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Academic literature on the topic 'Laser Interferometer Space Antenna'

Author: Grafiati

Published: 4 June 2021

Last updated: 4 February 2022

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Journal articles on the topic "Laser Interferometer Space Antenna"

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Zhan, Ming-Sheng, Jin Wang, Wei-Tou Ni, Dong-Feng Gao, Gang Wang, Ling-Xiang He, Run-Bing Li, et al. "ZAIGA: Zhaoshan long-baseline atom interferometer gravitation antenna." International Journal of Modern Physics D 29, no. 04 (July 2, 2019): 1940005. http://dx.doi.org/10.1142/s0218271819400054.

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The Zhaoshan long-baseline Atom Interferometer Gravitation Antenna (ZAIGA) is a new type of underground laser-linked interferometer facility, and is currently under construction. It is in the 200-m-on-average underground of a mountain named Zhaoshan which is about 80[Formula: see text]km southeast to Wuhan. ZAIGA will be equipped with long-baseline atom interferometers, high-precision atom clocks, and large-scale gyros. ZAIGA facility will take an equilateral triangle configuration with two 1-km-apart atom interferometers in each arm, a 300-m vertical tunnel with atom fountain and atom clocks mounted, and a tracking-and-ranging 1-km-arm-length prototype with lattice optical clocks linked by locked lasers. The ZAIGA facility will be used for experimental research on gravitation and related problems including gravitational wave detection, high-precision test of the equivalence principle of micro-particles, clock-based gravitational red-shift measurement, rotation measurement and gravitomagnetic effect.

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Shaddock, D. A. "An Overview of the Laser Interferometer Space Antenna." Publications of the Astronomical Society of Australia 26, no. 2 (2009): 128–32. http://dx.doi.org/10.1071/as08059.

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AbstractThe Laser Interferometer Space Antenna (LISA) will detect gravitational waves with frequencies from 0.1 mHz to 1 Hz. This article provides a brief overview of LISA's science goals followed by a tutorial of the LISA measurement concept.

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Zhao, Ya, Zhi Wang, Yupeng Li, Chao Fang, Heshan Liu, and Huilong Gao. "Method to Remove Tilt-to-Length Coupling Caused by Interference of Flat-Top Beam and Gaussian Beam." Applied Sciences 9, no. 19 (October 1, 2019): 4112. http://dx.doi.org/10.3390/app9194112.

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We discuss the tilt-to-length (TTL) coupling noise caused by interference between a flat-top beam and a Gaussian beam. Several physical models are presented to research the effects of non-diffracted and diffracted beams on TTL noise. A special case that can remove TTL coupling noise is discovered and is verified via both theoretical analysis and numerical simulations. The proposed case could provide desirable suggestions for the construction of high-precision interferometers such as the Laser Interferometer Space Antenna (LISA), Taiji program, or other interferometry systems.

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Liu, He-Shan, Zi-Ren Luo, and Wei Sha. "In-orbit performance of the laser interferometer of Taiji-1 experimental satellite." International Journal of Modern Physics A 36, no. 11n12 (February 22, 2021): 2140004. http://dx.doi.org/10.1142/s0217751x21400042.

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Taiji-1, which is the first experimental satellite for space gravitational wave detection in China, relies on key technologies which include the laser interferometer, the gravitational reference sensor (GRS), the micro-thruster and the satellite platform. Similarly to the Laser Interferometer Space Antenna (LISA) pathfinder, except for the science interferometer, the optical bench (OB) of Taiji-1 contains reference and test mass (TM) interferometers. Limited by the lower mechanical strength of the carrier rocket and by the orbit environment, the OB of Taiji-1 is made of invar steel and fused silica, and it is aimed to achieve a sensitivity of the order of 100[Formula: see text]pm/[Formula: see text]. The experimental results from in-orbit tests of Taiji-1 demonstrate that the interferometer can reach a sensitivity of 30[Formula: see text]pm/[Formula: see text] in the frequency range of 0.01–10[Formula: see text]Hz, which satisfies the requirements of Taiji-1 mission.

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Maghami, Peiman G., and T. Tupper Hyde. "Laser interferometer space antenna dynamics and controls model." Classical and Quantum Gravity 20, no. 10 (April 29, 2003): S273—S282. http://dx.doi.org/10.1088/0264-9381/20/10/330.

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Christensen, Nelson. "Lasers and Optics for the Laser Interferometer Space Antenna (LISA)." EPJ Web of Conferences 243 (2020): 08001. http://dx.doi.org/10.1051/epjconf/202024308001.

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Wang, Zhi, Tao Yu, Ya Zhao, Ziren Luo, Wei Sha, Chao Fang, Yukun Wang, et al. "Research on Telescope TTL Coupling Noise in Intersatellite Laser Interferometry." Photonic Sensors 10, no. 3 (November 29, 2019): 265–74. http://dx.doi.org/10.1007/s13320-019-0574-5.

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AbstractThe detection mission of gravitational waves in space is that the accuracy of the long-baseline intersatellite laser interferometry on the million-kilometer order needs to reach the order of $$8 \rm{pm}/\sqrt{\rm{Hz}}$$8pm/Hz. Among all noise sources that affect the interferometry accuracy, tilt-to-length (TTL) coupling noise is the second largest source of noise after shot noise. This paper focuses on studying the contribution of TTL coupling noise of the telescope system in the intersatellite scientific interferometer. By referring to the laser interferometer space antenna (LISA)’s noise budget, TTL coupling noise is required to be within ±25μm/rad (±300μrad). Therefore, this paper focuses on studying both the mechanism of TTL coupling noise due to the noise sources of the telescope and the method of suppressing the TTL noise, which can lay a foundation for noise distribution and the development of engineering prototypes in subsequent tasks.

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Escudero Sanz, Isabel, Astrid Heske, and Jeffrey C. Livas. "A telescope for LISA – the Laser Interferometer Space Antenna." Advanced Optical Technologies 7, no. 6 (December 19, 2018): 395–400. http://dx.doi.org/10.1515/aot-2018-0044.

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Abstract Gravitational waves are a prediction of Einstein’s general relativity theory. In autumn 2017, the Laser Interferometer Gravitational-Wave Observatory (LIGO; https://www.ligo.caltech.edu/) experiment reported the first detection of gravitational waves in addition to electromagnetic radiation from the collision of two neutron stars. This marks the first time that a cosmic event has been viewed in both gravitational waves and light and opens the door to a new type of astronomical observatory based on gravitational waves. The gravitational wave spectrum covers a broad span of frequencies and requires both space- and ground-based observatories to cover the full range. Space-based gravitational wave observatories, such as the proposed Laser Interferometer Space Antenna (LISA), operate at frequencies between 0.1 mHz and 1 Hz and complement the frequency range of 30–1000 Hz accessible by ground-based gravitational wave observatories, such as LIGO. A rich array of high-energy astrophysical sources is expected in the LISA measurement band. LISA was selected in 2017 as the third large mission of the Cosmic Vision program of the European Space Agency. The National Aeronautics and Space Administration will collaborate on both the scientific and technical aspects of this mission. This paper addresses the design of the optical telescope as an essential component of LISA’s long-distance interferometric measurement system.

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Xia, Yan, GuangYu Li, Gerhard Heinzel, Albrecht Rüdiger, and YongJie Luo. "Orbit design for the Laser Interferometer Space Antenna (LISA)." Science China Physics, Mechanics and Astronomy 53, no. 1 (January 2010): 179–86. http://dx.doi.org/10.1007/s11433-010-0100-7.

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Maghami, P. G., T. T. Hyde, and J. Kim. "An acquisition control for the laser interferometer space antenna." Classical and Quantum Gravity 22, no. 10 (April 28, 2005): S421—S428. http://dx.doi.org/10.1088/0264-9381/22/10/038.

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Dissertations / Theses on the topic "Laser Interferometer Space Antenna"

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Otto, Markus [Verfasser]. "Time-delay interferometry simulations for the laser interferometer space antenna / Markus Otto." Hannover : Technische Informationsbibliothek (TIB), 2016. http://d-nb.info/1118740769/34.

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Pollack, Scott E. "Analytic and interferometric techniques for the Laser Interferometer Space Antenna." Diss., Connect to online resource, 2005. http://wwwlib.umi.com/dissertations/fullcit/3178330.

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Goh, Allex. "Electrostatics problems relating to the laser interferometer space antenna mission /." May be available electronically:, 2007. http://proquest.umi.com/login?COPT=REJTPTU1MTUmSU5UPTAmVkVSPTI=&clientId=12498.

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Higuchi, Sei. "Microkelvin thermal control system for the laser interferometer space antenna mission and beyond /." May be available electronically:, 2009. http://proquest.umi.com/login?COPT=REJTPTU1MTUmSU5UPTAmVkVSPTI=&clientId=12498.

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Torres, Matos Edgar Omar. "Science frequency analysis of temperature sensors for the Laser Interferometer Space Antenna (LISA) /." May be available electronically:, 2008. http://proquest.umi.com/login?COPT=REJTPTU1MTUmSU5UPTAmVkVSPTI=&clientId=12498.

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Roberts, Peter. "Drag-free control and technological risk assessment for the LISA gravitational wave space antenna." Thesis, Cranfield University, 2000. http://dspace.lib.cranfield.ac.uk/handle/1826/11109.

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The quest for the direct detection and observation of gravitational waves remains one of the lasting scientific challenges of the 20th century, and one that will continue on into the 21 st. Concepts and technologies are being developed that will, early in the new millennium, allow their direct observation for the first time. This will be the beginning of the gravitational wave astronomy revolution. The LISA (Laser Interferometer Space Antenna) mISSIOn is one of the cornerstones of this revolution. Observing in the low-frequency band, it will provide information about our universe that cannot be gathered from the ground. This band contains sources fundamental to our understanding of how the universe began and operates. In turn, fundamental to the LISA mission is the concept of drag-free control. This provides the relatively undisturbed environment for the test-masses which form the references for the measurement of the gravitational waves. Without it the effect of gravitational waves would be but a whisper amongst a cacophony of disturbances. It is drag-free control for the LISA mission which forms the basis for the majority of this thesis. The research and development work carried out by the author has involved the development of a control model of the LISA dragfree control system to assess its feasibility. The author proposes a different approach to the problems involved from that suggested by other authors. It is shown that this approach, unlike those suggested in the mission baseline studies, fulfills the control requirements for the LISA mission. Technological risk assessment in general, as well as that associated with the LISA mission, is also considered.

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Schuldt, Thilo. "An optical readout for the LISA gravitational reference sensor." Doctoral thesis, Humboldt-Universität zu Berlin, Mathematisch-Naturwissenschaftliche Fakultät I, 2010. http://dx.doi.org/10.18452/16241.

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Der weltraumgestützte Gravitationswellendetektor LISA (Laser Interferometer Space Antenna) besteht aus drei identischen Satelliten an Bord derer sich jeweils zwei frei schwebende Testmassen befinden. Die Lage der einzelnen Testmassen in Bezug auf die zugehörige optische Bank muss mit einer Genauigkeit besser 1 pm/sqrt(Hz) in der Abstands- und besser 10 nrad/sqrt(Hz) in der Winkelmessung erfolgen. In der vorliegenden Arbeit wird ein kompaktes optisches Auslesesystem präsentiert, welches als Prototyp für diese Abstands- und Winkelmetrologie dient. Das dafür entwickelte polarisierende Heterodyn-Interferometer mit räumlich getrennten Frequenzen basiert auf einem hoch-symmetrischen Design, bei dem zur optimalen Gleichtakt-Unterdrückung Mess- und Referenzarm die gleiche Polarisation und Frequenz sowie annähernd gleiche optische Pfade haben. Für die Winkelmessung wird die Methode der differentiellen Wellenfrontmessung eingesetzt. In einem ersten Prototyp-Aufbau wird ein Rauschniveau von weniger als 100 pm/sqrt(Hz) in der Translations- und von weniger als 100 nrad/sqrt(Hz) in der Winkelmessung (beides für Frequenzen oberhalb 0.1 Hz) demonstriert. In einem zweiten Prototyp-Aufbau werden zusätzlich eine Intensitätsstabilisierung und ein Phasenlock der beiden Frequenzen implementiert. Die analoge Phasenmessung ist durch eine digitale, FPGA basierte, ersetzt. Mit diesem Aufbau wird ein Rauschen kleiner 5 pm/sqrt(Hz) in der Translationsmessung und kleiner 10 nrad/sqrt(Hz) in der Winkelmessung, beides für Frequenzen größer 0.01 Hz, erreicht. Eine Rausch-Analyse wurde durchgeführt und die Nichtlinearitäten des Interferometers bestimmt. Das Interferometer wurde im Hinblick auf die LISA Mission entwickelt, findet seine Anwendung aber auch bei der Charakterisierung der dimensionalen Stabilität von ultra-stabilen Materialien sowie in der optischen Profilometrie. Die Adaptierung des Interferometers dazu sowie erste Resultate zu beiden Anwendungen werden in dieser Arbeit präsentiert.
The space-based gravitational wave detector LISA (Laser Interferometer Space Antenna) consists of three identical satellites. Each satellite accommodates two free-flying proof masses whose distance and tilt with respect to its corresponding optical bench must be measured with at least 1 pm/sqrt(Hz) sensitivity in translation and at least 10 nrad/sqrt(Hz) sensitivity in tilt measurement. In this thesis, a compact optical readout system is presented, which serves as a prototype for the LISA proof mass attitude metrology. We developed a polarizing heterodyne interferometer with spatially separated frequencies. For optimum common mode rejection, it is based on a highly symmetric design, where measurement and reference beam have the same frequency and polarization, and similar optical pathlengths. The method of differential wavefront sensing (DWS) is utilized for the tilt measurement. In a first prototype setup noise levels below 100 pm/sqrt(Hz) in translation and below 100 nrad/sqrt(Hz) in tilt measurement (both for frequencies above 0.1 Hz) are achieved. A second prototype was developed with additional intensity stabilization and phaselock of the two heterodyne frequencies. The analog phase measurement is replaced by a digital one, based on a Field Programmable Gate Array (FPGA). With this setup, noise levels below 5 pm/sqrt(Hz) in translation measurement and below 10 nrad/sqrt(Hz) in tilt measurement, both for frequencies above 0.01Hz, are demonstrated. A noise analysis was carried out and the nonlinearities of the interferometer were measured. The interferometer was developed for the LISA mission, but it also finds its application in characterizing the dimensional stability of ultra-stable materials such as carbon-fiber reinforced plastic (CFRP) and in optical profilometry. The adaptation of the interferometer and first results in both applications are presented in this work.

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Petiteau, Antoine. "DE LA SIMULATION DE LISA A L'ANALYSE DES DONNEES. Détection d'ondes gravitationnelles par interférométrie spatiale (LISA : Laser Interferometer Space Antenna)." Phd thesis, Université Paris-Diderot - Paris VII, 2008. http://tel.archives-ouvertes.fr/tel-00383222.

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Les ondes gravitationnelles sont émises par une large gamme de sources astrophysiques et cosmologiques. L'étude des ondes à basse fréquence telles que celles émises par les binaires de trous noirs, les EMRIs ou encore les fonds galactique et stochastique, nécessite l'utilisation d'un détecteur spatial. C'est la mission LISA (Laser Interferometer Space Antenna) composée de trois satellites distants de 5 millions de kilomètres et qui s'échangent des faisceaux lasers afin de former plusieurs interféromètres. La bonne compréhension de ce projet complexe nécessite le développement d'un simulateur tel que celui réalisé pendant cette thèse, LISACode. C'est un simulateur scientifique de LISA qui s'attache à rester au plus proche de la réalité du détecteur, sans pour autant le décrire au niveau des détails d'ingénierie. Il fournit des flux de données similaires à ceux de la future mission et applique la méthode TDI qui réduit effectivement le bruit laser. Ainsi il permet de tester des points technologiques importants de LISA et de mener des études scientifiques sur les ondes gravitationnelles. C'est un outil essentiel pour la préparation de l'analyse de données qui est un point capital de la mission LISA. Ainsi le second point de cette thèse porte sur le développement d'une méthode d'analyse basée sur l'étude de la modulation d'amplitude du signal gravitationnel induite par le mouvement LISA. Cette étude donne accès à la position de la source. L'application de cette méthode a nécessité la mise en place de méthodes d'extraction du signal. Les résultats obtenus pour une onde monochromatique et pour une onde émise par une binaire de trous noirs super-massifs sont prometteurs.

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Petiteau, Antoine. "De la simulation de LISA à l'analyse des données : détection d'ondes gravitationnelles par interférométrie spatiale (LISA: Laser Interferometer Space Antenna)." Paris 7, 2008. http://www.theses.fr/2008PA077223.

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Les ondes gravitationnelles sont émises par une large gamme de sources astrophysiques et cosmologiques. L'étude des ondes à basse fréquence telles que celles émises par les binaires de trous noirs, les EMRIs ou encore les fonds galactique et stochastique, nécessite l'utilisation d'un détecteur spatial. C'est la mission LISA (Laser Interferometer Space Antenna) composée de trois satellites distants de 5 millions de kilomètres et qui s'échangent des faisceaux lasers afin de former plusieurs interféromètres. La bonne compréhension de ce projet complexe nécessite le développement d'un simulateur tel que celui réalisé pendant cette thèse, LISACode. C'est un simulateur scientifique de LISA qui s'attache à rester au plus proche de la réalité du détecteur, sans pour autant le décrire au niveau des détails d'ingénierie. Il fournit des flux de données similaires à ceux de la future mission et applique la méthode TDI qui réduit effectivement le bruit laser. Ainsi il permet de tester des points technologiques importants de LISA et de mener des études scientifiques sur les ondes gravitationnelles. C'est un outil essentiel pour la préparation de l'analyse de données qui est un point capital de la mission LISA. Ainsi le second point de cette thèse porte sur le développement d'une méthode d'analyse basée sur l'étude de la modulation d'amplitude du signal gravitationnel induite par le mouvement LISA. Cette étude donne accès à la position de la source. L'application de cette méthode a nécessité la mise en place de méthodes d'extraction du signal. Les résultats obtenus pour une onde monochromatique et pour une onde émise par une binaire de trous noirs super-massifs sont prometteurs
Gravitational waves are emitted from a variety of astrophysical and cosmological sources. Study of low frequency waves, emitted for example by coalescing massive black holes, by EMRIs or by the galactic or stochastic background, requires a space based detector. The LISA (Laser Interferometer Space Antenna) project is based on 3 satellites, separated by 5 million kilometers, which exchange laser beams, forming several interferometers. An understanding of this complex project requires the development of simulation softwares such as LISACode (this thesis). It is a new scientific Simulator for LISA. Its ambition is to achieve a degree of sophistication. Allowing to map, as closely as possible, the impact of the different sub-systems on the measurements. This is achieved by introducing, in a realistic manner, most of the ingredients that will influence LISA's sensitivity as well as the application of TDI combinations. This code allows to study different configurations of LISA thus testing different technological key points and performing scientific studies on gravitational waves. It is also an efficient tool for generating time series for data analysis developments. Therefore the second point is the development of a method of analysis based on the study of amplitude modulation of gravitational signal which is due to the LISA motion. This method gives access to the source position. In order to apply this method, specific methods for extracting signal have been developed. This analysis method was tested on monochromatic waves and on waves emitted by binary Systems. Present result s are promising and the method should be expanded further

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Sanjuán, Muñoz Josep. "Development and validation of the thermal diagnostics instrumentation in lisa pathfinder." Doctoral thesis, Universitat Politècnica de Catalunya, 2009. http://hdl.handle.net/10803/6366.

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This thesis focuses on the issues related to the thermal diagnostics aboard the space mission LISA Pathfinder (LPF). LPF is a technological mission devoted to put to test critical subsystems for the LISA mission. LISA will be the first space born gravitational wave (GW) observatory with the main objective of detecting GWs. GWs are ripples of the space-time geometry caused by acceleration of masses in an asymmetric way. Their detection requires put test masses (TMs) in an almost perfect inertial frame (or free fall).

Non-inertial forces perturbing the TMs must be less than 6 fN/sqrt(Hz) in the frequency range of 0.1 mHz to 0.1 Hz and the noise in the measurement between the TMs (separated by 5 Gm) must be of 40 pm/sqrt(Hz) in the same band. To reduce the risks of a direct launch of LISA, ESA has decided to first launch LPF to put all the LISA technologies to test.
The payload of LPF, the LISA Technology Package (LTP), contains two TMs placed in two cylinders inside a single spacecraft (SC) and an interferometric system that measures the relative distance between them. The SC isolates the TMs from the external disturbances but internal stray forces will still perturb the TMs. Their levels must be bounded not to challenge the free fall accuracy. One of these disturbances is temperature fluctuations and the aspects related to their measurement are the leitmotif of this thesis.

In chapter 1 we have presented how temperature fluctuations couple into the key subsystems of the LTP to degrade their performance. The foreseen effects are radiation pressure, radiometer effect, temperature coefficient of optical components, etc. Onground estimations conclude that the temperature stability in the LTP must be less than 100 microK/sqrt(Hz) in the frequency range of 1 mHz to 30 mHz (LTP band). Since temperature fluctuations are an important issue in LPF and in LISA, a thermal diagnostic subsystem is needed aboard both missions.

The task of the thermal diagnostics in the LTP is twofold: on the one hand, temperature fluctuations in different subsystems must be measured with noise levels of 10 microK/sqrt(Hz) in the LTP band. On the other hand, a set of heaters will generate heat pulses that in conjunction with temperature measurements will be used to estimate the actual coupling between temperature and systems performance. These actions will provide information on the behaviour of the system and will permit to identify the fraction of noise in the system coming from temperature issues. The main function of LPF, as precursor mission of LISA, is the understanding of all the noise sources in the system. This will provide clues to the final leap from LPF sensitivity to LISA one.

The main investigations carried out during this thesis can be split into three main categories: (i) the design and validation of the LTP temperature measurement subsystem (TMS); (ii) the extension of the system to the LISA requirements; and (iii) the analysis of the in-flight thermal experiments in the LTP. The thesis is organised as follows: in chapter 2 we describe the designed electronics and the temperature sensors chosen. Aspects related to the coupling of the TMS with other subsystems nearby are discussed in chapter 3. Chapter 4 focuses on the design of the testbed needed for the validation of the TMS. Two different testbeds are described: one for the LTP measurement bandwidth (MBW) and another one for the LISA MBW, 0.1 mHz. In chapter 5 we present the results of the test campaigns: the prototype, the engineering model and the flight model systems were put to test. The results of the investigations in the LISA band are also shown. Chapter 6 contains investigations in view of LISA requirements to reduce excess noise at very low frequency and to reduce the floor noise of the measurement. Chapter 7 focuses on the thermal experiment on-board LPF: a set of thermal excitations are proposed to extract information of the thermal behaviour of the key subsystems of the LTP.

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Books on the topic "Laser Interferometer Space Antenna"

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1968-, Merkowitz Stephen M., Livas Jeffrey C, and Goddard Space Flight Center, eds. Laser interferometer space antenna: 6th International LISA Symposium, Greenbelt, Maryland, 19-23 June 2006. Melville, N.Y: American Institute of Physics, 2006.

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M, Folkner William, United States. Office of Space Science and Applications., Jet Propulsion Laboratory (U.S.), and California Institute of Technology, eds. Laser interferometer space antenna: Second International LISA Symposium on the Detection and Observation of Gravitational Waves in Space : Pasadena, California, July 1998. Woodbury, New York: American Institute of Physics, 1998.

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(Editor), Stephen M. Merkowitz, and Jeffrey C. Livas (Editor), eds. Laser Interferometer Space Antenna: Sixth International LISA Symposium (AIP Conference Proceedings / Astronomy and Astrophysics). American Institute of Physics, 2006.

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RL-34 ring laser gyro laboratory evaluation for the deep space network antenna application: Final report. [Washington, DC: National Aeronautics and Space Administration, 1991.

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United States. National Aeronautics and Space Administration., ed. RL-34 ring laser gyro laboratory evaluation for the deep space network antenna application: Final report. [Washington, DC: National Aeronautics and Space Administration, 1991.

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United States. National Aeronautics and Space Administration., ed. RL-34 ring laser gyro laboratory evaluation for the deep space network antenna application: Final report. [Washington, DC: National Aeronautics and Space Administration, 1991.

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Folkner, William M. Laser Interfermeter Space Antenna: Second International LISA Symposium on the Detection and Observation of Gravitational Waves in Space: California Institute ... Proceedings / Astronomy and Astrophysics). American Institute of Physics, 1998.

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Book chapters on the topic "Laser Interferometer Space Antenna"

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Rüdiger, Albrecht, Gerhard Heinzel, and Michael Tröbs. "LISA, the Laser Interferometer Space Antenna, Requires the Ultimate in Lasers, Clocks, and Drag-Free Control." In Lasers, Clocks and Drag-Free Control, 427–55. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34377-6_20.

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Bellei, G., P. Droll, F. Delhaise, I. Harrison, and D. Amend. "Laser Interferometer Space Antenna (LISA) Pathfinder: New Methods for Acquisition of Signal After Large Apogee-Raising Maneuvers." In Space Operations: Contributions from the Global Community, 567–83. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-51941-8_25.

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Johann, U., K. Danzmann, C. J. Schalinski, and R. Sesselmann. "Flite: Free Flyer Laser Interferometer Technology Experiment." In Infrared Space Interferometry: Astrophysics & the Study of Earth-Like Planets, 205–11. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5468-0_28.

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Clifton, Timothy. "4. Gravitational waves." In Gravity: A Very Short Introduction, 46–57. Oxford University Press, 2017. http://dx.doi.org/10.1093/actrade/9780198729143.003.0004.

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As stars collapse they eject huge amounts of mass and energy; their gravitational field changes rapidly and, therefore, so does the curvature of the space-time around them. If the curvature of space-time is pushed out of equilibrium, by the motion of mass or energy, this disturbance travels outwards as waves. ‘Gravitational waves’ explains the effect of a gravitational wave: in a binary pulsar, the waves carry energy away from the system so that the two neutron stars slowly circle in towards each other. Gravitational waves were first detected in 2015 by the Laser Interferometer Gravitational-Wave Observatory in America. There are also plans to set up a detector in space.

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Conference papers on the topic "Laser Interferometer Space Antenna"

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Folkner, W. "The Laser Interferometer Space Antenna mission." In Space 2000 Conference and Exposition. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2000. http://dx.doi.org/10.2514/6.2000-5129.

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Waluschka, Eugene, Tracy R. Pedersen, and Paul McNamara. "Modeling the Laser Interferometer Space Antenna Optics." In Frontiers in Optics. Washington, D.C.: OSA, 2005. http://dx.doi.org/10.1364/fio.2005.ftuz2.

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Leonhardt, Volker, and Jordan B. Camp. "Iodine laser frequency stabilization for LISA." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405068.

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Killow, C. J., J. Bogenstahl, F. Guzmán Cervantes, M. Perreur-Lloyd, D. I. Robertson, F. Steier, and H. Ward. "Construction of the LTP Optical Bench Interferometer." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405059.

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Schulte, Hans Reiner, Peter F. Gath, and Markus Herz. "Laser Frequency Stabilization by Using Arm-Locking." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405073.

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Sun, Ke-Xun, Patrick Lu, and Robert L. Byer. "A Robust, Symmetric Grating Angular Sensor for Space Flights." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405074.

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Hogan, Craig J. "Gravitational Wave Sources from New Physics." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405019.

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Saulson, Peter R. "Status of Ground-Based Gravitational Wave Detectors." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405020.

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McNamara, P. W. "LISA Pathfinder." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405021.

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Volonteri, Marta. "Supermassive black hole mergers and cosmological structure formation." In LASER INTERFEROMETER SPACE ANTENNA: 6th International LISA Symposium. AIP, 2006. http://dx.doi.org/10.1063/1.2405022.

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Reports on the topic "Laser Interferometer Space Antenna"

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Meadors, Grant. Laser Interferometer Space Antenna (LISA) Launch 2034: how LANL can engage today. Office of Scientific and Technical Information (OSTI), June 2021. http://dx.doi.org/10.2172/1804320.

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