Anatomy of a Mission New Horizons From Idea To Launch Pad - Glen H. Fountain Johns Hopkins University Applied Physics Laboratory - Interstellar Probe
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Anatomy of a Mission
New Horizons
From Idea
To Launch Pad
Glen H. Fountain
Johns Hopkins University
Applied Physics Laboratory
After Voyager at Neptune – What’s Next?
AGU – Baltimore
1989
Anatomy of a Mission 27 September 2021 2
After Voyager at Neptune – What’s Next?
Pluto Workshop,
AGU – Baltimore
Lowell Observatory
1989
1993
Anatomy of a Mission 27 September 2021 3
An Abbreviated Pluto Mission Chronology
• 1989 – 1990: Farquhar et al. Pluto 350 Mission Study
• 1991 – 1992: Pluto 350 v. Mariner Mark II Trade Study
• 1993 – 1995: Pluto Fast Flyby (PFF) Study
• 1996 – 1997: Pluto Express (PE) Study
• 1998 – 2000: Pluto-Kuiper Express (PKE) Study
• Sept. 2000: PKE Cancelled. “Pluto is Over. Done. Dead.”
• Dec. 2000: NASA responds to Community pressure, Requests Competed Proposals
• None of these efforts ever
emerged from study phase.
• None resulted in any flight
hardware build.
Anatomy of a Mission 27 September 2021 4
It Sometimes Takes More Than A Successful Proposal Anatomy of a Mission 27 September 2021 5
It Sometimes Takes More Than A Successful Proposal Anatomy of a Mission 27 September 2021 6
Who Made It Happen?
• Several thousand individuals from
over 50 organizations made New
Horizons Possible
Anatomy of a Mission 27 September 2021 7
Anatomy of a Mission 27 September 2021 8
Larson, Wiley J., and James Richard Wertz. Space
mission analysis and design. No. DOE/NE/32145-T1.
Torrance, CA (United States); Microcosm, Inc., 1992.
4th Annual Interstellar Probe Exploration Workshop 30 September 2021 9
Anatomy of a Mission 27 September 2021 10
What Does a PI (Principal Investigator) Do? Ralph L. McNutt, Jr. Pragmatic Interstellar Probe Mission Study Principal Investigator
Role of Principal Investigator
§ Definition for NASA Missions
§ The PI is the sole Point of Contact (POC) for a grant or contact issued by NASA
§ Grant – Competitive award typically for one to five years for ~$100,000 up to ~$!,000,000
§ “Best effort basis” with no required “deliverables”, i.e., anything from paper reports to prototype
hardware
§ Contract – Usually, bot not always, competitive award for a “few” up to ~10 years with renewal options
§ Required deliverable items – hardware, software, and specified reports and reporting forms
§ The PI is “in charge”
§ Per the accepted proposal and issued contract, the PI is enabled to carry out the work proposed for the
contract value and in a time period as negotiated under the terms of the contract
§ The PI is responsible for performance – ESPECIALLY when there are problems in
executing the contact
§ This can include up to the termination of the project with no further funding, no additional time, and no (real)
appeal
4th Interstellar Probe Exploration Workshop - Student Program 27 September 2021 12Why Would Anyone Want to Be PI?
§ RHIP – “Rank Hath Its Privileges”
§ The PI has the opportunity to move science forward
§ The PI has the opportunity to learn really new things – new to everyone in the world
§ The PI stands to be recognized for these accomplishments
§ RHIR – “Rank Hath Its Responsibilities”
§ The PI has an implicit responsibility to contribute significantly to – if not lead – the advancement of
science and knowledge
§ The PI is an empowered agent of change using means put at her/his disposal by the government
§ The PI will be recognized for failures, and so has an implicit responsibility not to fail in the undertaking at
hand
§ Do you want to lead, or do you want to follow?
§ For better or worse, PIs help make the future … for everyone
4th Interstellar Probe Exploration Workshop - Student Program 27 September 2021 13Anatomy of a Mission 27 September 2021 14
Interstellar Probe (Quick) Overview Ralph L. McNutt, Jr. Pragmatic Interstellar Probe Mission Study Principal Investigator
A “Pragmatic” Interstellar Probe: Study
Status
§ The Johns Hopkins University Applied Physics
Laboratory was tasked by the NASA Heliophysics
Division to study the mission
§ Phase 1: 13 June 2018 – 12 June 2019
§ Phase 2 “Next Phase Concept Development”: 25
July 2019 – 30 April 2022
§ On schedule for Mission Concept Report to be
delivered early December 2021 for input to next
Solar and Space Physics Decadal Survey
4th Interstellar Probe Exploration Workshop - Student Program 27 September 2021 16Interstellar Probe Science Goal and Opportunities
Through Our Habitable Astrosphere and In To The Unknown
Primary Goal Astrophysics Opportunity
Our Habitable Astrosphere and The Sol Formation of Early Galaxies and Stars
Unexplored Interstellar Medium G2V Main Sequence Extragalactic Background Light
Star System
Planetary Science Opportunity
Status: Evolution of Planetary Systems
Astrosphere
Habitable KBOs Dwarf Planets Dust Disk
27 September 2021 4th Interstellar Probe Exploration Workshop - Student Program 17Purpose of the Study
§ Determine the accessible region of the box below given the Technology Horizon:
Could be ready to launch by 2030
§ “Estimate” the corresponding inclusivity of the identified “Compelling Science”
Power
D ow n g e v i ty
l i nk Lon
4th Interstellar Probe Exploration Workshop - Student Program 27 September 2021 18One (of many possible) scenarios KSC Launch Complex 39 Pad B: 28 August 2036… 4th Interstellar Probe Exploration Workshop - Student Program 27 September 2021
Anatomy of a Mission 27 September 2021 20
Interstellar Probe Explaining the MCR Jim Kinnison Interstellar Probe Concept Study System Engineer jim.kinnison@jhuapl.edu
What is an MCR?
(Engineering Perspective)
• Scientists have defined a great set of goals and objectives. Now how do we implement that?
- Science traceability matrix should ultimately lead to a set of mission requirements.
- The engineering team defines how we meet those through a set of trade studies.
- For Interstellar Probe, this is a point design demonstrating that such a mission can be done.
• Parts of a Mission Concept
- Where are we going?
- How are we going to get there?
- What will we do there?
- What is the flight system?
- How do we operate it to get the data?
• Ultimate goal is to convince the reader that the mission is well-understood, can be performed
with reasonable risk, and fits within the schedule and budget available.
4th Interstellar Probe Workshop 27 September 2021 22Where are we going?
How do we get there?
9.9 m
331 m3
4th Interstellar Probe Workshop 27 September 2021 23What will we do there?
Event Time Period Mission Time
Launch and Checkout 2 months 2 Months
Cruise to Jupiter 7 months 9 Months
JGA –5 weeks to +3 weeks 0.92 year
Wire Antenna 1 month 1 year
Deployment
Inner Heliosphere 11.86 years 12.86 years
Heliosheath 4.12 years 16.98 years
Interstellar Phase 33.02 years 50 years
Extended Mission 92.51 142.5 years
(1000 AU)
4th Interstellar Probe Workshop 27 September 2021 24What does the flight system look like? 4th Interstellar Probe Workshop 27 September 2021 25
How do we get the data? 4th Interstellar Probe Workshop 27 September 2021 26
Anatomy of a Mission 27 September 2021 27
Baseline Goal: Understand Our Habitable Astrosphere and its Home in the Galaxy
Science Specific
Measurement Objectives Measurements Mission Requiremets
Objectives Questions
Global Structure; Force In-situ spectra, composition, flows, densities, MAG, PLS, PUI, EPS, CRS, Spinning; ENA imaging from ~250 AU
Balance temps and fields across HS and into LISM, ENA, PWS, LYA
flows; Remote wave, Ly-a and ENA imaging.
Physical
Ribbon/Belt ENA imaging; In-situ within ribbon. ENA, PLS, PUI, EPS, MAG Spinning; through ribbon to ~300 AU
Processes and
ACRs, shocks, Fields, e/ion composition plasma to ACRs MAG, PLS, PUI, EPS, CRS, Spinning; through HP ~130 AU; spend
Global
reconnection, TS, HP across TS, HS; Fields, waves, particle spectra, PWS sufficient time in HS
Manifestation composition for HP instabilities
Neutrals in the LOS velocity, temperature, density of H LYA, NMS Through HP ~130 AU
Heliosphere
Solar Wind Effects on the In-situ variations in HS; MAG, PLS, PUI, EPS, ENA Spinning; spend sufficient time in HS
Boundary ENA variations remotely
Dynamics and Shock Propagation and Fields, e/ion plasma to GCR anisotropies; fields MAG, PLS, PUI, EPS, CRS, Spinning; sufficient time beyond HP out to
Evolution Turbulence turbulent spectra Earth to LISM PWS ~400 AU
GCR GCR e/ion composition, fields out to LISM MAG, CRS Spinning; sufficient time beyond HP out to
Modulation/Shielding ~400 AU
Nature of Bow In-situ fields, plasma MAG, PLS Spinning; ≤300 AU
Shock/Wave
Properties of the Hydrogen Wall LOS H; In-situ H and composition LYA, NMS ≥300 AU
Unexplored Neutrals/Dust Filtration In-situ elemental and isotopic out to LISM PLS, PUI, PWS, NMS, IDA ~400 AU
VLISM LISM gas and plasma Density, temp., composition, ionization MAG, PLS, PWS, NMS Spinning; ~400 AU
LISM Inhomogeneities Variability of properties on 100’s AU PLS, PWS, NMS, IDA Spinning; ~400 AU
Origin of GCRs Elemental/isotopic abundances, spectra CRS Spinning; sufficient time beyond HP
MAG Magnetometer PUI Pick-Up Ions CRS Cosmic Ray System ENA Energetic Neutral Atoms NMS Neutral Mass Spectrometer
PLS Plasma System EPS Energetic Particle System PWS Plasma Wave System IDA Interstellar Dust Analyzer LYA Ly-Alpha Spectrograph
Alice Cocoros 28Example Model Payloads
Instrument Mission
Measurement Requirements Science Driver
(Heritage) Requirements
Baseline Magnetometer (MAG) 0.01 - 100 nT; 0.01 nT ≤ 60 s; LISM
87.4 kg (MMS/DFG) (10-8 nT2/Hz turb.) (100 Hz)
Two FG, 10m boom
(turbulence)
86.7 W
Plasma Waves (PWS) ~1 Hz – 5 MHz; ∆f/f ≤ 4% ≤ 60 s 4x50 m wire; LISM ne, Te (QTN),
Charged Particles (Van Allen/EFW) ≤ 0.7 µV/m @ 3 kHz (≤ 4 s at TS) spin plane turbulence
Fields and Waves Plasma Subsystem (PLS) < 3 eV/e to 20 keV/e Flows, ne, Te, ni, Ti
(PSP/SWEAP/SPAN-A)
~4π; ≤ 60 s Spinning
ENA Imaging e, H+, He+, He++, C+, N-O+ Force balance
0.5-78 keV/e
Dust Pick-up Ions (PUI) iFOV ≥ Interstellar, inner PUI
H, 2H, 3He, 4He, 6Li, 12C, 14N, 16O, 20Ne, Spinning
(Ulysses/SWICS) 22 90°x15° Force balance
Neutrals Ne, Mg, Si, Ar, Fe, charge states
Ly-alpha Energetic Particles (EPS) 20 keV – 20 MeV S/W, HS and ACRs
~4π; ≤ 60 s Spinning
(PSP/EPI-Lo) H, 3He, 4He, C, O, Ne, Mg, Si, Ar, Fe Force balance
H to Sn;10 MeV/nuc - 1 GeV/nuc;
Cosmic Rays (CRS) 3 directions; ACRs, GCRs
m/∆m ≥ 10 Spinning
14% (PSP/EPI-Hi, new development) hours LiBeB cosmic story
electrons; 1-10 MeV
30% Interstellar Dust Analyzer (IDA) 10-19 to 10-14 g, 1-500 amu; Ram direction ISDs, galactic heavy ion
(IMAP/IDEX, new development)
iFOV ≥ 90˚
m/Δm ≥ 200 Co-boresighted NMS composition
11%
Neutral Mass Spectrometer (NMS) H, 3He, 4He, 14N, 16O, 20Ne, 22Ne, 36Ar, iFOV ≥ 10˚; Ram direction
(LunaResurs/NGMS, JUICE/NMS) 38 LISM composition
Ar, m/Δm ≥ 100 weekly Co-boresighted IDA
12% ENA (ENA) Shape, force balance,
(IMAP/Ultra, new development)
~1-100 keV H iFOV: ≥ 170° Spinning, 2 heads
ribbon/belt
19%
14% Lyman-Alpha Spectrograph (LYA) ±100 km/s doppler range, iFOV: ≤ 5˚;
Spinning LISM and heliosheath H
(MAVEN/IUVS, new development)Baseline Spacecraft Accommodation
Alice Cocoros 30Potential Planetary and Astrophysics Objectives on Interstellar Probe
Augmented Option: Goals 2 and 3 Only
Science Measurement Mission
Goal Questions Measurement Objectives
Objectives s Requirements
State and evolution of dwarf planets, KBOs Landforms, composition, thermal;
VIR, IRM, MAG,
2. Origin and Evolution of Planetary
Magnetic field strength and direction; 3-axis, ≤104 km flyby
NMS
atmospheres and rings
Collisional, orbital, geological history Rotation and phase curves of distant bodies
Planets, dwarf VIR, IRM 3-axis, 106 km
Atmospheres, rings, nightside temperatures
planets and KBOs Compositional state of Kuiper Belt PUI distribution and composition PUI, MAG, IDA,
≤100 AU
Dust composition and distribution NMS, VIR, IRM
Systems
Interstellar Space Weathering Panchromatic distant observations VIR, EPS, CRS 3-axis, 106 km
Solar System as Exoplanetary Analogues Planetary rotation and phase curves VIR 3-axis, look back @10’s AU
Dust disk total mass In-situ/Visible-FIR observations of dust IDA, NMS, IRM
≤0.1 RPM, ≤100 AU
(PWS)
Circum-solar Dust Interplanetary dust grain production In-situ dust mass distribution IDA, IDC, NMS ≤100 AU
Cloud Solar nebula chemical processing In-situ dust composition; spectral features IDA, NMS, IRM ≤0.1 RPM, ≤100 AU
Large-scale processes due to solid bodies In-situ/remote correlation with bodies; IR dust
IDA, NMS, IRM ≤0.1 RPM, ≤250 AU
and solar activity; comparables to exodisks extinction during CME passages; In-toto IR
Nearby and Properties of distant ISM dust NIR diffuse and FIR galactic emissions IRM ≤0.1 RPM, >150 AU
and Stellar
3. Galactic
Distant ISM
Evolution
Properties of VLISM dust In-situ ISD IDA, NMS ≤0.1 RPM, ≥120 AU
Nucleosynthesis and star formation Diffuse spectrum in optical/NIR/FIR IRM ≤0.1 RPM, ≥10 AU
EBL
Emissivity budget of galaxy formation Decompose NIR/FIR spectra IRM ≤0.1 RPM, ≥10 AU
Nucleosynthesis Evidence for recent nucleosynthesis Isotopic gas and dust ratios in the VLISM NMS, IDA, PLS Spinning, ≤400 AU
MAG Magnetometer PUI Pick-Up Ions CRS Cosmic Ray System IDA Interstellar Dust Analyzer VIR Visible/Near-IR v6.0
PLS Plasma System EPS Energetic Particle System PWS Plasma Wave System NMS Neutral Mass Spectrometer IRM IR Mapper
Alice Cocoros 31Example Model Payloads
Augmentation
89.1 kg
90.2 W
Charged Particles
Fields and Waves
ENA Imaging
Dust
Neutrals
Flyby Imaging
IRM
6%
12%
30%
Instrument Mission
Measurement Requirements Science Driver
11%(Heritage) Requirements
Flyby
Visible-Near-IR (VIR) 0.4-4 µm; ≥ 5 ch. ≤0.975 µm; iFOV: 5-20 µrad 3-axis
features/composition,
(New Horizons/Ralph) >240 ch. >0.975 µm FOV: 2.3°- 5.7° Co-boresighted IRM
distant KBOs, astro
11%
Visible-IR Mapper (IRM) 17% 0.5-15 µm NIR: 0.075 mrad/1˚ 3-axis; perp. to spin Dust Disk, surface
(New Horizons/LEISA, CIBER-2, in development) 30-100 µm FIR: 3 mrad/0.2˚ Co-boresighted VIR comp., ISM dust, CBL
13%
Alice Cocoros 32Anatomy of a Mission 27 September 2021 33
Interstellar Probe Study Next Steps and Future Planning Elena Provornikova Heliophysics Science Lead
Preparing for the upcoming Heliophysics Decadal Survey
§ >30 White Papers in preparation
https://docs.google.com/spreadsheets/d/1FJfWSsPgS41Ktqu1_X2UyAITiNnRpZ88P_RvhccvhI/edit#gid=0
§ Zoom discussion on Outer Heliosphere and Interstellar Medium Science and White papers.
Join in!
https://docs.google.com/forms/d/e/1FAIpQLSe4kWI5NQOvc1D3t90BTtwK_dM_lFNvDhqdzjqJmRojYXczvg/viewform
§ Oct 6th ”Heliospheric Tail” Erik Powell and Merav Opher
§ Oct 20th “The Interaction of Interstellar Dust with Our Heliosphere” Jamey Szalay
§ Nov 3rd “Supernova Explosion near the heliosphere” Brian Fields and Jesse Miller
§ Nov 17th “Solar wind turbulence from 1 to 45 AU” Charles Smith
§ Dec 1st “Theoretical analysis of the interstellar dust distribution in the heliosphere and heliospheric interface”
Egor Godenko
§ Publications in peer-reviewed journals
§ Interstellar Probe Book
26 September 2021 35AGU Fall Meeting
13-17 December 2021 New Orleans, LA and Online Everywhere
session SH018 - Interstellar Probe: a mission through
the heliosphere edge into the local interstellar space
Invited Talks
§ Alice Cocoros, JHU APL “Goldilocks and the Many
Science Instruments: Optimizing Example Payloads to
Maximize Science on an Interstellar Probe”
§ Pawel Swaczyna, Princeton “Interstellar Neutral Atom
Observations from 1 au to the Very Local Interstellar
Medium”
26 September 2021 36Anatomy of a Mission 27 September 2021 37
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