Deep Space Propulsion

Long, K. F.

doi:10.1007/978-1-4614-0607-5

Cited by 23 publications

(5 citation statements)

References 5 publications

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“…Landis (1999) and Frisbee (2009) found ways to reduce it dramatically to 1-10 km. Systems were further optimized, with higher peak power of ∼ 10 TW and smaller vehicle size of ∼ 0.1 − 1 km for the sail, requiring ∼ 100 km antenna array aperture (Dickinson 2001;Long 2011). Later concepts developed cost-optimized systems (Benford 2013).…”

Section: Interstellar Probesmentioning

confidence: 99%

Power Beaming Leakage Radiation as a Seti Observable

Benford

2016

ApJ

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The most observable leakage radiation from an advanced civilization may well be from the use of power beaming to transfer energy and accelerate spacecraft. Applications suggested for power beaming involve launching spacecraft to orbit, raising satellites to a higher orbit, and interplanetary concepts involving space-to-space transfers of cargo or passengers. We also quantify beam-driven launch to the outer solar system, interstellar precursors, and ultimately starships. We estimate the principal observable parameters of power beaming leakage. Extraterrestrial civilizations would know their power beams could be observed, and so could put a message on the power beam and broadcast it for our receipt at little additional energy or cost. By observing leakage from power beams we may find a message embedded on the beam. Recent observations of the anomalous star KIC 8462852 by the Allen Telescope Array (ATA) set some limits on extraterrestrial power beaming in that system. We show that most power beaming applications commensurate with those suggested for our solar system would be detectable if using the frequency range monitored by the ATA, and so the lack of detection is a meaningful, if modest, constraint on extraterrestrial power beaming in that system. Until more extensive observations are made, the limited observation time and frequency coverage are not sufficiently broad in frequency and duration to produce firm conclusions. Such beams would be visible over large interstellar distances. This implies a new approach to the SETI search: instead of focusing on narrowband beacon transmissions generated by another civilization, look for more powerful beams with much wider bandwidth. This requires a new approach for their discovery by telescopes on Earth. Further studies of power beaming applications should be performed, potentially broadening the parameter space of the observable features that we have discussed here.

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Section: Interstellar Probesmentioning

confidence: 99%

Power Beaming Leakage Radiation as a Seti Observable

Benford

2016

ApJ

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“…For manned spacecraft utilising Nuclear Thermal Propulsion (NTP) or Nuclear Electric Propulsion (NEP) as primary propulsion this would already be achieved by the release of propellant from the thrusters; typical propellants for these systems being hydrogen and other volatile propellants, and for NEP systems, also inert gases such as Argon and Xenon [44,45,46]. If more localised injection of plasma is required toward the shield region, ion or plasma sources, as already used for spacecraft propulsion [46], could be used to provide more directed ion or plasma beams from multiple locations on the spacecraft.…”

Section: Boosting the Shield Effectiveness: Mass Loadingmentioning

confidence: 99%

An exploration of the effectiveness of artificial mini-magnetospheres as a potential solar storm shelter for long term human space missions

Bamford¹,

Kellett²,

Bradford³

et al. 2014

Acta Astronautica

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If mankind is to explore the solar system beyond the confines of our Earth and Moon the problem of radiation protection must be addressed. Galactic cosmic rays and highly variable energetic solar particles are an ever-present hazard in interplanetary space. Electric and/or magnetic fields have been suggested as deflection shields in the past, but these treated space as an empty vacuum. In fact it is not empty. Space contains a plasma known as the solar wind; a constant flow of protons and electrons coming from the Sun. In this paper we explore the effectiveness of a "mini-magnetosphere" acting as a radiation protection shield. We explicitly include the plasma physics necessary to account for the solar wind and its induced effects. We show that, by capturing/containing this plasma, we enhance the effectiveness of the shield. Further evidence to support our conclusions can be obtained from studying naturally occurring "mini-magnetospheres" on the Moon. These magnetic anomalies (related to "lunar swirls") exhibit many of the effects seen in laboratory experiments and computer simulations. If shown to be feasible, this technology could become the gateway to manned exploration of interplanetary space

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“…Accurate computation of electromagnetic scattering by the natural and human-made objects will be necessary for remote detection and tracking. Accurate computation of electromagnetic scattering would also be needed to design propulsion systems for laserdriven spacecraft [1]. Experience with our current spacecraft [3] strongly indicates that relativistic effects in electromagnetic scattering by objects moving at an appreciable fraction of the speed of light will not be negligible.…”

Section: Introductionmentioning

confidence: 99%

“…Humans will become a spacefaring species when technology allows [1]. Our unmanned probes and manned spacecraft will need to travel at relativistic velocities if they are to reach their destinations within short periods of time.…”

Section: Introductionmentioning

confidence: 99%

Electromagnetic pulse scattering by a spacecraft nearing light speed

et al. 2017

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Humans will launch spacecraft that travel at an appreciable fraction of the speed of light. Spacecraft traffic will be tracked by radar. Scattering of pulsed electromagnetic fields by an object in uniform translational motion at relativistic speed may be computed using the frame-hopping technique. Pulse scattering depends strongly on the velocity, shape, orientation, and composition of the object. The peak magnitude of the backscattered signal varies by many orders of magnitude depending on whether the object is advancing toward or receding away from the source of the interrogating signal. The peak magnitude of the backscattered signal goes to zero as the object recedes from the observer at a velocity very closely approaching light speed, rendering the object invisible to the observer. The energy scattered by an object in motion may increase or decrease relative to the energy scattered by the same object at rest. Both the magnitude and sign of the change depend on the velocity of the object, as well as on its shape, orientation, and composition. In some cases, the change in total scattered energy is greatest when the object is moving transversely to the propagation direction of the interrogating signal, even though the Doppler effect is strongest when the motion is parallel or antiparallel to the propagation direction.

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Deep Space Propulsion

Cited by 23 publications

References 5 publications

Power Beaming Leakage Radiation as a Seti Observable

Power Beaming Leakage Radiation as a Seti Observable

An exploration of the effectiveness of artificial mini-magnetospheres as a potential solar storm shelter for long term human space missions

Electromagnetic pulse scattering by a spacecraft nearing light speed

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