Space surveillance architecture: issues and challenges – an integrated approach

2021 ◽  
pp. 154851292110316
Author(s):  
Dionysios Tompros
Keyword(s):  
Kuiper Belt ◽  
Integrated Approach ◽  
Asteroid Belt ◽  
Surveillance Systems ◽  
Deep Space ◽  
Common System ◽  
Natural Resource Extraction ◽  
Near Space ◽  
Commercial Applications ◽  
Security Organizations

The object of this study is space surveillance activity and the information systems involved for actors and national security organizations. Near and Deep Space Surveillance areas are presented, the former dealing with artificial objects and the latter the inner planetary system, including asteroids and its exploration and exploitation. (Near Space includes the upper layers of the atmosphere (thermosphere, exosphere) and the magnetosphere up to the limits of the magnetopause (6–15 RE). Deep Space refers to the space after the magnetopause and practically up to the limits of the Kuiper belt, about 50 A.U.) Due to the different matter of each area, the two sectors cannot have a common system for surveillance. The ever-increasing interest in natural resource extraction from the asteroid belt, the Moon, and Near-Earth Objects, combined with the explosive growth of the number of satellite commercial applications, makes the development and interconnection of the two distinct sector systems a necessity. This study describes the surveillance systems, the available technologies and methods, and develops a comprehensive oversight proposal.

scholarly journals Ceres’ partial differentiation: undifferentiated crust mixing with a water-rich mantle

2020 ◽  
Vol 633 ◽  
pp. A117 ◽  
Author(s):  
Wladimir Neumann ◽  
Ralf Jaumann ◽  
Julie Castillo-Rogez ◽  
Carol A. Raymond ◽  
Christopher T. Russell
Keyword(s):  
Thermal Evolution ◽  
Kuiper Belt ◽  
Radioactive Decay ◽  
Thermal Conditions ◽  
Asteroid Belt ◽  
Final Size ◽  
Water Ice ◽  
Modeled Structure ◽  
Internal States ◽  
And Migration

Aims. We model thermal evolution and water-rock differentiation of small ice-rock objects that accreted at different heliocentric distances, while also considering migration into the asteroid belt for Ceres. We investigate how water-rock separation and various cooling processes influence Ceres’ structure and its thermal conditions at present. We also draw conclusions about the presence of liquids and the possibility of cryovolcanism. Methods. We calculated energy balance in bodies heated by radioactive decay and compaction-driven water-rock separation in a three-component dust-water/ice-empty pores mixture, while also taking into consideration second-order processes, such as accretional heating, hydrothermal circulation, and ocean or ice convection. Calculations were performed for varying accretion duration, final size, surface temperature, and dust/ice ratio to survey the range of possible internal states for precursors of Ceres. Subsequently, the evolution of Ceres was considered in five sets of simulated models, covering different accretion and evolution orbits and dust/ice ratios. Results. We find that Ceres’ precursors in the inner solar system could have been both wet and dry, while in the Kuiper belt, they retain the bulk of their water content. For plausible accretion scenarios, a thick primordial crust may be retained over several Gyr, following a slow differentiation within a few hundreds of Myr, assuming an absence of destabilizing impacts. The resulting thermal conditions at present allow for various salt solutions at depths of ≲10 km. The warmest present subsurface is obtained for an accretion in the Kuiper belt and migration to the present orbit. Conclusions. Our results indicate that Ceres’ material could have been aqueously altered on small precursors. The modeled structure of Ceres suggests that a liquid layer could still be present between the crust and the core, which is consistent with Dawn observations and, thus, suggests accretion in the Kuiper belt. While the crust stability calculations indicate crust retention, the convection analysis and interior evolution imply that the crust could still be evolving.

scholarly journals The Locations of Secular Resonances and the Evolution of Small Solar System Bodies

1992 ◽  
Vol 152 ◽  
pp. 123-132
Author(s):  
Ch Froeschle ◽  
P. Farinella ◽  
C. Froeschle ◽  
Z. Knežević ◽  
A. Milani
Keyword(s):  
Perturbation Theory ◽  
Solar System ◽  
Small Body ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Asteroid Belt ◽  
Secular Resonances ◽  
Outer Planets ◽  
Proper Elements ◽  
Solar System Bodies

Generalizing the secular perturbation theory of Milani and Knežević (1990), we have determined in the a — e — I proper elements space the locations of the secular resonances between the precession rates of the longitudes of perihelion and node of a small body and the corresponding eigenfrequencies of the secular perturbations of the four outer planets. We discuss some implications of the results for the dynamical evolution of small solar system bodies. In particular, our findings include: (i) the fact that the g = g6 resonance in the inner asteroid belt lies closer than previously assumed to the Flora region, providing a plausible dynamical route to inject asteroid fragments into planet-crossing orbits; (ii) the possible presence of some low-inclination “stable islands” between the orbits of the outer planets; (iii) the fact that none of the secular resonances considered in this work exists for semimajor axes > 50 AU, so that these resonances do not provide a mechanism for transporting inwards possible Kuiper–belt comets.

scholarly journals Linking the Origin of Asteroids to Planetesimal Formation in the Solar Nebula

2015 ◽  
Vol 10 (S318) ◽  
pp. 1-8 ◽  
Author(s):  
Hubert Klahr ◽  
Andreas Schreiber
Keyword(s):  
Numerical Simulations ◽  
Turbulent Flows ◽  
Kuiper Belt ◽  
Asteroid Belt ◽  
Kuiper Belt Objects ◽  
Physical Size ◽  
Zonal Flows ◽  
Numerical Resolution ◽  
Streaming Instability ◽  
Current Paradigm

AbstractThe asteroids (more precisely: objects of the main asteroid belt) and Kuiper Belt objects (more precisely: objects of the cold classical Kuiper Belt) are leftovers of the building material for our earth and all other planets in our solar system from more than 4.5 billion years ago. At the time of their formation those were typically 100 km large objects. They were called planetesimals, built up from icy and dusty grains. In our current paradigm of planet formation it was turbulent flows and metastable flow patterns, like zonal flows and vortices, that concentrated mm to cm sized icy dust grains in sufficient numbers that a streaming instability followed by a gravitational collapse of these particle clump was triggered. The entire picture is sometimes referred to as gravoturbulent formation of planetesimals. What was missing until recently, was a physically motivated prediction on the typical sizes at which planetesimals should form via this process. Our numerical simulations in the past had only shown a correlation between numerical resolution and planetesimal size and thus no answer was possible (Johansen et al.2011). But with the lastest series of simulations on JUQUEEN (Stephan & Doctor 2015), covering all the length scales down to the physical size of actual planetesimals, we were able to obtain values for the turbulent particle diffusion as a function of the particle load in the gas. Thus, we have all necessary data at hand to feed a 'back of the envelope' calculation that predicts the size of planetesimals as result of a competition between gravitational concentration and turbulent diffusion. Using the diffusion values obtained in the numerical simulations it predicts planetesimal sizes on the order of 100 km, which suprisingly coincides with the measured data from both asteroids (Bottke et al.2005) as well from Kuiper Belt objects (Nesvorny et al.2011).

Planetesimal formation in the solar nebula

1999 ◽  
Vol 173 ◽  
pp. 17-30
Author(s):  
T.V. Ruzmaikina
Keyword(s):  
Interstellar Dust ◽  
Solar Nebula ◽  
Kuiper Belt ◽  
Asteroid Belt ◽  
Dust Grains ◽  
Small Bodies ◽  
Interstellar Dust Grains ◽  
Formation And Evolution ◽  
Cloud Cores ◽  
Solid Bodies

AbstractTerrestrial planets, cores of giant planets and small bodies of the solar system − comets and asteroids − resulted from the coagulation of interstellar dust grains, and grains which were melted or evaporated and condensed again in the solar nebula.The paper describes the growth and processing of dust grains and their aggregates, starting from molecular cloud cores through the formation and evolution of the solar nebula and the accumulation of these aggregates in larger solid bodies − planetesimals. Discussed are the processes which could be responsible for the interruption of accumulation in the region of the asteroid belt, and processes which shaped the Kuiper belt.

Nursery for Planets

2017 ◽  
Author(s):  
John Chambers ◽  
Jacqueline Mitton
Keyword(s):  
Solar System ◽  
Immanuel Kant ◽  
Kuiper Belt ◽  
Planetary Systems ◽  
Protoplanetary Disks ◽  
Young Stars ◽  
Asteroid Belt ◽  
Two Dimensional

This chapter illustrates how the solar system has a decidedly two-dimensional aspect to it. The orbits of the eight major planets all lie in almost the same plane, deviating by no more than seven degrees. Bodies in the asteroid belt and the Kuiper belt stray a little further afield, but these belts are arranged like flattened donuts, aligned with the same plane as the planets. Immanuel Kant and Pierre-Simon de Laplace noted the planar nature of the solar system and used this as the basis for their nebular theories in which the solar system grew out of a flattened disk of matter. Young stars like those in the constellation Orion are often surrounded by disk-shaped clouds of gas and dust. Astronomers quickly dubbed these “protoplanetary” disks, assuming that they will someday form planetary systems.

scholarly journals Warm dust around ϵ Eridani

2010 ◽  
Vol 6 (S276) ◽  
pp. 455-456
Author(s):  
Martin Reidemeister ◽  
Alexander V. Krivov ◽  
Christopher C. Stark ◽  
Jean-Charles Augereau ◽  
Torsten Löhne ◽  
...  
Keyword(s):  
Numerical Simulation ◽  
Thermal Emission ◽  
Kuiper Belt ◽  
Asteroid Belt ◽  
Outer Ring ◽  
Stellar Winds

Abstractϵ Eridani hosts one known inner planet and an outer Kuiper belt analog. Further, Spitzer/IRS measurements indicate that warm dust is present at distances as close as a few AU from the star. Its origin is puzzling, since an “asteroid belt” that could produce this dust would be unstable because of the inner planet. We tested a hypothesis that the observed warm dust is generated by collisions in the outer belt and is transported inward by P-R drag and strong stellar winds. With numerical simulation we investigated how the dust streams from the outer ring into the inner system, and calculated the thermal emission of the dust. We show that the observed warm dust can indeed stem from the outer belt. Our models reproduce the shape and magnitude of the observed SED from mid-IR to sub-mm wavelengths, as well as the Spitzer/MIPS radial brightness profiles.

scholarly journals GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec

2020 ◽  
Vol 641 ◽  
pp. A23 ◽  
Author(s):  
Francisco J. Pozuelos ◽  
Juan C. Suárez ◽  
Gonzalo C. de Elía ◽  
Zaira M. Berdiñas ◽  
Andrea Bonfanti ◽  
...  
Keyword(s):  
Planetary System ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Asteroid Belt ◽  
Physical Parameters ◽  
Planetary Formation ◽  
Low Mass Stars ◽  
The Individual ◽  
The Masses ◽  
M Dwarf

Context. Planets orbiting low-mass stars such as M dwarfs are now considered a cornerstone in the search for planets with the potential to harbour life. GJ 273 is a planetary system orbiting an M dwarf only 3.75 pc away, which is composed of two confirmed planets, GJ 273b and GJ 273c, and two promising candidates, GJ 273d and GJ 273e. Planet GJ 273b resides in the habitable zone. Currently, due to a lack of observed planetary transits, only the minimum masses of the planets are known: Mb sin ib = 2.89 M⊕, Mc sin ic = 1.18 M⊕, Md sin id = 10.80 M⊕, and Me sin ie = 9.30 M⊕. Despite its interesting character, the GJ 273 planetary system has been poorly studied thus far. Aims. We aim to precisely determine the physical parameters of the individual planets, in particular, to break the mass–inclination degeneracy to accurately determine the mass of the planets. Moreover, we present a thorough characterisation of planet GJ 273b in terms of its potential habitability. Methods. First, we explored the planetary formation and hydration phases of GJ 273 during the first 100 Myr. Secondly, we analysed the stability of the system by considering both the two- and four-planet configurations. We then performed a comparative analysis between GJ 273 and the Solar System and we searched for regions in GJ 273 which may harbour minor bodies in stable orbits, that is, the main asteroid belt and Kuiper belt analogues. Results. From our set of dynamical studies, we find that the four-planet configuration of the system allows us to break the mass–inclination degeneracy. From our modelling results, the masses of the planets are unveiled as: 2.89 ≤ Mb ≤ 3.03 M⊕, 1.18 ≤ Mc ≤ 1.24 M⊕, 10.80 ≤ Md ≤ 11.35 M⊕, and 9.30 ≤ Me ≤ 9.70 M⊕. These results point to a system that is likely to be composed of an Earth-mass planet, a super-Earth and two mini-Neptunes. Based on planetary formation models, we determine that GJ 273b is likely an efficient water captor while GJ 273c is probably a dry planet. We find that the system may have several stable regions where minor bodies might reside. Collectively, these results are used to offer a comprehensive discussion about the habitability of GJ 273b.

Integrative and Comprehensive Understanding on Polar Environments (iCUPE) – concept, results and outlook

2021 ◽  
Author(s):  
Tuukka Petäjä ◽  
Keyword(s):  
Integrated Approach ◽  
The Arctic ◽  
Observation Data ◽  
Polar Regions ◽  
Comprehensive Understanding ◽  
Natural Resource Extraction ◽  
Pollutant Concentrations ◽  
Earth Observation Data ◽  
Art Research ◽  
Set Up

<p>The world is changing. The polar regions are critical component in the Earth system and influenced by on-going megatrends, such as globalization and demographical changes. The extensive use of Arctic natural resources will have effects on regional pollutant concentrations in the Arctic. We set up the ERA-PLANET Strand 4 project “iCUPE – integrative and Comprehensive Understanding on Polar Environments” to provide novel insights and observational data on global grand challenges with a polar focus. We deploy an integrated approach with in-situ observations, satellite remote sensing and multi-scale modeling to synthesize data from a suite of comprehensive long-term measurements, intensive campaigns, and satellites. This enabled us to deliver novel data and indicators descriptive of the polar environment. The iCUPE framework includes thematic state-of-the-art research and the provision of novel data in atmospheric pollution, local sources and transboundary transport, characterization of arctic surfaces and their changes, an assessment of the concentrations and impacts of heavy metals and persistent organic pollutants and their cycling, the quantification of emissions from natural resource extraction, and the validation and optimization of satellite Earth observation data streams. Here we summarize the project results and provide novel insights into continuation of the work. </p>

From Subsurface to Riser: An Integrated Approach to Subsea Surveillance

2010 ◽  
Author(s):  
Jon Machin
Keyword(s):  
Surveillance System ◽  
Production Control ◽  
High Reliability ◽  
Cost Effective ◽  
Integrated Approach ◽  
Production Optimization ◽  
Surveillance Systems ◽  
Physical Layers ◽  
Key Enabling Technologies ◽  
Reliability Performance

The high reliability performance of a subsea surveillance system, from subsurface to riser, is of the utmost importance for maximizing production availability. In designing such a surveillance system, there are a multitude of considerations that need to be addressed. These have traditionally focused on safe and cost effective production control system availability. However, they are now being extended to also address enablers for secondary recovery, production optimization, and increased recovery activities. This paper addresses the idea that latest-generation surveillance systems must operate seamlessly from the subsurface to the seabed and in turn from seabed to riser. In doing so they must integrate a number of key enabling technologies over different physical layers and predefined technical interfaces. They must also serve to integrate these technologies over the project management interfaces which arise from the selection of the different proprietary technologies, and the commercial and contractual barriers which can result.

Sign in / Sign up

Export Citation Format

Share Document