_E_S_Angle

Average Clockwise Angle of the Closest Ey Antenna to the Dust Impact on the Spacecraft Bus from the Earth-Sun Line, roughly GSE +X, Channel 2

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

-360.0

360.0

-1.0e+31

Average Clockwise Angle of +Ex Antenna from the Spacecraft-Sun Line

Time series defined by using: EPOCH

Pos_Ax_SCS_Angle

Average Clockwise Angle of +Ex Antenna from the Spacecraft-Sun Line

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

-360.0

360.0

-1.0e+31

Average Clockwise Angle of +Ex Antenna from the Earth-Sun Line

Time series defined by using: EPOCH

Pos_Ax_E_S_Angle

Average Clockwise Angle of +Ex Antenna from the Earth-Sun Line, roughly GSE +X

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

-360.0

360.0

-1.0e+31

Average Clockwise Angle of +Ey Antenna from the Earth-Sun Line

Time series defined by using: EPOCH

Pos_Ay_E_S_Angle

Average Clockwise Angle of +Ey Antenna from the Earth-Sun Line, roughly GSE +X

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

-360.0

360.0

-1.0e+31

Average Clockwise Angle of +Ex Antenna from the Earth-Sun Line, Uncertainty

Time series defined by using: EPOCH

Pos_Ax_E_S_Delta_Angle

Average Clockwise Angle of +Ex Antenna from the Earth-Sun Line, roughly GSE +X, Uncertainty

The Angle accounts for the XY-GSE Displacement of Wind but assumes Earth remains at exactly 1 AU always. The Error introduced by not including the Change of the Earth's Radial Position throughout its annual Orbit is less than ~0.017°. The Error introduced by not including the Change of the Spacecraft's Out-of-Ecliptic Displacement is less than ~0.0018°. The Spacecraft, SC, Spin Axis is aligned within ~0.8° of the South Ecliptic Pole. This varies annually due to the Differences in Torque applied to the SC Bus by Solar Radiation. The Angle can be as low as 0.1°. We define Clockwise (CW) Angles as being less than zero for CW Rotations to remain consistent with Euler Angle Notation. We define CW as viewed from the North Ecliptic Pole looking down upon the XY-GSE Plane. All Angles herein vary from 0° to 360°, Absolute Values, thus a positive Counter-Clockwise Angle corresponds to a Clockwise Angle plus 360° that is greater than 0°. The Impact Antenna Angle depends upon the closest Impact Antenna, defined by the CDF Variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An Example Image illustrating the various Angles within these CDF Files can be found in the Malaspina and Wilson, 2016.

PT1S

°

0.0174532925>rad

0.0

360.0

-1.0e+31

Average Clockwise Angle of the E[x,y] Impact Antenna from the Earth-Sun Angle, Uncertainty

Time series defined by using: EPOCH

ImpAnt_E_S_Delta_Angle

Average Clockwise Angle of the E[x,y] Impact Antenna from the Earth-Sun Angle, roughly GSE +X, Uncertainty

The Impact Angle Uncertainties are mostly controlled by the Quadrant or Hemisphere in which the Dust Impact occurred. This is true for the Ch1ImpAnt_E_S_Angle and Ch2ImpAnt_E_S_Angle. This is roughly ±45°, i.e., Quadrant, for all Events. For the other Sun Angles, that is, Pos_Ax_SCS_Angle, Pos_Ax_E_S_Angle, and Pos_Ay_E_S_Angle, the Uncertainty is controlled by the Spin Rate of the Spacecraft as determined by Event Duration and Angle subtended during an Event multiplied by the TDSF Event Duration plus the DPU Clock Latency Uncertainty, i.e., about 10.6 ms. Thus, this Uncertainty is currently less than 13° for the Worst Case Scenario with Fastest Spin Rate and Slowest Sampling Rate. In the Best Case Scenario and for most Events, the Uncertainties drop to ~3°.

PT1S

°

0.0174532925>rad

0.0

360.0

-1.0e+31