| LWS/Space Weather Effect |
 |
LWS/Geospace General Objective: |
| Satellite Systems |
The capability to monitor and predict energetic electron
and ion exposure is needed for diagnosis of satellite anomalies and consideration during spacecraft design.
(LWS program goal ranking 4) |
A |
A |
Priority 1: Understanding
the acceleration, global distribution, and variability
of energetic electrons and ions in the inner magnetosphere.
SAT report: WG1-5 and 6, WG2-4 |
| C |
|
NAV/Com/Rad Systems
|
The spatial distribution of electron density in the ionosphere
is the key environmental parameter impacting NavComRad systems.
(LWS program goal ranking 3) |
B |
B |
Priority
2A: Determine the effects of long and short-term
variability of the Sun on the global-scale behavior
of the ionospheric electron density.
SAT report: WG1-1, WG2-1 |
| E |
| Human Flight |
The capability to monitor and predict energetic electron
and ion exposure is needed to ensure the safety of
astronauts in Earth orbit and of flight crews of
high-altitude aircraft.
(LWS program goal ranking 2) |
C |
B |
Priority
2B: Determine the solar and geospace causes of
small-scale ionosphereic density irregularities in
the 100 to 1000 km altitude range.
SAT report: WG1-2, WG2-2 |
| Satellite Drag |
Neutral
density is the key environmental parameter determining
satellite drag.
(LWS program goal ranking 5) |
D |
C |
Priority
3A: Determine the effects of solar and geospace
variability on the atmosphere enabling an improved
specification of the neutral density in the thermosphere.
SAT report: WG1-3, WG2-3 |
| D |
| Ground Systems |
Enhanced ionospheric currents during geomagnetic storms induce
currents in ground-level conductors.
(LWS program goal ranking 6) |
E |
B |
Priority
3B: Understand how solar variability and the
geospace response determine the distribution of electric
currents that connect the magnetosphere to the ionosphere.
SAT report: WG1-4, WG2-5 |
| D |
| E |
| Global Climate Change |
The
effect of solar variability on ozone distribution
and on near-surface temperature change must be characterized.
(LWS program goal ranking 1) |
F |
A |
Priority
4: Determine the quantitative relationship between
very energetic electron and ion fluxes in the interplanetary
medium and their fluxes at low altitude, particularly
the geomagnetic cutoffs.
SAT report: WG1-9, WG2-6 |
| B |
| C |
| F |
| F |
Priority
5: Quantify the geospace drivers that potentially
affect ozone and climate.
SAT report: WG2-8 |
| LWS/Geospace General Objective |
|
Specific Objectives: |
Priority
1: Understanding the acceleration, global distribution,
and variability of energetic electrons and ions in
the inner magnetosphere.
SAT report WG1-5 and 6, WG2-4 |
|
Priority1:
1.1 — Differentiate among competing processes
affecting the acceleration and transport of outer
radiation belt electrons. |
Priority 2:
1.2a — Differentiate among competing processes
affecting precipitation and loss of outer radiation belt
electrons.
1.2b — Understanding the creation and decay
of new electron radiation belts.
1.2c — Develop and validate physics-based
data assimilation and specification models of outer radiation
belt electrons. |
Priority 3:
1.3a — Understand the role of "seed" or
source populations for relativistic electron events.
1.3b — Quantify the relative contribution
of adiabatic and nonadiabatic processes on energetic
electrons.
1.3c — Understanding the effects of the ring
current and other storm phenomena on radiation belt electrons
and ions. |
Priority 4:
1.4a — Understand how and why the ring current
and associated henomena vary during storms.
1.4b — Develop and validate physics-based
and specification models of inner belt protons for solar
cycle time scales. |
Priority
2A: Determine the effects of long and short-term
variability of the Sun on the global-scale behavior
of the ionospheric electron density.
SAT report: WG1-1, WG2-1 |
|
Priority1:
1A.1a — Quantify the relationship between
the magnitude and variability of the solar spectral
irradiance and the global electron density.
2A.1b — Quantify the effects of geomagnetic
storms on the electron density. |
Priority 2:
2A.2 — Quantify how the interaction between
the neutral atmosphere and the ionosphere affects the
distribution of ionosphere plasma. |
Priority 3:
2A.3 — Discover the origin and nature of
propagating disturbances in the ionosphere. |
Priority
2B: Determine the solar and geospace causes of
small-scale ionosphereic density irregularities in
the 100 to 1000 km altitude range.
SAT report: WG1-2, WG2-2 |
|
Priority 1:
2B.1 — Characterize and understand the origin
and evolution of newly-discovered storm-time mid-latitude
ionospheric irregularities. |
Priority
2:
2B.2a — Understand the conditions leading
to the formation of equatorial spread-F irregularities,
and their location, magnitude, and spatial and temporal
evolution.
2B.2b — Understand the conditions leading
to the formation of polar patches and their high latitude
irregularities. |
Priority
3:
2B.3 — Enable prediction of the onset, location,
and development of high latitude E-region irregularities. |
Priority
3A: Determine the effects of solar and geospace
variability on the atmosphere enabling an improved
specification of the neutral density in the thermosphere.
SAT report: WG1-3, WG2-3 |
|
Priority 1:
3A.1a — Determine the variability in the
neutral atmosphere attributable to the solar EUV spectral
irradiance.
3A.1b — Determine the variability in the
neutral atmosphere attributable to magnetospheric inputs. |
Priority
2:
3A.2 — Determine the variability in the neutral
atmosphere attributable to internal processes. |
Priority 3:
3A.3 — Determine the variability in the neutral
atmosphere attributable to atmospheric waves from below. |
