LISA Pathfinder

McNamara, P. W.; Vitale, S.; Danzmann, K.

doi:10.1088/0264-9381/25/11/114034

Cited by 111 publications

(108 citation statements)

References 2 publications

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“…In each satellite the lattice confining the clock atoms is created using the standing wave formed by retroreflecting a magic wavelength laser [11][12][13] off of a mirror mounted on a free-floating reference mass, such that the atoms are strongly confined in the reference frame of the free mass and are therefore in free fall, despite their confinement. Drag-free masses have been studied in great detail by the LISA collaboration, and this technology is currently undergoing testing and verification in the LISA Pathfinder space mission [42,43]. The phase of the clock lasers in each satellite is kept referenced to the same mirror using interferometry [44] to cancel out any relative motion of the lasers or optics with respect to the atoms.…”

Section: Sensing Gravitational Waves Using Optical Lattice Atomicmentioning

confidence: 99%

Gravitational wave detection with optical lattice atomic clocks

et al. 2016

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We propose a space-based gravitational wave (GW) detector consisting of two spatially separated, dragfree satellites sharing ultrastable optical laser light over a single baseline. Each satellite contains an optical lattice atomic clock, which serves as a sensitive, narrowband detector of the local frequency of the shared laser light. A synchronized two-clock comparison between the satellites will be sensitive to the effective Doppler shifts induced by incident GWs at a level competitive with other proposed space-based GW detectors, while providing complementary features. The detected signal is a differential frequency shift of the shared laser light due to the relative velocity of the satellites, and the detection window can be tuned through the control sequence applied to the atoms' internal states. This scheme enables the detection of GWs from continuous, spectrally narrow sources, such as compact binary inspirals, with frequencies ranging from ∼3 mHz-10 Hz without loss of sensitivity, thereby bridging the detection gap between spacebased and terrestrial optical interferometric GW detectors. Our proposed GW detector employs just two satellites, is compatible with integration with an optical interferometric detector, and requires only realistic improvements to existing ground-based clock and laser technologies.

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Section: Sensing Gravitational Waves Using Optical Lattice Atomicmentioning

confidence: 99%

Gravitational wave detection with optical lattice atomic clocks

et al. 2016

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“…One example is the LISA Pathfinder mission which features both FEEP and colloidal thrusters and plans to be launch in 2013. [34] The colloidal thruster was developed by Busek Company in the U.S.. One of advantages of electrospray thrusters is that they do not need conditioning time which is usually required for other electric propulsion and FEEP thrusters. Liquid metal used for FEEP propellant needs to be heated up to liquefy.…”

Section: Precise Attitude Control Of Spacecraftmentioning

confidence: 99%

Electrospray Propulsion

Lozano¹,

Martı́nez-Sánchez²,

Hruby³

2010

Encyclopedia of Aerospace Engineering

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Micro-propulsion has been studied for many years due to its applications in small-tomedium sized spacecraft for precise satellite attitude control. Electrospray thrusters are promising thrusters built upon the state of the art in micro-technology and with flexible performance in terms of their high efficiency and high specific impulse. One challenge is to investigate in detail the mechanism for ion emission to complement experimental results and understand better how emission occurs in the micro to nano scale. Thus, atomistic modeling is used to understand properties of emitted charged particles which determine how the thrusters perform.As a preliminary study of ion emission from Taylor cones, ion evaporation from 3 -5 nm droplets was observed in molecular dynamics (MD) simulations to validate the atomistic modeling and to investigate activation energies. Ion emission was examined in terms of internal and external electric fields and the activation energies of each case were obtained using Schottky's model and direct energy calculation to compare with experimental values. Ion emission was mainly observed with electric field strengths between 1.2 -2.0 V/nm and the emitted species include both solvated and non-solvated ions. Propulsive properties from Taylor cones are examined using results from the analysis of electric current from ion emission.In addition to an observation of ion emission from liquid droplets, numerical simulations for interactions between a solid plate and liquid droplets were conducted with MD simulation. It was concluded that another selection of force field needs to be considered to pursue further details, such as electrochemical effects.

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“…Thus ESA decided in 2002 to provide a technology demonstration mission called LISA Pathfinder [McNamara (2006);McNamara et al (2008); Racca & McNamara (2009)] to validate the performance in space of the Gravitational Reference Sensors that were being developed to be flown on LISA [Armano et al (2009)]. Initial design studies for the LISA GRSs were done at ONERA in Paris, but most of the later development of the GRSs for LISA Pathfinder and for LISA has been carried out at the University of Trento (see e.g., [Carbone et al (2007)]).…”

Section: Lisa Pathfinder Missionmentioning

confidence: 99%

Gravitational wave astronomy, relativity tests, and massive black holes

Bender

2009

Proc. IAU

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Abstract. The gravitational wave detectors that are operating now are looking for several kinds of gravitational wave signals at frequencies of tens of Hertz to kilohertz. One of these is mergers of roughly 10 M BH binaries. Sometime between now and about 8 years from now, it is likely that signals of this kind will be observed. The result will be strong tests of the dynamical predictions of general relativity in the high field regime. However, observations at frequencies below 1 Hz will have to wait until the launch of the Laser Interferometer Space Antenna (LISA), hopefully only a few years later. LISA will have 3 main objectives, all involving massive BHs. The first is observations of mergers of pairs of intermediate mass (100 to 10 5 M ) and higher mass BHs at redshifts out to roughly z=10. This will provide new information on the initial formation and growth of BHs such as those found in most galaxies, and the relation between BH growth and the evolution of galactic structure. The second objective is observations of roughly 10 M BHs, neutron stars, and white dwarfs spiraling into much more massive BHs in galactic nuclei. Such events will provide detailed information on the populations of such compact objects in the regions around galactic centers. And the third objective is the use of the first two types of observations for testing general relativity even more strongly than ground based detectors will. As an example, an extreme mass ratio event such as a 10 M BH spiraling into a galactic center BH can give roughly 10 5 observable cycles during about the last year before merger, with a mean relative velocity of 1/3 to 1/2 the speed of light, and the frequencies of periapsis precession and Lense-Thirring precession will be high. The LISA Pathfinder mission to prepare for LISA is scheduled for launch in 2011.

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LISA Pathfinder

Cited by 111 publications

References 2 publications

Gravitational wave detection with optical lattice atomic clocks

Gravitational wave detection with optical lattice atomic clocks

Electrospray Propulsion

Gravitational wave astronomy, relativity tests, and massive black holes

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