Valuation of On-Orbit Servicing in Proliferated Low-Earth Orbit Constellations
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6 Orbit Relative to the Sun. Crossing Times
6 Orbit Relative to the Sun. Crossing Times We begin by studying the position of the orbit and ground track of an arbi- trary satellite relative to the direction of the Sun. We then turn more specif- ically to Sun-synchronous satellites for which this relative position provides the very definition of their orbit. 6.1 Cycle with Respect to the Sun 6.1.1 Crossing Time At a given time, it is useful to know the local time on the ground track, i.e., the LMT, deduced in a straightforward manner from the UT once the longitude of the place is given, using (4.49). The local mean time (LMT) on the ground track at this given time is called the crossing time or local crossing time. To obtain the local apparent time (LAT), one must know the day of the year to specify the equation of time ET. In all matters involving the position of the Sun (elevation and azimuth) relative to a local frame, this is the time that should be used. The ground track of the satellite can be represented by giving the crossing time. We have chosen to represent the LMT using colour on Colour Plates IIb, IIIb and VII to XI. For Sun-synchronous satellites such as MetOp-1, it is clear that the cross- ing time (in the ascending or descending direction) depends only on the latitude. At a given place (except near the poles), one crossing occurs during the day, the other at night. For the HEO of the Ellipso Borealis satellite, the stability of the crossing time also shows up clearly. -
Astrodynamics
Politecnico di Torino SEEDS SpacE Exploration and Development Systems Astrodynamics II Edition 2006 - 07 - Ver. 2.0.1 Author: Guido Colasurdo Dipartimento di Energetica Teacher: Giulio Avanzini Dipartimento di Ingegneria Aeronautica e Spaziale e-mail: [email protected] Contents 1 Two–Body Orbital Mechanics 1 1.1 BirthofAstrodynamics: Kepler’sLaws. ......... 1 1.2 Newton’sLawsofMotion ............................ ... 2 1.3 Newton’s Law of Universal Gravitation . ......... 3 1.4 The n–BodyProblem ................................. 4 1.5 Equation of Motion in the Two-Body Problem . ....... 5 1.6 PotentialEnergy ................................. ... 6 1.7 ConstantsoftheMotion . .. .. .. .. .. .. .. .. .... 7 1.8 TrajectoryEquation .............................. .... 8 1.9 ConicSections ................................... 8 1.10 Relating Energy and Semi-major Axis . ........ 9 2 Two-Dimensional Analysis of Motion 11 2.1 ReferenceFrames................................. 11 2.2 Velocity and acceleration components . ......... 12 2.3 First-Order Scalar Equations of Motion . ......... 12 2.4 PerifocalReferenceFrame . ...... 13 2.5 FlightPathAngle ................................. 14 2.6 EllipticalOrbits................................ ..... 15 2.6.1 Geometry of an Elliptical Orbit . ..... 15 2.6.2 Period of an Elliptical Orbit . ..... 16 2.7 Time–of–Flight on the Elliptical Orbit . .......... 16 2.8 Extensiontohyperbolaandparabola. ........ 18 2.9 Circular and Escape Velocity, Hyperbolic Excess Speed . .............. 18 2.10 CosmicVelocities -
Evolution of the Rendezvous-Maneuver Plan for Lunar-Landing Missions
NASA TECHNICAL NOTE NASA TN D-7388 00 00 APOLLO EXPERIENCE REPORT - EVOLUTION OF THE RENDEZVOUS-MANEUVER PLAN FOR LUNAR-LANDING MISSIONS by Jumes D. Alexunder und Robert We Becker Lyndon B, Johnson Spuce Center ffoaston, Texus 77058 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON, D. C. AUGUST 1973 1. Report No. 2. Government Accession No, 3. Recipient's Catalog No. NASA TN D-7388 4. Title and Subtitle 5. Report Date APOLLOEXPERIENCEREPORT August 1973 EVOLUTIONOFTHERENDEZVOUS-MANEUVERPLAN 6. Performing Organizatlon Code FOR THE LUNAR-LANDING MISSIONS 7. Author(s) 8. Performing Organization Report No. James D. Alexander and Robert W. Becker, JSC JSC S-334 10. Work Unit No. 9. Performing Organization Name and Address I - 924-22-20- 00- 72 Lyndon B. Johnson Space Center 11. Contract or Grant No. Houston, Texas 77058 13. Type of Report and Period Covered 12. Sponsoring Agency Name and Address Technical Note I National Aeronautics and Space Administration 14. Sponsoring Agency Code Washington, D. C. 20546 I 15. Supplementary Notes The JSC Director waived the use of the International System of Units (SI) for this Apollo Experience I Report because, in his judgment, the use of SI units would impair the usefulness of the report or I I result in excessive cost. 16. Abstract The evolution of the nominal rendezvous-maneuver plan for the lunar landing missions is presented along with a summary of the significant developments for the lunar module abort and rescue plan. A general discussion of the rendezvous dispersion analysis that was conducted in support of both the nominal and contingency rendezvous planning is included. -
Some Special Types of Orbits Around Jupiter
aerospace Article Some Special Types of Orbits around Jupiter Yongjie Liu 1, Yu Jiang 1,*, Hengnian Li 1,2,* and Hui Zhang 1 1 State Key Laboratory of Astronautic Dynamics, Xi’an Satellite Control Center, Xi’an 710043, China; [email protected] (Y.L.); [email protected] (H.Z.) 2 School of Electronic and Information Engineering, Xi’an Jiaotong University, Xi’an 710049, China * Correspondence: [email protected] (Y.J.); [email protected] (H.L.) Abstract: This paper intends to show some special types of orbits around Jupiter based on the mean element theory, including stationary orbits, sun-synchronous orbits, orbits at the critical inclination, and repeating ground track orbits. A gravity model concerning only the perturbations of J2 and J4 terms is used here. Compared with special orbits around the Earth, the orbit dynamics differ greatly: (1) There do not exist longitude drifts on stationary orbits due to non-spherical gravity since only J2 and J4 terms are taken into account in the gravity model. All points on stationary orbits are degenerate equilibrium points. Moreover, the satellite will oscillate in the radial and North-South directions after a sufficiently small perturbation of stationary orbits. (2) The inclinations of sun-synchronous orbits are always bigger than 90 degrees, but smaller than those for satellites around the Earth. (3) The critical inclinations are no-longer independent of the semi-major axis and eccentricity of the orbits. The results show that if the eccentricity is small, the critical inclinations will decrease as the altitudes of orbits increase; if the eccentricity is larger, the critical inclinations will increase as the altitudes of orbits increase. -
Tilting Saturn II. Numerical Model
Tilting Saturn II. Numerical Model Douglas P. Hamilton Astronomy Department, University of Maryland College Park, MD 20742 [email protected] and William R. Ward Southwest Research Institute Boulder, CO 80303 [email protected] Received ; accepted Submitted to the Astronomical Journal, December 2003 Resubmitted to the Astronomical Journal, June 2004 – 2 – ABSTRACT We argue that the gas giants Jupiter and Saturn were both formed with their rotation axes nearly perpendicular to their orbital planes, and that the large cur- rent tilt of the ringed planet was acquired in a post formation event. We identify the responsible mechanism as trapping into a secular spin-orbit resonance which couples the angular momentum of Saturn’s rotation to that of Neptune’s orbit. Strong support for this model comes from i) a near match between the precession frequencies of Saturn’s pole and the orbital pole of Neptune and ii) the current directions that these poles point in space. We show, with direct numerical inte- grations, that trapping into the spin-orbit resonance and the associated growth in Saturn’s obliquity is not disrupted by other planetary perturbations. Subject headings: planets and satellites: individual (Saturn, Neptune) — Solar System: formation — Solar System: general 1. INTRODUCTION The formation of the Solar System is thought to have begun with a cold interstellar gas cloud that collapsed under its own self-gravity. Angular momentum was preserved during the process so that the young Sun was initially surrounded by the Solar Nebula, a spinning disk of gas and dust. From this disk, planets formed in a sequence of stages whose details are still not fully understood. -
Orbital Dynamics and Numerical N-Body Simulations of Extrasolar Moons and Giant Planets
ORBITAL DYNAMICS AND NUMERICAL N-BODY SIMULATIONS OF EXTRASOLAR MOONS AND GIANT PLANETS. A Dissertation Presented to the Faculty of the Graduate School of Cornell University in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy by Yu-Cian Hong August 2019 c 2019 Yu-Cian Hong ALL RIGHTS RESERVED ORBITAL DYNAMICS AND NUMERICAL N-BODY SIMULATIONS OF EXTRASOLAR MOONS AND GIANT PLANETS. Yu-Cian Hong, Ph.D. Cornell University 2019 This thesis work focuses on computational orbital dynamics of exomoons and exoplanets. Exomoons are highly sought-after astrobiological targets. Two can- didates have been discovered to-date (Bennett et al., 2014, Teachey & Kipping, 2018). We developed the first N-body integrator that can handle exomoon orbits in close planet-planet interactions, for the following three projects. (1) Instability of moons around non-oblate planets associated with slowed nodal precession and resonances with stars.This work reversed the commonsensical notion that spinning giant planets should be oblate. Moons around spherical planets were destabilized by 3:2 and 1:1 resonance overlap or the chaotic zone around 1:1 resonance between the orbital precession of the moons and the star. Normally, the torque from planet oblateness keeps the orbit of close-in moons precess fast ( period ∼ 7 yr for Io). Without planet oblateness, Io?s precession period is much longer (∼ 104 yr), which allowed resonance with the star, thus the in- stability. Therefore, realistic treatment of planet oblateness is critical in moon dynamics. (2) Orbital stability of moons in planet-planet scattering. Planet- planet scattering is the best model to date for explaining the eccentricity distri- bution of exoplanets. -
Low Earth Orbit Slotting for Space Traffic Management Using Flower
Low Earth Orbit Slotting for Space Traffic Management Using Flower Constellation Theory David Arnas∗, Miles Lifson†, and Richard Linares‡ Massachusetts Institute of Technology, Cambridge, MA, 02139, USA Martín E. Avendaño§ CUD-AGM (Zaragoza), Crtra Huesca s / n, Zaragoza, 50090, Spain This paper proposes the use of Flower Constellation (FC) theory to facilitate the design of a Low Earth Orbit (LEO) slotting system to avoid collisions between compliant satellites and optimize the available space. Specifically, it proposes the use of concentric orbital shells of admissible “slots” with stacked intersecting orbits that preserve a minimum separation distance between satellites at all times. The problem is formulated in mathematical terms and three approaches are explored: random constellations, single 2D Lattice Flower Constellations (2D-LFCs), and unions of 2D-LFCs. Each approach is evaluated in terms of several metrics including capacity, Earth coverage, orbits per shell, and symmetries. In particular, capacity is evaluated for various inclinations and other parameters. Next, a rough estimate for the capacity of LEO is generated subject to certain minimum separation and station-keeping assumptions and several trade-offs are identified to guide policy-makers interested in the adoption of a LEO slotting scheme for space traffic management. I. Introduction SpaceX, OneWeb, Telesat and other companies are currently planning mega-constellations for space-based internet connectivity and other applications that would significantly increase the number of on-orbit active satellites across a variety of altitudes [1–5]. As these and other actors seek to make more intensive use of the global space commons, there is growing need to characterize the fundamental limits to the capacity of Low Earth Orbit (LEO), particularly in high-demand orbits and altitudes, and minimize the extent to which use by one space actor hampers use by other actors. -
Lunar Orbiting Cubesat Sensor Transport System Mike Seibert, Alejandro Levi, and Mitchell Paradis Graduate Students, Colorado School of Mines
Lunar Orbiting CubeSat Sensor Transport System Mike Seibert, Alejandro Levi, and Mitchell Paradis Graduate Students, Colorado School of Mines Concept Origin Notional Mission Evaluated Carrier Spacecraft Conceptual Design The 2018 Lunar Polar Prospecting (LPP) Workshop Objective: • Structure: Based on EELV Secondary generated a series of recommendations for Deploy a constellation of 6 sensor spacecraft in single Payload Adapter (ESPA) Grande. prospecting of lunar water. Recommendation 3 was polar low lunar orbit plane. • Propulsion: Monoprop system with 2.5 km/s for swarms CubeSats overflying polar regions at delta-V capability. altitudes below 20 km. Recommendation 3 also Cruise Phase: Includes 179 m/s for 110 days of recommended “a swarm of hundreds of low cost LOCuST is released from the launch vehicle in a GTO. orbit eccentricity control impactors instrumented for volatile detection and A series of perigee maneuvers using carrier spacecraft • Earth Telecom: Optical derived from LADEE or quantification.” [1] propulsion are used to raise apogee to lunar distance. IRIS Version 2.0 radio • Relay Telecom: IRIS Version 2.0 (multiple if all RF) The graduate student team developed both mission Lunar Orbit Insertion/Optimization • Thermal control:Accounts for challenges of low and vehicle designs that address the LPP Lunar orbit capture into an initial 200km altitude orbit over lunar day side. recommendation during the Space Resources Design I polar orbit. Orbit is lowered to 10km altitude Main Propulsion course at the Colorado School of Mines in Spring perilune, 100km apolune. All capture and initial 2019. CubeSat optimization maneuvers use carrier spacecraft Deployers propulsion. The CubeSat swarm concept was interpreted to mean a constellation of small short mission duration Deployments spacecraft with sensors optimized for localizing After each deployment orbit phasing maneuvers to Solar Array surface water ice. -
Astro 250: Solutions to Problem Set 5 by Eugene Chiang
Astro 250: Solutions to Problem Set 5 by Eugene Chiang Problem 1. Precessing Planes and the Invariable Plane Consider a star of mass mc orbited by two planets on nearly circular orbits. The mass and semi-major axis of the inner planet are m1 and a1, respectively, and those of the outer planet, m2 = (1/2) × m1 and a2 = 4 × a1. The mutual inclination between the two orbits is i 1. This problem explores the inclination and nodal behavior of the two planets. a) What is the inclination of each planet with respect to the invariable plane of the system? The invariable plane is perpendicular to the total (vector) angular momentum of all planetary orbits. Neglect the contribution of orbital eccentricity to the angular momentum. Call these inclinations i1 and i2. The masses and semi-major axes of the two planets are so chosen as to make the arithmetic easy;√ the norm of each planet’s angular momentum is the same as the other, |~l1| = |~l2| = m1 Gmca1. Orient the x-y axes in the invariable plane so that the y-axis lies along the line of intersection between the two orbit planes (the nodal line). Then in the x-z plane, the total angular momentum vector lies along the z-axis, while ~l1 lies (say) in quadrant II and makes an angle with respect to the z-axis of i1 > 0, while l~2 lies in quadrant I and makes an angle with respect to the z-axis of i2 > 0. Remember that the mutual inclination i = i1 + i2. -
ISTS-2017-D-110ⅠISSFD-2017-110
50,000 Laps Around Mars: Navigating the Mars Reconnaissance Orbiter Through the Extended Missions (January 2009 – March 2017) By Premkumar MENON,1) Sean WAGNER,1) Stuart DEMCAK,1) David JEFFERSON,1) Eric GRAAT,1) Kyong LEE,1) and William SCHULZE1) 1)Jet Propulsion Laboratory, California Institute of Technology, USA (Received May 25th, 2017) Orbiting Mars since March 2006, the Mars Reconnaissance Orbiter (MRO) spacecraft continues to perform valuable science observations, provide telecommunication relay for surface assets, and characterize landing sites for future missions. Previous papers reported on the navigation of MRO from interplanetary cruise through the end of the Primary Science Phase in December 2008. This paper highlights the navigation of MRO from January 2009 through March 2017, covering the Extended Science Phase, the first three extended missions, and a portion of the fourth extended mission. The MRO mission returned over 300 terabytes of data since beginning primary science operations in November 2006. Key Words: Navigation, orbit determination, propulsive maneuvers, reconstruction, phasing 1. Introduction Siding Spring at Mars in October 20144) and imaged the Exo- Mars lander Schiaparelli in October 2016.5,6) MRO plans to The Mars Reconnaissance Orbiter spacecraft launched from provide telecommunication support for the Entry, Descent, and Cape Canaveral Air Force Station on August 12, 2005. MRO Landing (EDL) phase of NASA’s InSight mission in November entered orbit around Mars on March 10, 2006 following an in- 2018 and NASA’s Mars 2020 mission in February 2021. terplanetary cruise of seven months. After five months of aer- obraking and three months of transition to the Primary Sci- 2.1. -
Retrograde-Rotating Exoplanets Experience Obliquity Excitations in an Eccentricity- Enabled Resonance
The Planetary Science Journal, 1:8 (15pp), 2020 June https://doi.org/10.3847/PSJ/ab8198 © 2020. The Author(s). Published by the American Astronomical Society. Retrograde-rotating Exoplanets Experience Obliquity Excitations in an Eccentricity- enabled Resonance Steven M. Kreyche1 , Jason W. Barnes1 , Billy L. Quarles2 , Jack J. Lissauer3 , John E. Chambers4, and Matthew M. Hedman1 1 Department of Physics, University of Idaho, Moscow, ID, USA; [email protected] 2 Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA, USA 3 Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, CA, USA 4 Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC, USA Received 2019 December 2; revised 2020 February 28; accepted 2020 March 18; published 2020 April 14 Abstract Previous studies have shown that planets that rotate retrograde (backward with respect to their orbital motion) generally experience less severe obliquity variations than those that rotate prograde (the same direction as their orbital motion). Here, we examine retrograde-rotating planets on eccentric orbits and find a previously unknown secular spin–orbit resonance that can drive significant obliquity variations. This resonance occurs when the frequency of the planet’s rotation axis precession becomes commensurate with an orbital eigenfrequency of the planetary system. The planet’s eccentricity enables a participating orbital frequency through an interaction in which the apsidal precession of the planet’s orbit causes a cyclic nutation of the planet’s orbital angular momentum vector. The resulting orbital frequency follows the relationship f =-W2v , where v and W are the rates of the planet’s changing longitude of periapsis and longitude of ascending node, respectively. -
[Astro-Ph.EP] 3 Jul 2020 Positions of Ascending Nodes of the Orbits
MNRAS 000,1{24 (2020) Preprint 7 July 2020 Compiled using MNRAS LATEX style file v3.0 Evidence for a high mutual inclination between the cold Jupiter and transiting super Earth orbiting π Men Jerry W. Xuan,? and Mark C. Wyatt Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK Accepted 2020 July 2. Received 2020 June 4; in original form 2020 April 1. ABSTRACT π Men hosts a transiting super Earth (P ≈ 6:27 d, m ≈ 4:82 M⊕, R ≈ 2:04 R⊕) discovered by TESS and a cold Jupiter (P ≈ 2093 d, m sin I ≈ 10:02 MJup, e ≈ 0:64) discovered from radial velocity. We use Gaia DR2 and Hipparcos astrometry to derive the star's velocity caused by the orbiting planets and constrain the cold Jupiter's sky- ◦ projected inclination (Ib = 41 − 65 ). From this we derive the mutual inclination (∆I) between the two planets, and find that 49◦ < ∆I < 131◦ (1σ), and 28◦ < ∆I < 152◦ (2σ). We examine the dynamics of the system using N-body simulations, and find that potentially large oscillations in the super Earth's eccentricity and inclination are suppressed by General Relativistic precession. However, nodal precession of the inner orbit around the invariable plane causes the super Earth to only transit between 7-22 per cent of the time, and to usually be observed as misaligned with the stellar spin axis. We repeat our analysis for HAT-P-11, finding a large ∆I between its close-in Neptune and cold Jupiter and similar dynamics. π Men and HAT-P-11 are prime examples of systems where dynamically hot outer planets excite their inner planets, with the effects of increasing planet eccentricities, planet-star misalignments, and potentially reducing the transit multiplicity.