ELECTRODYNAMIC TETHER MICROSATS AT THE GIANT PLANETS
|
|
- Coleen Underwood
- 5 years ago
- Views:
Transcription
1 ELECTRODYNAMIC TETHER MICROSATS AT THE GIANT PLANETS Summary Report for ARIADNA Study No. 05 / 3203 September Universidad Politécnica de Madrid Juan R. Sanmartín Mario Charro European Space Agency / ESTEC Cristina Bramanti Claudio Bombardelli Collaborators: E. Lorenzini / University of Padua; H. Garrett / JPL -NASA Space Issue Addressed A full study of the complex Jovian system, particularly moons Europa and Io and Jupiter itself, is a central goal in space science. Future ESA and NASA Jovian missions face basic issues concerning power and propulsion needs, trip times, and harsh radiation environment. The present Study has addressed those issues; its approach involves an electrodynamic (ED) tether accounting for some fraction of full spacecraft (SC) mass to tap Jupiter s rotational energy for power and propulsion, during both capture by Jupiter and a tour following capture. The otherwise successful Galileo mission was limited in the above respects. The high wet-mass fraction characteristic of chemical propulsion reduced orbit manoeuvring after capture, and kept scientific payload to a few per cent in mass; jointly with launcher limitations, it led to a protracted, indirect trip to Jupiter requiring gravity-assist manoeuvres (GAs). The power source used, Radioisotope Thermal Generators (RTGs), is characterised by a very low specific power and is based on Pu 238, a material difficult to manufacture and extremely expensive, with Russia being presently the only manufacturer at industrial scale. Moreover, just a few RTG units are left from previous NASA missions. ESA faces export restrictions on US RTG technology, and an ecological worry about Earth flybys, in addition to the limitations that NASA itself faces at present. A variety of approaches to a challenging Jovian mission have rapidly followed each other. NASA s Europa Orbiter mission, cancelled in Phase B, would keep RTG s and rockets, skipping GAs however during a cruise on direct trajectory to Jupiter, while using GAs, on the contrary, for moon manoeuvres. The Jovian Icy Moons Orbiter (or Prometheus 1), now deferred indefinitely, would have used a nuclear reactor system for both power and powering high specific-impulse electrical thrusters (NEP). The JUNO
2 polar orbiter mission will revert to chemical propulsion and indirect-trajectory/gas, but will replace RTGs with low-intensity/low-temperature (LILT) cell-arrays for solar power. Jet Propulsion Laboratory studies for NASA (Europa Geophysical Explorer, Europa Explorer Concept), and planning within NASA s OPAG (Outer Planets Assessment Group), would keep RTG s and rockets but would use GAs for both indirect trip and moon tour leading to capture into low orbit around Europa, with emphasis on facing radiation damage; advances in electronics hardening might allow 3 months in orbit at Europa with over 3 Mrad(Si) radiation dose. An Io-Community Panel proposed a Jovicentric Orbiter for multiple flybys of the same Io hemisphere. ESA s Jovian Minisat Explorer would use GAs for indirect trajectory and post-capture manoeuvring, chemical propulsion (with Solar Electric Propulsion backup), and solar arrays for power, with solar concentrators and GaAs-LILT cells; should its solar power program fail, ESA would revert to RTGs. After capture by Jupiter the JME would split into a Jovian Europan Orbiter and a Jovian Relay Satellite, due to acquire a low circular orbit around Europa and a Jovian elliptical orbit at 3:1 resonance with Europa, respectively, through extended moon GAs. JRS would both do science and relay JEO data to Earth. JEO hardware would tolerate 1 Mrad(Si) dose with 10 mm aluminium shielding; ESA is developing a Highly Integrated Payload Suites program to reduce payload mass and volume (and thus shielding mass too). A 2005 Space Physics of Life proposal to NASA, the Ganymede Exploration Orbiter, also involved two spacecraft. 2.- Tethered-SC Mission Concept An ED-tether in prograde orbit can provide power and drag/thrust. A satellite corotates with its planet at the stationary circular orbit with the radius a s ( / 2 ) 1/3 R ( / 2 ) 1/ 3,,, R, and being planet spin rate, gravitational-constant, radius, and mean density; if corotating atmosphere was present beyond a s, satellites at a > a s would be pushed by faster-moving air to higher, though slower, orbits. This is a kinetic mechanism driving the planet/satellite system to thermodynamic equilibrium: for a small satellite, mechanical energy versus radius a presents a maximum, which is always unstable, and lies at the stationary orbit for the comparatively light artificial satellites. Any mechanism for dissipation (tidal forces in case of natural moons) drives the satellite away from a(max) on either side of it. An ED-tether provides a similar mechanism in planets having magnetic field ( B ) and corotating ionosphere/magnetosphere. In the highly conductive ambient plasma around, there is a motional electric field in the tether frame, Em ( v v ) B, which drives pl a current I inside the tether ( v, v pl are tether and plasma velocities). Electrical power is always generated at the tether circuit ( I E L > 0, L tether length); that power is the m net loss-rate in mechanical energy, which involves the Lorentz force and the velocity difference v v. The Lorentz force will be thrust if v is opposite v v pl, a pl condition applying for prograde orbits with radius a > a s ; the Lorentz force will be drag for radius a < a s. The force would always be drag for retrogade orbits.
3 ED-tether operation requires effective contact, both anodic and cathodic, with the highly rarefied ambient plasma. Electron ejection at a hollow cathode is not an issue. As regards anodic contact, it was proposed in 1992 that, instead of using a big end collector, the tether be left bare of insulation, allowing it to collect electrons over the segment coming out positively polarized, as a giant cylindrical Langmuir probe in the orbital-motionlimited (OML) regime. Collection is efficient if the tether is thin. The collecting area of a thin bare tether is still large because the anodic segment is tens of kilometers long. A thin tape collects the same OML current as a round wire of equal cross-section perimeter and is much lighter; the tether is thus characterized by three quite disparate dimensions, tape length (L) >> tape width (w) >> tape thickness (h). The Jovian system is particularly appropriate for the use of ED-tethers in thrusting, as well as dragging, producing power either way. Operating conditions require plasma beyond the radius a s to i) be dense enough, and ii) corotate with the planet. Jupiter has both low density and high spin ; as a result the stationary orbit lies at 2.24 Jupiter radii (a s 2.24 R J ), which is one third the relative distance for Earth. Further, the surface magnetic field is ten times greater at Jupiter than at Earth; magnetic stresses are thus 10 2 times greater at Jupiter, and allow for corotating plasma beyond a s. A Jovian plasmasphere reaches to about 3.8 R J. In addition, moon Io is both at a 1:2 Laplace resonance with Europa, and ten times relatively closer to its planet than the Moon is to Earth (a Io 5.9 R J ). This leads to tidal deformations inside Io that produce extreme tectonics and volcanism. Neutral gas continuosly ejected by Io is ionized and accelerated by the fast-flowing Jovian magnetosphere, and made to corotate as a giant plasma torus denser than the plasmasphere and reaching near Europa, which orbits at a Eu 9.4 R J. This is a natural plasma source that can be advantageously used by the ED-tether. 3.- Tethered-SC capture operation and constraints The Jovian mission starts with the SC approaching Jupiter at the relative velocity v 5.6 km/s of a minimum-energy transfer, i.e. a Hohmann transfer when ignoring the 1.3 degrees inclination of Jupiter s orbit with respect to the ecliptic. The critical phase is SC capture; closed orbits could substantially evolve afterwards under repeated Lorentz force. The issue is whether a ED tape-tether can capture a SC, with full mass M SC a few times the tether mass m t, into an equatorial, highly elliptical, low perijove orbit at Jupiter. Design parameters, tape length L and thickness h, and perijove radius r p, face opposite criteria. A high mass-ratio M SC / m t requires a low perijove and (in the weak ohmic-effects limit best representing conditions at the Jovian mission) a high L 3/2 /h ratio (i.e. a relatively long and thin tether). Low gravity gradients and high lateral Lorentz forces at Jupiter make a tether spin t necessary (hollow cathodes at both tether ends take turns in becoming cathodic as the tether rotates). Tether tensile stress scales as t t 2 L 2 ( t tether density) while tether bowing from the Lorentz force scales as L 1/2 / h t t 2, or L 5/2 /h for a given upper bound on stress.
4 Also, tether temperature is in thermal equilibrium both local and quasisteady, heating and radiated power keeping nearly equal at each point as the tether rotates. In the weak ohmic effects limit, heating arises from the impact of collected electrons, and maximum temperatures occur at tether ends, even though they only receive heating when acting anodically, i.e. half the time. Maximum tether temperature scales as L 3/8 / t 1/4, with t being the tether surface emissivity. Beyond limiting tether length, an acceptable temperature around the perijove during capture will require coating the tape to reach values t 0.8. In addition, boh tether temperature and bowing are greater the closer to Jupiter is the perijove. A preliminary design that sets a mass ratio M SC / m t 3 and the perijove at 1.5 R J, and uses a coated aluminium tape that is 80 km long and 0.05 mm thick, with thermal emissivity t 0.8 and a 20 minutes spin, satisfies all constraints, though it barely captures the SC. Capture may be eased by decreasing the excess hyperbolic velocity v below the Hohmann transfer value, and reducing both the tether material density t and its thickness h: with ohmic effects weak, the tape cross section need not be all conductive; it could be partly made of aluminium and partly of fiber, e.g. Kevlar, to both reduce density and increase tensile strength (and prevent tape tearing). No characteristic dimensionless number involves the tape width w, which may easily range from 1.5 cm to 15 cm. The upper end arises from OML-regime validity considerations, with the thermal electron gyroradius reaching a minimum value during capture about 7.5 cm. Below w = 1 cm, there might be an issue of survivality to micrometeoroid cuts. For a 3 cm wide tape, m t and M SC would be 324 kg and 972 kg respectively; the spacecraft mass will just scale up with w, from 500 kg to 5000 kg for the width range above. If ignoring thermal and bowing considerations, tether current at capture could be increased by decreasing r p and h/l 3/2 but would be ultimately limited by ohmic effects to a (short-circuit) value independent of ambient plasma density. Ambient conditions could then only affect the capture mass ratio through the planetary magnetic field B. In the capture region, B (for both Jupiter and Saturn) is dominantly produced by currents inside the planet, a magnetic-dipole field approximation being valid for estimates. It was found that, in the case of Saturn, where B is 20 times smaller than at Jupiter, a ratio M SC /m t below unity appears required for tether capture, which would make it impossible. 4.- Tether-operated Jovian missions Following capture, repeated application of Lorentz drag at perijove passes can efficiently lower the orbit apojove. This can give lead to three different mission profiles: Mission 1. Frequent Galilean Moons Flybys A tethered SC could rapidly and frequently visit Galilean moons. Elliptical orbits with (capture) perijove at about r p = 1.5 R J and apojoves down at the Io, Europa and Ganymede orbits, are in resonances 1:2, 4:9, and 2:5 with the respective moons. For
5 the design tape, about 25 slow flybys of Io could take place before the accumulated radiation dose exceeds 3 Mrad(Si) with 10 mm Al shield thickness, for a total mission duration of over 5 months after capture. The respective number of flybys for Ganymede would be 12, with total duration of about 9 months. Mission 2. Low Circular Jovian Orbit A tethered SC could acquire a safe, low circular orbit around Jupiter (below the radiation belts) and manoeuvre to get an optimal altitude, with no major radiation effects, in less than 5 months after capture. An 80-km-long, 0.05-mm-thick tape, and several centimeters wide, could survive 1 year in the Jovian environment with probability very close to unity, allowing all three missions here. Mission 3. Low Circular Orbit at Io By thrusting at the apojove once down at the Io torus, in order to raise the perijove from the plasmasphere, a tethered SC could acquire a low circular orbit around moon Io in about 4 months, or 8 months after capture. This corresponds, however, to well over one hundred apojove passes, torus thrusting being weak; the accumulated radiation dose, about 7.5 Mrad(Si), poses a critical issue. Again, accumulated radiation dose for all three types of missions could be reduced by decreasing tape thickness and density. Also, thrusting at the torus to raise the perijove in Mission 3 is more efficient the higher the perijove; preliminary use of rocket thrust for limited perijove rise could skip tether thrusting at inefficient apojove passes. Once a full orbit is inside the torus, raising the apojove to moon Europa through a series of (torus) perijove passes would again face a radiation issue. A recent modification, GIRE, of the radiation model here used (Divine/Garrett, 1983), with data from the Galileo Energetic Particle Detector, has little effect on dose per orbit for orbits that reach very close to Jupiter. A second modification of the radiation model, arising from new fittings to synchrotron emission data, just affects the energetic-electron flux at the narrow (equatorial) radial range 2 R J R J. 5.- Main pending issues for further study Basic standing issues concern high radiation dose and model uncertainties in plasma density. Radiation damage could effectively block Mission 3, which will require advances in electronics hardening, and a design that allows greater shielding (use of ESA s Highly Integrated Payload Suites). As regards plasma modeling, the capture operation requires an accurate inner-plasmasphere description, whereas Mission 3 is strongly affected by uncertainties in torus radial and latitudinal profiles; beyond a factor of 2 error in published ion temperatures entering the Divine/Garrett torus model, late Galileo data suggests plasma density in the torus is higher by a factor of 2 than indicated by Voyager data, while there are reports of greater latitudinal extent in the torus ribbon region. Issues deserving further detailed study include:
6 - Sensitivity of performance to uncertainties and temporal variations in plasma density at the inner plasmasphere and in torus latitudinal extent. A mismatch between model and actual values would be particularly problematic for the critical capture phase in all three Missions. Possible temperature differences among species and possible temperature anisotropies keep a degree of uncertainty in torus thickness, affecting Mission 3; also, recent analyses from a Cassini flyby show long term variations in plasma conditions in the Io torus, from the Voyager 1, 2 era, but also monthly and even hourly variations. - A thorough determination of radiation dose per orbit and accumulated dose throughout Missions Assuming the SC in Io orbit, use of the Lorentz force to make that orbit stable against the pull of Jupiter. The radius of the sphere of influence of Io against its planet is only 7200 km, Io s radius itself being 1820 km. Galileo data showed that Io has a substantial ionosphere, with electron densities at hundreds of kilometers above Io's surface reaching values 10 5 cm -3, well above the ambient magnetospheric density; and with plasma that arises from Io, and goes into its torus, corotating with the Jupiter s magnetosphere at distances from Io's center as close as 7 times Io s radius, or about 13,000 km only. - Both lateral tether dynamics and the long-term effect of the Lorenz torque on tether spin. Deployment uses 2-phase, in-line / off-line rocket thrust that provides temporary spin with no mass penalty on capture and tour operations. Off-line rocket thrust would also provide the 20 minutes spin (opposite the Jupiter spin) that eases tether dynamics and keeps it taut. - Detailed power strategy in using electrical energy generated over high-current segments of orbits, and saved/stored in regenerative fuel cells / batteries, to cover overall power needs; in particular, the possibility of powering electric propulsion at the critical thrusting needs for Mission 3. - Radiation impedance for tether-circuit current closure in the Jovian plasma, throughout the missions above. - Detailed selection of tape materials, when considering tensile stress and possibly large thermal excursions. - Detailed analysis of survivality of tapes to hypervelocity micrometeoroid impacts in case of Mission 2, which could extend for several years. - Detailed design of a conductive-tape deployer. - Mission cruise analysis on the reduction of the excess hyperbolic velocity.
Electrodynamic Tether at Jupiter 1. Capture operation and constraints
Electrodynamic Tether at Jupiter 1. Capture operation and constraints Juan R. Sanmartin and M. Charro, Universidad Politecnica de Madrid E. Lorenzini, University of Padova, H. Garrett, Jet Propulsion Laboratory
More informationPropellantless deorbiting of space debris by bare electrodynamic tethers
Propellantless deorbiting of space debris by bare electrodynamic tethers Juan R. Sanmartín Universidad Politécnica de Madrid Presentation to the 51 th Session of the Scientific and Technical Subcommittee
More informationJOVIAN ORBIT CAPTURE AND ECCENTRICITY REDUCTION USING ELECTRODYNAMIC TETHER PROPULSION
AAS 14-216 JOVIAN ORBIT CAPTURE AND ECCENTRICITY REDUCTION USING ELECTRODYNAMIC TETHER PROPULSION Maximilian M. Schadegg, Ryan P. Russell and Gregory Lantoine INTRODUCTION The use of electrodynamic tethers
More informationOverview of the Jovian Exploration Technology Reference Studies
Overview of the Jovian Exploration Technology Reference Studies The Challenge of Jovian System Exploration Peter Falkner & Alessandro Atzei Solar System Exploration Studies Section ESA/ESTEC Peter.Falkner@esa.int,
More informationESA s Juice: Mission Summary and Fact Sheet
ESA s Juice: Mission Summary and Fact Sheet JUICE - JUpiter ICy moons Explorer - is the first large-class mission in ESA's Cosmic Vision 2015-2025 programme. Planned for launch in 2022 and arrival at Jupiter
More informationOutline. Characteristics of Jupiter. Exploration of Jupiter. Data and Images from JUNO spacecraft
Outline Characteristics of Jupiter Exploration of Jupiter Data and Images from JUNO spacecraft 2 Characteristics of Jupiter Orbit Size Around Sun Mass Scientific Notation: 7.7834082 10 8 km Astronomical
More informationJUpiter Icy Moons Explorer (JUICE) Status report for OPAG. N. Altobelli (on behalf of O. Witasse) JUICE artist impression (Credits ESA, AOES)
JUpiter Icy Moons Explorer (JUICE) Status report for OPAG N. Altobelli (on behalf of O. Witasse) JUICE artist impression (Credits ESA, AOES) Message on behalf of the JUICE Science Working Team Congratulations
More informationJuno. Fran Bagenal University of Colorado
Juno Fran Bagenal University of Colorado Cassini 2000 Cassini 2000 Jupiter s Pole When the Galileo Probe entered Jupiter clouds Expected ammonia + water clouds But found! very few clouds Probe entered
More informationThe Jovian Planets. Why do we expect planets like this in the outer reaches of the solar system?(lc)
The Jovian Planets Beyond Mars and the Asteroid belt are the Jovian or Gas Giant Planets that are totally different than the terrestrial planets: They are composed almost entirely of gas They do not have
More informationChapter 11 Jovian Planet Systems. Comparing the Jovian Planets. Jovian Planet Composition 4/10/16. Spacecraft Missions
Chapter 11 Jovian Planet Systems Jovian Planet Interiors and Atmospheres How are jovian planets alike? What are jovian planets like on the inside? What is the weather like on jovian planets? Do jovian
More informationJupiter. Jupiter is the third-brightest object in the night sky (after the Moon and Venus). Exploration by Spacecrafts
Jupiter Orbit, Rotation Physical Properties Atmosphere, surface Interior Magnetosphere Moons (Voyager 1) Jupiter is the third-brightest object in the night sky (after the Moon and Venus). Exploration by
More informationLast Class. Today s Class 11/28/2017
Today s Class: The Jovian Planets & Their Water Worlds 1. Exam #3 on Thursday, Nov. 30 th! a) Covers all the reading Nov. 2-28. b) Covers Homework #6 and #7. c) Review Space in the News articles/discussions.
More informationOrbital energy of natural satellites converted into permanent power for spacecraft
Orbital energy of natural satellites converted into permanent power for spacecraft J. Peláez January 14, 2008 1 Introduction Some of the most startling discoveries about our solar system have been made
More information12a. Jupiter. Jupiter Data (Table 12-1) Jupiter Data: Numbers
12a. Jupiter Jupiter & Saturn data Jupiter & Saturn seen from the Earth Jupiter & Saturn rotation & structure Jupiter & Saturn clouds Jupiter & Saturn atmospheric motions Jupiter & Saturn rocky cores Jupiter
More informationReduction of Trapped Energetic Particle Fluxes in Earth and Jupiter Radiation Belts
Reduction of Trapped Energetic Particle Fluxes in Earth and Jupiter Radiation Belts Robert Hoyt, Michelle Cash Tethers Unlimited, Inc. 11711 N. Creek Pkwy S., Suite D-113, Bothell, WA 98011 (425) 486-0100
More informationJUICE: A European Mission to Jupiter and its Icy Moons. Claire Vallat Prague, 15 th November 2018
JUICE: A European Mission to Jupiter and its Icy Moons Claire Vallat Prague, 15 th November 2018 Emergence of habitable worlds around the gas giants The Jupiter icy moons family portrait [Lammer et al,
More information11.2 A Wealth of Worlds: Satellites of Ice and Rock
11.2 A Wealth of Worlds: Satellites of Ice and Rock Our goals for learning: What kinds of moons orbit the jovian planets? Why are Jupiter's Galilean moons so geologically active? What is remarkable about
More informationJovian Radiation Environment Models at JPL
Copyright 2016 California Institute of Technology. Government sponsorship acknowledged. Jovian Radiation Environment Models at JPL By Insoo Jun and the JPL Natural Space Environments Group Jet Propulsion
More informationLast Class. Jupiter. Today s Class
Today s Class: Jupiter & Its Waterworld Moons 1. Reading for Next Class: Saturn and its moons Chapter 11 in Cosmic Perspective. 2. Homework #8 will be due next Wednesday, April 18. 3. Need 2 more volunteers
More informationPhys 214. Planets and Life
Phys 214. Planets and Life Dr. Cristina Buzea Department of Physics Room 259 E-mail: cristi@physics.queensu.ca (Please use PHYS214 in e-mail subject) Lecture 28. Search for life on jovian moons. March
More informationTechnology Reference Studies
In the proceedings of the 8th ESA Workshop on Advanced Space Technologies for Robotics and Automation 'ASTRA 2004' ESTEC, Noordwijk, The Netherlands, November 2-4, 2004 Technology Reference Studies P.
More informationLecture Outlines. Chapter 11. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 11 Astronomy Today 8th Edition Chaisson/McMillan Chapter 11 Jupiter Units of Chapter 11 11.1 Orbital and Physical Properties 11.2 Jupiter s Atmosphere Discovery 11.1 A Cometary
More informationPlanetary magnetospheres
Planetary magnetospheres Text-book chapter 19 Solar system planets Terrestrial planets: Mercury Venus Earth Mars Pluto is no more a planet! Interiors of terrestrial planets are different very different
More informationDesign of a Multi-Moon Orbiter
C C Dynamical A L T E C S H Design of a Multi-Moon Orbiter Shane D. Ross Control and Dynamical Systems and JPL, Caltech W.S. Koon, M.W. Lo, J.E. Marsden AAS/AIAA Space Flight Mechanics Meeting Ponce, Puerto
More informationAn introduction to the plasma state in nature and in space
An introduction to the plasma state in nature and in space Dr. L. Conde Departamento de Física Aplicada E.T.S. Ingenieros Aeronáuticos Universidad Politécnica de Madrid The plasma state of condensed matter
More informationEarth 110 Exploration of the Solar System Assignment 4: Jovian Planets Due in class Tuesday, Feb. 23, 2016
Name: Section: Earth 110 Exploration of the Solar System Assignment 4: Jovian Planets Due in class Tuesday, Feb. 23, 2016 The jovian planets have distinct characteristics that set them apart from the terrestrial
More informationSHORT, HIGH CURRENT ELECTRODYNAMIC TETHER. N.A.Savich Institute of Radio Engineering and Electronics Russian Academy of Science, Moscow, Russia
SHORT, HIGH CURRENT ELECTRODYNAMIC TETHER N.A.Savich Institute of Radio Engineering and Electronics Russian Academy of Science, Moscow, Russia J.R.Sanmartin E.T.S.I. Aeronauticos, Universidad Politecnia,
More informationON THE THRUST CAPABILITY OF ELECTRODYNAMIC TETHERS WORKING IN GENERATOR MODE
AA 09-4 ON THE THRUT APABILITY O ELETRODYNAMI TETHER WORKING IN GENERATOR MODE laudio Bombardelli and Jesus Pelaez The problem of estimating the necessary conditions under which a passive electrodynamic
More informationarxiv: v1 [gr-qc] 7 Oct 2009
Earth Flyby Anomalies Michael Martin Nieto 1 and John D. Anderson 2 Michael Martin Nieto is a fellow at Los Alamos National Laboratory and John D. Anderson is a senior research scientist emeritus at the
More information9.2 Worksheet #3 - Circular and Satellite Motion
9.2 Worksheet #3 - Circular and Satellite Motion 1. A car just becomes airborne as it comes off the crest of a bridge that has circular cross section of radius 78.0 m. What is the speed of the car? 2.
More informationDiscovery and Surprise from Entry Probes to Giant Planets
Discovery and Surprise from Entry Probes to Giant Planets Thomas R. Spilker 2014 June 14 11th International Planetary Probes Workshop Short Course Pasadena, CA, USA TRS-1 TRS-2 Planet Characteristic Mass
More informationNASA Future Magnetospheric Missions. J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC
NASA Future Magnetospheric Missions J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC Future Magnetospheric Missions Strategic Missions Radiation Belt Storm Probes (LWS/2011) Magnetospheric
More informationMAE 180A: Spacecraft Guidance I, Summer 2009 Homework 4 Due Thursday, July 30.
MAE 180A: Spacecraft Guidance I, Summer 2009 Homework 4 Due Thursday, July 30. Guidelines: Please turn in a neat and clean homework that gives all the formulae that you have used as well as details that
More informationJupiter and its Moons
Jupiter and its Moons Summary 1. At an average distance of over 5 AU, Jupiter takes nearly 12 years to orbit the Sun 2. Jupiter is by far the largest and most massive planet in the solar system being over
More informationChapter 11 Jovian Planet Systems
Chapter 11 Jovian Planet Systems 11.1 A Different Kind of Planet Our goals for learning: Are jovian planets all alike? What are jovian planets like on the inside? What is the weather like on jovian planets?
More informationChapter 11 Jovian Planet Systems. Jovian Planet Composition. Are jovian planets all alike? Density Differences. Density Differences
Chapter 11 Jovian Planet Systems 11.1 A Different Kind of Planet Our goals for learning:! Are jovian planets all alike?! What are jovian planets like on the inside?! What is the weather like on jovian
More informationEuropa Exploration: Challenges and Solutions
Europa Exploration: Challenges and Solutions T. V. Johnson 1, K. Clark 1, R. Greeley 2, R. Pappalardo 1,3 1 Jet Propulsion Laboratory, Pasadena, CA, 2 Arizona State University, Tempe AZ, 3 U. of Colorado,
More informationMoons of Sol Lecture 13 3/5/2018
Moons of Sol Lecture 13 3/5/2018 Tidal locking We always see the same face of the Moon. This means: period of orbit = period of spin Top view of Moon orbiting Earth Earth Why? The tidal bulge in the solid
More informationJovian Meteoroid Environment Model JMEM: Dust from the Galilean Satellites
Jovian Meteoroid Environment Model JMEM: Dust from the Galilean Satellites J. Schmidt, X. Liu (U Oulu) M. Sachse, F. Spahn (U Potsdam) R. Soja, R. Srama (U Stuttgart) N. Altobelli, C. Vallat (ESA) (images:
More informationScott Bolton OPAG February 1, 2016
Scott Bolton OPAG February 1, 2016 Juno Status Launched August 2011 Earth flyby October 2013 Jupiter arrival July 4, 2016 Spacecraft is healthy and all instruments are working. Juno Science Juno Science
More informationChapter 11 Lecture. The Cosmic Perspective Seventh Edition. Jovian Planet Systems Pearson Education, Inc.
Chapter 11 Lecture The Cosmic Perspective Seventh Edition Jovian Planet Systems Jovian Planet Systems 11.1 A Different Kind of Planet Our goals for learning: Are jovian planets all alike? What are jovian
More informationS E C T I O N 8 T H E T O U R
S E C T I O N 8 T H E T O U R The Jovian tour is much more that just a series of targeted encounters with the Galilean satellites. The tour is the culmination of a strategy developed over 20 years ago
More informationAstronomy 1140 Quiz 4 Review
Astronomy 1140 Quiz 4 Review Anil Pradhan November 16, 2017 I Jupiter 1. How do Jupiter s mass, size, day and year compare to Earth s? Mass: 318 Earth masses (or about 1/1000th the mass of the Sun). Radius:
More informationJuno Status and Earth Flyby Plans. C. J. Hansen
Juno Status and Earth Flyby Plans C. J. Hansen July 2013 Juno will improve our understanding of the history of the solar system by investigating the origin and evolution of Jupiter. To accomplish this
More informationChapter 11 Jovian Planet Systems. Jovian Planet Composition. Are jovian planets all alike? Density Differences. Density Differences
Chapter 11 Jovian Planet Systems 11.1 A Different Kind of Planet Our goals for learning Are jovian planets all alike? What are jovian planets like on the inside? What is the weather like on jovian planets?
More informationScience Scenario Modeling
Science Scenario Modeling Rob Lock, Erick Sturm, Tracy Van Houten Presented to OPAG Satellite Break-out Group February 2010 Introduction Scenario Strategy For Europa Explorer and Jupiter Europa Orbiter
More informationSatellite Components & Systems. Dr. Ugur GUVEN Aerospace Engineer (P.hD) Nuclear Science & Technology Engineer (M.Sc)
Satellite Components & Systems Dr. Ugur GUVEN Aerospace Engineer (P.hD) Nuclear Science & Technology Engineer (M.Sc) Definitions Attitude: The way the satellite is inclined toward Earth at a certain inclination
More informationThe Fathers of the Gods: Jupiter and Saturn
The Fathers of the Gods: Jupiter and Saturn Learning Objectives! Order all the planets by size and distance from the Sun! How are clouds on Jupiter (and Saturn) different to the Earth? What 2 factors drive
More informationSolar System. The Jovian Satellites. Regular vs. Irregular Satellites. Jovian satellites reside beyond the frost line
The Jovian Satellites Satellites are common around Jovian planets Some are as large as Mercury, & thus are like planets Some have atmospheres Discovery of the first Jovian satellites In 1610, Galileo discovered
More informationUnderstanding Motion, Energy & Gravity
Speed, Velocity & Acceleration Understanding Motion, Energy & Gravity Chapter 4 speed: distance traveled per unit time (e.g., m/s, mph, km/ hr) velocity: speed & direction acceleration: change in velocity
More informationUnderstanding Motion, Energy & Gravity
Speed, Velocity & Acceleration Understanding Motion, Energy & Gravity Chapter 4 speed: distance traveled per unit time (e.g., m/s, mph, km/ hr) velocity: speed & direction acceleration: change in velocity
More informationChapter 8 Jovian Planet Systems
Chapter 8 Jovian Planet Systems How do jovian planets differ from terrestrials? They are much larger than terrestrial planets They do not have solid surfaces The things they are made of are quite different
More informationBravoSat: Optimizing the Delta-V Capability of a CubeSat Mission. with Novel Plasma Propulsion Technology ISSC 2013
BravoSat: Optimizing the Delta-V Capability of a CubeSat Mission with Novel Plasma Propulsion Technology Sara Spangelo, NASA JPL, Caltech Benjamin Longmier, University of Michigan Interplanetary Small
More informationChapter 8 Jovian Planet Systems
Chapter 8 Jovian Planet Systems 8.1 A Different Kind of Planet Goals for learning: How are jovian planets different from terrestrials? What are jovian planets made of? What are jovian planets like on the
More informationProbing planetary interiors by spacecraft orbital observations
Probing planetary interiors by spacecraft orbital observations Alexander Stark, Jürgen Oberst, Frank Preusker, Klaus Gwinner, Gregor Steinbrügge, Hauke Hussmann Funded by Deutsche Forschungsgemeinschaft
More informationLEARNING ABOUT THE OUTER PLANETS. NASA's Cassini spacecraft. Io Above Jupiter s Clouds on New Year's Day, Credit: NASA/JPL/University of Arizona
LEARNING ABOUT THE OUTER PLANETS Can see basic features through Earth-based telescopes. Hubble Space Telescope especially useful because of sharp imaging. Distances from Kepler s 3 rd law, diameters from
More informationThe Interaction of the Atmosphere of Enceladus with Saturn s Plasma
LA-UR-05-7699 The Interaction of the Atmosphere of Enceladus with Saturn s Plasma R.L.Tokar 1, R.E.Johnson 2, T.W.Hill 3, D.H.Pontius 4, W.S. Kurth 5, F. J.Crary 6, D.T. Young 6, M.F. Thomsen 1, D.B.Reisenfeld
More informationSpace Environments and Effects Section. Pioneer. Voyager. New Horizons. D.J. Rodgers ESA-ESTEC, The Netherlands
Pioneer Voyager New Horizons D.J. Rodgers ESA-ESTEC, The Netherlands 20 January EJSM/Laplace instruments workshop 1 Possible launch 2020 Spacecraft Jupiter Europa Orbiter Jupiter Ganymede Orbiter Ganymede
More informationDavid versus Goliath 1
David versus Goliath 1 or A Comparison of the Magnetospheres between Jupiter and Earth 1 David and Goliath is a story from the Bible that is about a normal man (David) who meets a giant (Goliath) Tomas
More informationINTERSTELLAR PRECURSOR MISSIONS USING ADVANCED DUAL-STAGE ION PROPULSION SYSTEMS
INTERSTELLAR PRECURSOR MISSIONS USING ADVANCED DUAL-STAGE ION PROPULSION SYSTEMS David G Fearn, 23 Bowenhurst Road, Church Crookham, Fleet, Hants, GU52 6HS, UK dg.fearn@virgin.net Roger Walker Advanced
More informationTheory and Modeling (High Performance Simulation)
Theory and Modeling (High Performance Simulation) Mater. Res. Soc. Symp. Proc. Vol. 929 2006 Materials Research Society 0929-1101-01 Radiation Shielding Analysis for Various Materials in the Extreme Jovian
More informationCassini observations of the thermal plasma in the vicinity of Saturn s main rings and the F and G rings
GEOPHYSICAL RESEARCH LETTERS, VOL. 32, L14S04, doi:10.1029/2005gl022690, 2005 Cassini observations of the thermal plasma in the vicinity of Saturn s main rings and the F and G rings R. L. Tokar, 1 R. E.
More informationOn the formation of the Martian moons from a circum-mars accretion disk
ROYAL OBSERVATORY OF BELGIUM On the formation of the Martian moons from a circum-mars accretion disk Rosenblatt P. and Charnoz S. 46 th ESLAB Symposium: Formation and evolution of moons Session 2 Mechanism
More informationSolar System. The Jovian Satellites. Regular vs. Irregular Satellites. Jovian satellites reside beyond the frost line
The Jovian Satellites Satellites are common around Jovian planets Some are as large as Mercury, & thus are like planets Some have atmospheres Discovery of the first Jovian satellites In 1610, Galileo discovered
More informationOuter Solar System. Jupiter. PHY outer-solar-system - J. Hedberg
Outer Solar System 1. Jupiter 1. Pressure & Density & size 2. Jupiter's Magnetosphere 3. Juno Mission 4. Jovian Satellites 2. Saturn 1. The Rings! 2. Saturn's Moons 3. Titan 3. Uranus 4. Neptune 5. Dwarf
More informationLaunch Period Development for the Juno Mission to Jupiter
AIAA/AAS Astrodynamics Specialist Conference and Exhibit 18-21 August 2008, Honolulu, Hawaii AIAA 2008-7369 Launch Period Development for the Juno Mission to Jupiter Theresa D. Kowalkowski *, Jennie R.
More information12. Jovian Planet Systems Pearson Education Inc., publishing as Addison Wesley
12. Jovian Planet Systems Jovian Planet Properties Compared to the terrestrial planets, the Jovians: are much larger & more massive 2. are composed mostly of Hydrogen, Helium, & Hydrogen compounds 3. have
More informationAstronomy Ch. 11 Jupiter. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 11 Jupiter MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) Jupiter is noticeably oblate because: A) it has a
More informationJUICE/Laplace Mission Summary & Status
JUICE/Laplace Mission Summary & Status C. Erd JUICE Instrument WS, Darmstadt 9/11/2011 Activities during the Reformulation Phase 1. Feasible JGO s/c as a starting point a. no re-design of s/c necessary
More informationChapter 8 Jovian Planet Systems
Chapter 8 Jovian Planet Systems How do jovian planets differ from terrestrials? They are much larger than terrestrial planets They do not have solid surfaces The things they are made of are quite different
More informationJuno Update for OPAG. Steve Levin Juno Project Scien8st September 7, 2017
Juno Update for OPAG Steve Levin Juno Project Scien8st September 7, 2017 Juno Mission Overview Salient Features: First solar-powered mission to Jupiter Eight science instruments to conduct gravity, magnetic
More informationDesign of Orbits and Spacecraft Systems Engineering. Scott Schoneman 13 November 03
Design of Orbits and Spacecraft Systems Engineering Scott Schoneman 13 November 03 Introduction Why did satellites or spacecraft in the space run in this orbit, not in that orbit? How do we design the
More informationElectrodynamic Tether at Jupiter I: Capture Operation and Constraints
Electrodynamic Tether at Jupiter I: Capture Operation and Constraints Juan R. Sanmartin, Mario Charro, Enrico C. orenzini, Henry B. Garrett, Claudio Bombardelli, and Cristina Bramanti Abstract Tethered
More informationThe Interior of Giant Planets. Cyrill Milkau
The Interior of Giant Planets Cyrill Milkau 01.12.15 Outline 1. What is a planet? 2. Nuclear fusion 3. Properties of Jupiter 4. Summary 5. Sources Cyrill Milkau 2 1. What is a Planet? Definition by International
More informationELECTRODYNAMIC TETHERS FOR SPACECRAFT PROPULSION
ELECTRODYNAMIC TETHERS FOR SPACECRAFT PROPULSION Les Johnson Mail Code PS02, NASA Marshall Space Flight Center Huntsville.AL 35812 205-544-0614 (phone); 205-544-6669 (fax) Robert D. Estes* and Enrico Lorenzmi*
More informationLecture 23: Jupiter. Solar System. Jupiter s Orbit. The semi-major axis of Jupiter s orbit is a = 5.2 AU
Lecture 23: Jupiter Solar System Jupiter s Orbit The semi-major axis of Jupiter s orbit is a = 5.2 AU Jupiter Sun a Kepler s third law relates the semi-major axis to the orbital period 1 Jupiter s Orbit
More informationESA s Cosmic Vision Programme: Outer Planet Mission Studies
ESA s Cosmic Vision Programme: Outer Planet Mission Studies Jean-Pierre LEBRETON (ESA s EJSM and TSSM Study Scientist) Europa Lander workshop IKI, Moscow, 9-13 February 2009 ESA/ESTEC, Noordwijk, Pays-Bas
More informationOptimal Gravity Assisted Orbit Insertion for Europa Orbiter Mission
Optimal Gravity Assisted Orbit Insertion for Europa Orbiter Mission Deepak Gaur 1, M. S. Prasad 2 1 M. Tech. (Avionics), Amity Institute of Space Science and Technology, Amity University, Noida, U.P.,
More informationPlanetary Protection Trajectory Analysis for the Juno Mission
AIAA/AAS Astrodynamics Specialist Conference and Exhibit 18-21 August 2008, Honolulu, Hawaii AIAA 2008-7368 Planetary Protection Trajectory Analysis for the Juno Mission Try Lam 1, Jennie R. Johannesen
More informationScience in the news Voyager s 11 billion mile journey
Name:... Date:... Read the article from The Week magazine Voyager s 11 billion mile journey. The Voyager 1 spacecraft was launched on the 5 th September 1977. Together with Voyager 2, which was launched
More informationJovian radiation models for JUICE mission
Jovian radiation models for JUICE mission Hugh Evans and David Rodgers 19/09/2016 ESA UNCLASSIFIED - For Official Use Hugh Evans ESTEC 19/09/2016 Slide 1 ESA UNCLASSIFIED - For Official Use The Jovian
More informationAstrodynamics (AERO0024)
Astrodynamics (AERO0024) 10. Interplanetary Trajectories Gaëtan Kerschen Space Structures & Systems Lab (S3L) Motivation 2 6. Interplanetary Trajectories 6.1 Patched conic method 6.2 Lambert s problem
More informationTenuous ring formation by the capture of interplanetary dust at Saturn
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 110,, doi:10.1029/2004ja010577, 2005 Tenuous ring formation by the capture of interplanetary dust at Saturn C. J. Mitchell, 1 J. E. Colwell, and M. Horányi 1 Laboratory
More informationTilts and Obliquities!
Fran Bagenal! University of Colorado! Tilts and Obliquities! Offset Tilted Dipole Approximation Earth Stanley & Bloxham 2006 Jupiter Saturn B radial @ surface Uranus Neptune Magnetic Potential 3-D harmonics
More informationDesign of low energy space missions using dynamical systems theory
C C Dynamical A L T E C S H Design of low energy space missions using dynamical systems theory Shane D. Ross Control and Dynamical Systems, Caltech www.cds.caltech.edu/ shane Collaborators: J.E. Marsden
More informationAstronomy. physics.wm.edu/~hancock/171/ A. Dayle Hancock. Small 239. Office hours: MTWR 10-11am. Page 1
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Planetology I Terrestrial and Jovian planets Similarities/differences between planetary satellites Surface and atmosphere
More informationSpace Physics. An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres. May-Britt Kallenrode. Springer
May-Britt Kallenrode Space Physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres With 170 Figures, 9 Tables, Numerous Exercises and Problems Springer Contents 1. Introduction
More informationGravitational Potential Energy and Total Energy *
OpenStax-CNX module: m58347 Gravitational Potential Energy and Total Energy * OpenStax This work is produced by OpenStax-CNX and licensed under the Creative Commons Attribution License 4.0 By the end of
More informationChapter 11 Jovian Planet Systems
Chapter 11 Jovian Planet Systems 11.1 A Different Kind of Planet Our goals for learning: Are jovian planets all alike? What are jovian planets like on the inside? What is the weather like on jovian planets?
More informationRadiation: Lessons Learned
Radiation: Lessons Learned Scott Bolton Southwest Research Institute Insoo Jun Jet Propulsion Laboratory This document has been reviewed for export control and it does NOT contain controlled technical
More informationLecture #27: Saturn. The Main Point. The Jovian Planets. Basic Properties of Saturn. Saturn:
Lecture #27: Saturn Saturn: General properties. Atmosphere. Interior. Origin and evolution. Reading: Chapters 7.1 (Saturn) and 11.1. The Main Point Saturn is a large Jovian-class planet with a composition
More informationChapter 14 Satellite Motion
1 Academic Physics Mechanics Chapter 14 Satellite Motion The Mechanical Universe Kepler's Three Laws (Episode 21) The Kepler Problem (Episode 22) Energy and Eccentricity (Episode 23) Navigating in Space
More informationJupiter and Saturn. Guiding Questions. Long orbital periods of Jupiter and Saturn cause favorable viewing times to shift
Jupiter and Saturn 1 2 Guiding Questions 1. Why is the best month to see Jupiter different from one year to the next? 2. Why are there important differences between the atmospheres of Jupiter and Saturn?
More informationActa Futura - Issue 2
ACT-PUB-AF0502 Acta Futura - Issue 2 Special Issue on Innovative System Concepts Editor: Dr. Dario Izzo Acta Futura: From ESA's Advanced Concepts Team Advanced Concepts Team http://www.esa.int/act a Contents
More information10/6/16. Observing the Universe with Gravitational Waves
Lecture Outline Observing the Universe with Gravitational Waves Thursday, October 13 7:00 PM Bell Museum Auditorium This event is free and open to the public, and will be followed by telescope observing.
More informationTides and Lagrange Points
Ast111, Lecture 3a Tides and Lagrange Points Arial view of Tidal surge in Alaska (S. Sharnoff) Tides Tidal disruption Lagrange Points Tadpole Orbits and Trojans Tidal Bulges Tides Tidal Force The force
More informationCold plasma in the jovian system
Cold plasma in the jovian system Chris Arridge 1,2 and the JuMMP Consortium 1. Mullard Space Science Laboratory, Department of Space and Climate Physics, University College London, UK. 2. The Centre for
More informationCHAPTER 6. The Solar System
CHAPTER 6 The Solar System 6.1 An Inventory of the Solar System The Greeks knew about 5 planets other than Earth They also knew about two other objects that were not planets or stars: meteors and comets
More informationJUpiter Icy Moons Explorer (JUICE) Status report for OPAG. O. Witasse and N. Altobelli. JUICE artist impression (Credits ESA, AOES)
JUpiter Icy Moons Explorer (JUICE) Status report for OPAG O. Witasse and N. Altobelli JUICE artist impression (Credits ESA, AOES) Jupiter Icy Moons Explorer MISSION SCIENCE (1/3) EXPLORATION OF HABITABLE
More informationThe Galilean Satellites. Jupiter has four planetary-sized moons first seen by Galileo and easily visible in binoculars.
1 The Galilean Satellites Jupiter has four planetary-sized moons first seen by Galileo and easily visible in binoculars. 2 The Galilean Satellites Jupiter has four planetary-sized moons first seen by Galileo
More information