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Times
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Authors (*Presenter)
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Abstract
Title and Summary
|
|
11:00
a.m.
|
|
Introduction
|
|
11:15 a.m.
|
Futaana Y. * Dandouras I. Bamford R. A. Bergman J. Beth A. Chaufray J. Y. Constantinescu D. Della Corte V. Grison B. Jarvinen R. Nakamura R. Postberg F. Ranvier S. Roussos E. Vorburger A. H. Götz C. McDonald F. Taylor M.
|
Space Plasma
Physics Science Opportunities from the Moon Surface [#1035]
In preparation for the scientific
opportunities offered by the Deep Space Gateway, including from the Moon
surface, we have formed an ESA topical team to prepare and to support the
definition of payload studies in the field of space plasma physics.
|
|
11:30
a.m.
|
Dobynde M. I. * Guo J.
|
The REDMoon
Model: Radiation Environment and Dose
Rates on the Lunar Surface and Subsurface [#1012]
We
present a recently developed and validated model of the radiation environment
at the surface and subsurface of the Moon created with the Galactic Cosmic
Rays and Solar Energetic Particles. The model provides angular
and energy differential spectra of primary space radiation particles and
secondary particles induced in the lunar soil. The model covers the range of
depths from the surface down to 10 m and provides information on the
directionality of radiation particles. Also, the model provides spectra of
the albedo radiation from the lunar surface. Particle-matter interaction is
calculated using the GEANT4 Monte-Carlo code. The model is built using the
concept of response function and allows calculation of the radiation
environment for any input GCR or SEP spectrum without running time-consuming
modelling. We have used the predicted radiation environment during the last
two solar cycles to create a schedule of lunar expeditions that would allow a
persistent presence of humans on the Moon. We give the number of crews and
flights required in scenarios with different depths, aluminum
extra-shielding, and exposure limits.
|
|
11:40 a.m.
|
Freeman R. H. *
|
Artemis Base
Camp: Resilience Engineering to Enable
Lunar Surface Operations [#1021]
This paper explores current shielding and
sensor technologies needed to protect and monitor the health of lunar
missions involving astronauts, autonomous rovers, mobile habitats, ISRU
equipment, and facilities. Exposed to solar wind plasma, GCRs, and secondary
radiation due to the lack of a magnetosphere or a dense atmosphere. Sparse
regional mini-magnetospheres don’t spare the intense space weathering of the
Moon’s regolith-covered surface nor exposure risk to mission operations. The
paper further considers low gravity and levitated dust particles in how
resilience engineering of lunar material science may be developed. The
combination of small dust particles, electric potentials plus micrometeorites
can lead to lunar regolith being levitated, and levitation is likely to
increase with human activity on the Moon. Levitated dust particles may settle
and accumulate on hardware which may result in potential degradation of
radiative heat transfer and optical components through the fouling of
surfaces, visibility reduction during extravehicular activities, dust
contamination of equipment, and prevention of effective sealing.
|
|
11:50
a.m.
|
Iles G. N. * Ng M. X. J. Moshovelis L. D. Auld M. Currie J. Carter B.
|
“RADICAL-S” an Active
Radiation Shield Flying on the Swedish Space Corporation
Sub-Orbital Express [#1003]
NASA’s
Artemis program aims to establish a long-term human presence on the Moon by
2024, in preparation for further space exploration to Mars. However, for this
to be possible, suitable materials for spacecrafts and planetary habitats
need to be developed to shield humans against the harmful radiation in space.
The Space Physics Research Group at RMIT is researching radiation shielding
for use on the Artemis missions. We have built shielding prototypes utilizing
both passive and active shielding. The 1U payload, “RADICAL-S” (Radiation
Deflector of Ionising Charges using a Lorentz
Shield) consists of an electromagnetic shield and an instrument suite of
sensors. Bench testing and modelling of the shield have been conducted
in-house and the instrument suite comprised of a magnetometer, Geiger
counter, and GPS receiver have been successfully connected and programmed.
The payload will be launched by the Swedish Space Corporation late 2022 on
the Sub-Orbital Express sounding rocket to test the effectiveness of the
shield at 250km altitude.
|
|
12:00 p.m.
|
Xu S. * Poppe A. R. Harada Y. Halekas J. S. Chamberlin P. C.
|
Lunar
Photoemission Yields Inferred from ARTEMIS Measurements [#1027]
Photoemission yield (the number of emitted
electrons per incoming photon) is one of the fundamental properties of solid
materials but is not yet well constrained for the lunar surface for photon
energies >~20 eV. In this study, we constrain this yield for incident
photons with energies of ~10 - 500 eV with data from the ARTEMIS mission
along with solar irradiance spectra from Version 2 of the Flare Irradiance
Spectral Model (FISM2). We also report the first oxygen Auger electron
observations at the Moon by the ARTEMIS spacecraft, which provides a unique
feature to identify photoelectrons emitted from the lunar surface. With lunar
photoelectron observations identified in both Earth’s magnetotail lobes and
the solar wind for four selected days, we infer a lower bound of 10–3
in yield for photon energies >~20 eV. However, our investigation also
reveals uncertainty over ~4 orders of magnitude in derived yields with a
sensitivity study, owing to a poorly constrained photoelectron energy
probability function. This uncertainty motivates future experiments on lunar
samples to better characterize the lunar surface charging environment.
|
|
12:10
p.m.
|
|
BREAK
|
|
Times
|
Authors (*Presenter)
|
Abstract
Title and Summary
|
|
12:30
p.m.
|
Farrell W. M. * Zimmerman M. I. Rhodes D. J. Killen R. M. Sarantos M. Halekas J. S. Stubbs T. J. Poppe A. R.
|
The Complex Plasma
Environment at the Wake Formation Region Along the Terminator [#1008]
The
Moon is an obstacle in the solar wind, creating a downstream wake region. The
wake initiation region is located along the terminator annulus that belts the
Moon. In this region, a plasma-vacuum discontinuity forms in association with
flow obstruction by local topography (mountains, craters). The discontinuity
evolves downstream via an ambipolar (E-driven) plasma expansion that includes
a reduction in near-surface plasma flux, negative plasma potentials, and
large negative surface potentials in shadowed regions adjacent to the terminator.
This ambipolar region has been directly measured by orbiting spacecraft.
However, there are no surface measurements where the discontinuity first
forms. Analytical and PIC models of the discontinuity evolution have been
developed by the SSERVI/DREAM2 and LEADER teams, and these will be reviewed
herein. One consequence of the low plasma flux expected in downstream
shadowed regions is that systems walking, roving, or drilling may develop a
charge build-up due to triboelectric contact with the regolith. We emphasize
the need for landed electron and ion spectrometers at the terminator/poles to
quantify the flux levels associated with wake formation.
|
|
12:45 p.m.
|
Kallio E. * Jarvinen R. Nyman L. Knuuttila O.
|
On the
Properties and Effects of the Near Lunar Surface Plasma, Electric and
Magnetic Fields, and Charged Dust Particles [#1013]
Lunar surface is under a continuous impact
by the solar wind, i.e., electrically charged particles from the Sun. The
impacting charged particles have many consequences on the surface and above
it. Especially, the particle precipitation, together with Sun’s extreme
ultraviolet radiation, charges the lunar surface, as well as man-made devices
on it, electrically. The formed electric field can, in turn, accelerate
electrically charged dust particles near the surface, which can cause hazards
for manned missions and the malfunction of human-operated and robotic
systems. Other detrimental effects on thermo-optical coatings and systems
utilizing thin-film membranes could occur. In this presentation, we describe
different numerical simulations developed and used at the Aalto University,
to investigate lunar electric, plasma and dust environment at various spatial
and temporal scales, different phases of the Moon, at different latitudes and
longitudes on the lunar surface, as well as magnetized and non-magnetized
regions. We also address the issue of how risks of the lunar dust on humans
and man-made devices can be reduced by appropriate technological design.
|
|
12:55
p.m.
|
Xu Z. * Guo J. Wimmer-Schweingruber R. F. Dobynde M. I.
|
Primary and Albedo Protons
Measured by the Chang’E 4 Lunar Lander Neutron and Dosimetry (LND) Experiment
on the Lunar Far Side [#1010]
The
Lunar Lander Neutron and Dosimetry (LND) Experiment aboard the Chang’E-4
Lander on the lunar far side surface measures energetic charged particles and
monitors the corresponding radiation level. The charged particles have two
main sources, solar energetic particles (SEPs) and galactic cosmic rays
(GCR), which dominate during solar quiet times. We present LND measurements
of GCR primary and secondary protons. Apart from the GCR primary protons, LND
also measures the albedo protons from a limited field of view. These albedo
protons are secondary particles that are generated when the GCR interacts
with the lunar regolith. LND provides measurements of the upward-directed
albedo protons between 64.7 MeV and 76.0 MeV. The average albedo to primary
ratio of proton fluxes in this energy channel from 2019.7 (the 7th lunar day
after Chang’E-4’s landing) to 2020.6 (the 20th lunar day) is around
0.64+-0.09, and the averaged albedo flux is about (1.12+-0.14)×10-4
cm-2sr-1 s-1 Mev-1. These results are consistent with the albedo flux
predicted from the Lunar Subsurface Radiation Model (Dobynde
et al 2021).
|
|
1:05 p.m.
|
Tucker O. J. * McLain J. L. Morrissey L. S. Farrell W. M. Killen R. M. Honniball C. I. Hurley D. M.
|
Investigations
on Solar Wind Implantation in the Lunar Regolith and Volatile Stability [#1016]
Solar wind implantation (SWI) is an
important source of volatiles for planetary bodies without significant
outgassing such as the Moon. However, the surface chemistry of minerals
induced by SWI, and the degassing of newly formed volatiles is not
understood. Lunar based experiments offer a unique vantage point needed to
constrain surface properties for porous silicate minerals. Of special
interest is SWI leading to the chemical formation of OH, H2, H2O,
and CH4, observed in the regolith and exosphere. Hydrogenated species
are predicted to vary with SWI, but direct observations linking SWI to the
variability of H-bearing molecules are sparse. A goal of the Lunar
Environment And Dynamics for Exploration Research
(LEADER) center is to understand the effect of SWI on the Moon’s surface and
volatile stability. I will review SWI [4] and recent work by LEADER
scientists on models [1–2] and experiments [3] used to examine H diffusion
and H-bearing molecules in the exosphere, including discussion of potential
lunar experiments to constrain this process. 1)Farrell, W.M. et al. JGR,
2017. 2)Tucker, O.J. et al. JGR, 2021. 3)McLain, J.L. et al. JGR, 2021.4)Starukhina, L.V. Adv. Sp.
Res, 2006.
|
|
1:15
p.m.
|
Morrissey L. S. * Killen R. M. Tucker O. J. Savin D. W.
|
Solar-Wind Induced Sputtering
on the Lunar Surface: Quantifying
Mineral Specific Surface Binding Energies [#1018]
Lunar
surface sputtering by solar wind (SW) ion irradiation is important for
understanding the Moon’s surface and exosphere compositions. A fundamental
physical parameter for theoretical sputtering models is the surface binding
energy (SBE) of atoms in the substrate. Despite the clear importance of the
SBE in simulating sputtering, its actual value is not well understood for
many substrates. For single component substrates, the SBE is often
approximated as the heat of sublimation for the atoms in the substrate.
However, there is no universal approach to estimating the SBE for
multicomponent substrates, with studies often assuming the SBE is constant
regardless of the substrate composition. We use molecular dynamics (MD)
simulations to quantify the SBE Na and O from various silicates and
demonstrate that the elemental SBE is instead a mineral specific value. The
MD SBE values are ~8 times larger than mono-elemental cohesive energies. This
has a significant effect on the predicted SW ion sputtering yield and energy
distribution of sputtered atoms. Therefore, future studies on the
contributions of SW-surface interactions should instead be using mineral
specific SBEs.
|
|
1:25 p.m.
|
|
BREAK TO THE
POSTER SESSION
|
|
Authors
|
Abstract
Title and Summary
|
|
Goswami V. K.
|
Development of Lunar
Mass-Energy Equation to Study Dynamics of Lunar Environment to Explore Life
on Moon Through the Detoxification of Lunar Toxins [#1001]
|
|
Schorghofer N.
|
Constraints on
the Past Solar Constant from Lunar Borehole Temperatures [#1004]
Accurately measured borehole temperatures
provide constraints on past surface temperatures. On Earth, borehole
temperatures have been used to reconstruct the surface temperature history
over the past several centuries [1]. Implementation on the Moon would provide
constraints on the history of the total solar irradiance (TSI). Direct
measurements of the TSI are available only since 1978. Miyahara et al. [2]
have explored this method for the lunar surface. A difference of 0.1% in TSI
during the Maunder minimum would correspond to a 0.01 K deviation at about 10
m depth [2]. Such a measurement should be feasible and could be combined with
an experiment for the geothermal heat flux. The temperature sensitivity is
greatest at the equator and smallest at polar latitudes [2]. Borehole
temperatures from multiple latitudes can potentially reduce uncertainties.
Caves provide access to greater depths. Thermometers can be inserted into
horizontal borings to reach undisturbed rock temperatures, as has been done
in underground mines [1]. Works Cited: [1] Pollack HN & Huang S (2000)
Ann. Rev. Earth Planet. Sci. 28, 339. [2] Miyahara H et al. (2008) Geophys. Res. Lett. 35, L02716.
|
|
Kroupa M.
|
Advanced, Modular, Scalable,
Space-Time Agnostic, Continuous Power Generation for Mobility and Derivative
Applications [SP] [#1009]
NASA
seeks solutions for low-cost lunar exploration and maximizing resource
utilization while minimizing energy use and mass of equipment required to be
transported to the Moon. Same holds true for inner and outer planet
exploration and beyond, all of which share common hurdles [as missions will
show]. The common underlying challenge of first order is the supply of energy
which ℕ𝔽𝕋𝔾 solves in a simple,
readily available solution by leveraging current technologies, physics and ℕ𝔽𝕋𝔾’s innovations. The
groundbreaking concept gives rise to high efficiency power system [300-500%
increase] solutions for low-cost power generation and structure or equipment
operation including long range lunar terrain vehicles (LTV) and atmospheric
mobility systems (LAV). The versatility and scalability of the modular high
‘specific power and energy’ components allows relatively unconstrained
exploration of the surface or sub-surface despite geographic location or
solar energy flux. The derivative components and constellation of synergistic
systems are rapidly implemented anywhere early on in missions with no
supporting infrastructure required.
|
|
Vines S. K.
Anderson B. J.
Regoli L.
Harden B. Hood L. Tikoo S. Weiczorek M. Blewett D. T. Halekas J. Ho G. C. Greenhagen B.
|
Lunar Vertex
Vector Magnetometers: Revealing the
Surface Magnetic Structure of the Lunar Magnetic Anomaly at Reiner Gamma [#1014]
The first Payloads and Research
Investigations on the Surface of the Moon (PRISM-1a) lander mission (flight
in 2024) targets the Reiner Gamma (RG) swirl and magnetic anomaly. To study
the anomaly and the relationship of the “mini-magnetosphere” to albedo
variations, the Lunar Vertex investigation will carry a suite of
science-grade and commercial fluxgate magnetometers on the lander (VML) and
on a rover (VMR). Measurements during descent by VML and during surface
operations by both VML and VMR will characterize the altitudinal variation
and surface magnetic field across contrasting albedo regions of a strong
magnetic anomaly. These measurements will constrain the orientation,
strength, and depth of the source of the RG magnetic anomaly, allowing us to
infer its most likely origin and also determine the
relationship between the magnetic field, the swirl, and surface space
weathering. Characterization of the surface strength and structuring of the
RG anomaly by VML and VMR is also vital for understanding interactions with
the space plasma environment and electromagnetic processes occurring on and
near the lunar surface which may impact future surface activities.
|
|
Jahn J.-M. Halekas J. S. Ho G. C. Kollmann P. Fatemi S. Hood L. L. Vines S. K. Blewett D. T. Mokashi P. S. Focia R. J. Gomez R. G.
|
Lunar Vertex Magnetic Anomaly
Particle Spectrometer (MAPS) — Studying the Charged Particle Impact on the
Lunar surface Inside the Reiner Gamma Magnetic Anomaly [#1015]
The
Reiner Gamma (RG) magnetic anomaly is the target for the first Payloads and
Research Investigations on the Surface of the Moon (PRISM) lander delivery
(PRISM-1a), planned for 2024. As part of the PRISM-1a Lunar Vertex
investigation, the MAPS plasma spectrometer measures the energy, flux, and
direction of thermal to supra-thermal (10eV to ~20keV) ions and electrons
from the impinging solar wind that reach the lunar surface. MAPS determines
how effectively the surface is shielded from this plasma by quantifying the
amount of flux that is excluded (reflected or deflected) from the surface in
strongly magnetized regions. This differentiates between a protective mini-magnetosphere where the solar wind is largely
excluded, and an extended boundary layer where the solar wind is merely
decelerated close to the surface. MAPS data are used to deduce the relative
roles of electrostatic fields and wave-particle interactions, and electron
pitch angles are used to diagnose the anomaly’s magnetic topology. MAPS
measurements of the shielding from impinging plasma inside Reiner Gamma will
have implications for our understanding of surface weathering and the
formation of lunar swirls.
|
|
Vidmachenko A. P. Steklov A. F.
|
The Moon Needs
to be Turned into a Testing Ground for Development of Thermal and
Gravitational Adaptation Systems for Terraforming Planets [#1006]
Humanity needs to work out method of
habitation and long-term life of people on planets, planetoids, and in space
in general. Due to significant radiation, habitation bases must be located
below surface, or in massive planetoid structures [Morozhenko,
Vidmachenko (2004) JAIS, 36(11), 27]. We propose
that it is necessary to place person under Moon surface. It is there that
most suitable option in order to protect astronauts
from extreme temperatures and radiation [Steklov & Vidmachenko
(2020) 22 ISC ASYS, Kyiv, 84]. For this, it is necessary to develop a special
technology for rapid construction of premises directly below surface for
housing and industrial purposes [Steklov et al. (2019) Lunar ISRU 2019, 2152,
id. 5107]. It is necessary to develop projects to turn Moon into special
testing ground for the deployment and testing of systems for gravitational
and thermal adaptation and terraforming of planets and planetoids of
different scales. Such systems are required to provide reliable thermal and
gravitational adaptation for long-term residence of people there. In case of
successful adaptation to the Moon, terraforming Mars, Mercury, and other
planetoids will be much easier task.
|
|
Abdelaal M. E. Zakharov A. V. Kuznetsov I. Inna
Anton Lyash A.
|
Investigate the Dynamics of
Dust Particles Under the Airless Bodies’ Conditions to Study the Lunar
Horizon Glow [#1007]
The aim
of this research was to investigate and improve the measurement technique for
determining the trajectory parameters of dust particles. One of the benefits
of this technique is that it can accommodate limited optical access to the
investigation volume by using low-speed cameras and lasers with limited
power. The developed technique was used to visualize dust particle levitation
with particles of various sizes and materials. The ability to measure
particle velocities and charges was facilitated by the ability to determine
3D trajectories of levitated particles. These parameters will be useful in
future experiments involving the modeling of dust plasma levitation. The
previous experiments in the same area and the numerical findings from these
experiments agree well. The use of a stereo camera device, on the other hand,
represents a significant advancement in assessing 3D particle levitation
trajectories. This method increases the measurement precision of quantitative
values, allowing the theoretical models of the near-surface dynamics of atmosphereless bodies to be refined. Our method will be
used to analyze data collected during future lunar missions.
|
|
de Nolfo G.-A. Bruno A. Daehn M. Dumonthier J. Legere J. Messner R. Mitchell J.-G. Ryan J.-M. Suarez G. Tatoli T. Williams L.
|
Neutron
Measurements on the Moon [#1011]
Lunar scientific outposts offer an
opportunity to advance human exploration of space, while serving as both a
platform for industrial and scientific research and a gateway to more distant
locations. Neutrons can play a significant role in lunar exploration and the
science of the Moon and Sun. Specifically, fast neutrons are an egregious
form of radiation for crew and avionics. Broadband neutron spectroscopy
(covering thermal, epithermal, and fast neutrons) can also serve as an
effective probe of regolith composition and in situ resource utilization,
including the localization of water-ice. A lunar platform is invaluable for
measuring neutrons originating from the Sun. Neutrons constitute a critical
missing piece in understanding the production mechanisms of energetic
particles at the Sun and the harmful space weather events spawned by such
particles. A lunar-based solar neutron observatory would benefit from the
long lunar day, with uninterrupted extended observations of the Sun,
resulting in an excellent duty cycle for solar measurements. Key benefits of
neutron spectroscopy on the Moon and a review several neutron spectrometers
currently being developed by our team is discussed.
|
|
Waller C. D. Cahill J. T. S. Meyer H. M.
|
Modeling Temporal Variations
in Solar Wind Conditions at Reiner Gamma:
Preparations for Lunar Vertex [#1022]
While
the Moon presently lacks a dynamo, the crust contains localized magnetic
anomalies (MAs), many of which are correlated with lunar swirls. The swirl
Reiner Gamma and its associated MA will be visited in 2024 by the Lunar
Vertex (LVx) mission, carrying two vector
magnetometers. Similar to Earth’s magnetosphere, MAs
are compressed by the dynamic solar wind ram pressure which establishes
“mini-magnetospheres” where crustal magnetic pressure is equal to or greater
than the ram pressure. The targeted LVx landing
site and traverse path were not optimized to sample the MA, but rather to
examine spectral signatures thought to be a result of the MA influence. Based
on current launch and orbital estimates, LVx will
cross the bow shock and magnetopause boundaries once, observing lunar MA
interactions with Earth’s magnetosphere and lunar mini-magnetosphere formation.
LVx will observe the MA under varying ram pressure
and record the surface field responses and we predict the lander and MAPP-C
rover will operate beneath a potential mini-magnetosphere. Understanding this
dynamic environment will inform future exploration as well as improve surface
models from orbital magnetic data inversion.
|
|
Wu X.
|
Mini.PAN: Real-Time Penetrating Particle Analyzer
for ARTEMIS [#1032]
Mini.PAN is an innovative energetic particle detector to precisely
measure and monitor the flux and composition of highly penetrating particles
(> ~100 MeV/nucleon) in the lunar orbit and on the lunar surface in the
framework of the ARTEMIS program.
|
|
Rahmanifard F. R. Schwadron N. A. Wilson J. K. Jordan A. P. Spence H. E. de Wet W. C.
|
Realtime Monitoring of
Ionizing Radiation on the Lunar Surface in the Upcoming Worsening
Space Environment [#1034]
The
unprecedented decline in the strength of solar cycles has been persisting
over a decade, indicating that we are at the beginning of a secular solar
minimum. We use data from CRaTER to investigate the
radiation environment throughout cycle 25.
|
|
Saxena P.
|
Tracking
Evolution of the Sun Using Multiple Lines of Evidence that are Accessible on
the Lunar Surface [#1024]
How the Sun may have varied over time is key
to understanding how the solar system evolved. Evidence from solar analogues
suggests the Sun likely had a changing rotation rate and consequently
changing properties over time. These properties include flux, space weather
properties, and the morphology of the heliosphere. These are fundamental to
understanding how atmospheres, surfaces, and habitability of bodies in the
solar system may have been effected by the Sun over
time. Future human presence on the lunar surface as part of exploration
efforts offers a powerful means by which to potentially constrain the
evolution of the Sun. Multiple lines of evidence accessible from the lunar
surface through both spatial variations and stratigraphy are key to this
understanding. Variations in chemical abundances, isotopic fractionation and
other proxies can put limits on space weather properties, UV flux, and GCR
flux — all of which will inform the extent to which the Sun changed
over time.
|
|
Poppe A. R. Fillingim M. O. Xu S. Halekas J. S. Barani M.
|
Distinguishing Atomic and
Molecular Terrestrial Ionospheric Fluxes to the Lunar Surface
with HERMES [#1025]
Previous
measurements by the THEMIS-ARTEMIS spacecraft in orbit around the Moon were
suggested to be outflowing terrestrial ionospheric molecular ions (e.g., N2+,
NO+, O2+). However, the THEMIS-ARTEMIS ElectroStatic
Analyzers lack ion composition discrimination and thus, a definitive
identification of these events as either atomic O+ or molecular ions was not
possible. The HERMES SPAN-ion electrostatic analyzer has moderate mass
resolution capable of distinguishing atomic versus molecular species.
Monitoring and investigation of these outflows, including comparison with
concurrent THEMIS-ARTEMIS measurements, will reveal the true composition of
these ions. Compositional knowledge of these outflowing terrestrial
ionospheric fluxes is critical for lunar surface science, including accurate
calculations of surface weathering and sputtering rates, and the
implantation–and potential archiving–of terrestrial ionospheric material
within lunar regolith that can be accessed and returned to Earth for study by
astronauts on the lunar surface.
|
|
Vandegriff J. D. Weigel R. S. Candey R. Roberts D. A. Thomas B.
|
Using Heliophysics Data Environment Technologies and Standards
for Lunar Research Data [#1028]
NASA’s lunar push will generate new datasets
relevant for Heliophysics and understanding space
weather impacts in lunar environments is critical for the success of human
exploration. Integrating new data within the Heliophysics
data environment will simplify the use of this data for space weather
studies. Many communities contributing to lunar missions come from planetary
or commercial space realms and may not be familiar with Heliophysics
data practices. We give an overview of techniques that could make lunar data
accessible to both planetary and Heliophysics
research. Three items are important for interoperability: metadata, data format, and data access
protocols. The SPASE metadata model allows all Heliophysics
datasets to be registered uniformly. The Common Data Format (CDF, see
https://cdf.gsfc.nasa.gov) is approved for use at both Heliophysics
and planetary archives. The Heliophysics
Application Programmer’s Interface (HAPI, see Weigel, 2021,
do:10.1029/2021JA029534) is a standard for serving time series data. Finally,
there are emerging cloud-based analysis systems within Heliophysics
that can assist with data-model comparisons for large volume datasets.
|
|
Traore D. S.
|
Real-Time Electromagnetic
Radiation Sensor [#1019]
We are
presenting the preliminary result of the CLuS’N
spacecraft optical system accessible at https://eee.orbitzone.space. Your
dashboard is equipped with a Real-time Electromagnetic Radiation Sensor that
calculates and mirrors the percentage of photons as a function of time
relevant to the angle of view. You may position your camera to your telescope
eyepiece and plug in the camera to your computer USB port, or just connect
your telescope-cam for the use of Eee Vision to
study your favorite light source.
|
|
Times
|
Authors (*Presenter)
|
Abstract
Title and Summary
|
|
2:30
p.m.
|
Y. Collado-Vega *
|
Moon-to-Mars Space Weather
Analysis Office [Invited]
As NASA plans for human
missions beyond Low-Earth Orbit (LEO), the need for improvements in space
weather environment modeling capabilities, communication of radiation risks,
and real-time space weather analysis support is essential for mission
success. These future missions will be flying in deep space and no longer
have the Earth's protective magnetic field shielding them from radiation in
space. The Space Radiation Analysis Group (SRAG) at Johnson Space Center and
the Community Coordinated Modeling Center (CCMC) at Goddard Space Flight
Center have worked on the Integrated Solar Energetic Particle (ISEP) Warning
System project which is a collaboration that expands SRAG's current space
weather monitoring capabilities beyond LEO. Last year, NASA established an
interface of communications with SRAG to improve science and prediction capabilities
both for lunar and Mars missions in support of crewed missions beyond LEO.
The Moon to Mars (M2M) Space Weather Analysis Office located at Goddard Space
Flight Center will provide SRAG with additional expert-based analysis of the
space radiation environment in support of human exploration activities. The
M2M Office will analyze state-of the-art space weather model output tailored
to SRAG’s needs as part of the ISEP project and the collaboration with CCMC.
The M2M Office will also support NASA robotic missions with space weather
assessments and anomaly analysis. The goal between CCMC and M2M is to create
an effective NASA in-house R2O2R pipeline for space radiation environment
predictive capabilities in support of human missions beyond LEO. One key
element of the partnership is the transition of ISEP models/software from
CCMC to M2M. We will present the M2M Office's goals, infrastructure, and
activities to support SRAG and NASA missions in collaboration with CCMC.
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2:45 p.m.
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Bale S. D. * Bonnell J. W. Burns J. Goetz K. Halekas J. S. Malaspina D. M. Page B. Pulupa M. Poppe A. R. MacDowall R. J. Maksimovic M. Zaslavsky A.
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The Lunar
Surface Electromagnetics Experiment (LuSEE) [#1030]
We will describe the Lunar Surface
Electromagnetics Experiment (LuSEE), which is
selected under the LSITP program to be manifested as a payload on a lunar
polar lander.
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2:55
p.m.
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Golub L. *
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Improving Space Weather
Forecasting with EUV Observations [#1031]
Accurate
predictions of harmful space weather effects are mandatory for the protection
of astronauts at the Moon. Observation of the corona at EUV wavelengths
offers the possibility of improving our forecasts of geo- and seleno-effective events.
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3:05 p.m.
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Wilson J. K. * Spence H. E. Schwadron N. A. Case A. W. Looper M. D. Jordan A. P. de Wet W. Kasper J.
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CRaTER’s SEP Index
Detects Small Solar Particle Events and Maps Lunar Radiation [#1033]
Search for solar trend / Finds lunar
radiation / Serendipity!
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3:15
p.m.
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Hegedus A. M. * Kasper J. C. Burns J. O. SunRISE Science Team
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Combining SunRISE
and Lunar Surface Interferometer Observations of Solar Radio Bursts [#1029]
The
Earth’s ionosphere limits radio measurements on its surface, blocking out any
radiation below 10 MHz. Valuable insight into many
astrophysical processes could be gained by having a radio interferometer in
space to image the low frequency window, which has never been achieved. One
application for such a system is observing type II bursts that track solar
energetic particle acceleration occurring at Coronal Mass Ejection
(CME)-driven shocks. A related application is localizing type III bursts
during storms to determine the level of magnetic connectivity of the source
region on the solar surface. These are the primary science targets for SunRISE, a 6 CubeSat interferometer to circle the Earth
in a GEO graveyard orbit. SunRISE is a NASA Heliophysics Mission of Opportunity that just passed its
Integrated Design Review, and plans to launch for a
12-month mission in mid-2024. In this work, we present the added benefit of
combining SunRISE observations with 2 or more
antenna on the lunar surface. The data added from lunar observations would
help us reconstruct the sky brightness patterns of larger radio bursts,
leading to a better understanding of the phenomena.
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3:25 p.m.
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BREAK
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Times
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Authors (*Presenter)
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Abstract
Title and Summary
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3:45
p.m.
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Paterson W. R. * Gershman D. J. Kanekal S. G. Livi R. L. Moldwin M. B. Randol B. Samara M. Zesta E. Christe S. D. Schiff C.
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Heliophysics from
Lunar Orbit with HERMES on Gateway [#1026]
The Heliophysics Environmental and Radiation Measurement
Experiment Suite (HERMES) is an external scientific space-weather payload set
to launch with the initial Gateway modules as early as November 2024. Arrival
in lunar orbit and the beginning of the science mission occurs about one year
after launch. HERMES was selected by NASA’s Science Mission Directorate
(SMD), and accommodation on Gateway’s Habitation and Logistics Outpost (HALO)
is provided by the Human Exploration and Operations Mission Directorate
(HEOMD). From its polar lunar orbit, HERMES will acquire data to address
multiple Heliophysics science objectives during
monthly traversals of the solar wind and the magnetotail. The measurements
can additionally support studies of the lunar exosphere and surface, and the
full data set will be available to all researchers through a public data
center. In this presentation, we discuss the mission objectives,
accommodation on Gateway, anticipated data products, and international
participation for this significant collaboration between SMD and HEOMD.
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4:00 p.m.
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Runov A. * Liu J. Khurana K. Balikhin M. Angelopoulos V. THEMIS/ARTEMIS Team
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Towards
Multi-Point Investigations of the Near-Moon Electromagnetic and
Plasma Environment [#1005]
For further exploration of the Moon with
potentially habitable orbital and surface stations, it is critically
important to characterize the near-Moon plasma environment, including
energetic particle fluxes, and understand physical processes of particle
acceleration at magnetic structures in the solar wind and in the magnetotail.
The two THEMIS-ARTEMIS probes have provided measurements of magnetic and
electric fields, ion and electron fluxes for almost
an entire Solar Cycle 24. The probes are in stable equatorial, 26-hr period
orbits, of ∼100km ×
19,000km altitude. Along with the HERMES instrument suite ARTEMIS will enable
three-point measurements to study plasma characteristics, particle energy
spectra in the solar wind, and in the magnetotail in a wide energy range from
10 eV to 10 MeV and their associations with magnetic field structures, such
as current sheets, flux ropes, fast flow fronts. Future magnetic field and
particle fluxes measurements from the Moon surface, coordinated ARTEMIS and
HERMES observations will greatly advance our knowledge on the near-Moon
electromagnetic and plasma environment.
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4:10
p.m.
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Williams M. N. Moshovelis L. D. * Iles G. N.
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Simulations of Radiation
Shielding Materials on the Lunar Gateway [#1002]
Future
crewed missions beyond Earth’s magnetosphere will involve significant
radiation exposure in an environment unlike anywhere else on Earth. Through
the Artemis 3 mission, the Lunar Orbital Gateway will be the newest
spacecraft to orbit the moon and provide vital support for a sustainable and
long-term return to the lunar surface. This research explores shielding
options to reduce radiation dose on a spacecraft for the safe success of
future lunar missions. Monte-Carlo simulations have been conducted using the
particle transport software, GEANT4. A life-size model of the Lunar Orbital
Gateway was constructed in SolidWorks. Radiation modeled by a solar particle
event was simulated onto the spacecraft to analyse
the effectiveness of shielding materials. It can be determined that the
materials — lunar regolith, polyethylene, and water all reduce the radiation
dose that astronauts would be exposed to in lunar orbit. For a prosperous and
safe future related to space exploration, shielding blocks should be a vital
component in the structure of any spacecraft to reduce the risk of exposure
from ionised particles.
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4:20 p.m.
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Mann I. R. * Fedosejevs R. Ozeke L. G. Tiedje H. Ball K. Yu B. Rowlands N. Zheng D. Caldwell D. Barona D. Yau A. W. Miles D. M.
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The Canadian SWeeping Energetic Particle Telescope (SWEPT): Steerable Energy and Pitch Angle Resolved
Energetic Particle Measurements in the Lunar Environment [#1023]
The Canadian SWeeping
Energetic Particle Telescope (SWEPT) targets an assessment of the pitch angle
dependence of particular space radiation, and will
address and characterize the energy and directional dependence of this space
radiation in the lunar environment. The project focuses on an assessment of
the fundamental plasma processes which accelerate the particles to create
this severe radiation hazard for astronauts in deep space,
and assess radiation risk mitigation. By using an innovative sweeping
look direction to determine the angular and energy dependence of the
radiation at the Moon, the SWEPT can assess the temporally evolving solar
energetic particle (SEP) radiation in the heliosphere, emitted in solar eruptions and accelerated at interplanetary shocks, as
well as address the impacts of primary and secondary radiation hazards on the
Lunar Gateway and on the lunar surface. The SWEPT will also contribute to the
development of effective deep space radiation mitigation strategies, such as
those based on the early arrival of solar energetic electrons in advance of
SEP protons for humans on the lunar surface or in the lunar vicinity. It will
also contribute to the assessment of space radiation-regolith interactions on
the lunar surface.
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4:30
p.m.
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Green J. C. Turner D. L. Likar J. J. * Parker L. Pitchford D. Keys C. C.
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Towards the Prediction of
Space Weather for Lunar Missions [#1020]
Sustained
operations and/or habitation on the lunar surface, in lunar orbit, or
cis-lunar space will require advances in space weather nowcasting and forecasting
as well as effective and actionable means of user interface. Recently, the
project “Understanding, Specification, and Prediction of Lunar Space Weather”
commenced in support of a NASA Heliophysics
Environmental and Radiation Measurement Experiment Suite Interdisciplinary
Science Teams study. The motivating research questions include: 1. What are the particle populations that
present a hazard to lunar operations? 2. How do those populations vary with
time, location, and different driving conditions? 3. How does the environment
translate into impacts? 4. How can we characterize and predict the
environment and impacts and best convey hazards to users? Here, we plan to
introduce the challenges, methods, and solutions under development as part of
this project, focusing first on efforts currently underway (e.g., prior to
Gateway/HERMES launch). We will describe all relevant particle populations,
their variation along the lunar orbit, and translations of such populations
and their intensities to expected impacts (hazards).
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4:40 p.m.
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Closing Remarks
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5:00
p.m.
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Adjourn
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