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Yasunobu Nakamura - One of the best experts on this subject based on the ideXlab platform.
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single photon quantum regime of artificial Radiation Pressure on a surface acoustic wave resonator
Nature Communications, 2020Co-Authors: Atsushi Noguchi, Rekishu Yamazaki, Yutaka Tabuchi, Yasunobu NakamuraAbstract:Electromagnetic fields carry momentum, which upon reflection on matter gives rise to the Radiation Pressure of photons. The Radiation Pressure has recently been utilized in cavity optomechanics for controlling mechanical motions of macroscopic objects at the quantum limit. However, because of the weakness of the interaction, attempts so far had to use a strong coherent drive to reach the quantum limit. Therefore, the single-photon quantum regime, where even the presence of a totally off-resonant single photon alters the quantum state of the mechanical mode significantly, is one of the next milestones in cavity optomechanics. Here we demonstrate an artificial realization of the Radiation Pressure of microwave photons acting on phonons in a surface acoustic wave resonator. The order-of-magnitude enhancement of the interaction strength originates in the well-tailored, strong, second-order nonlinearity of a superconducting Josephson junction circuit. The synthetic Radiation Pressure interaction adds a key element to the quantum optomechanical toolbox and can be applied to quantum information interfaces between electromagnetic and mechanical degrees of freedom. The Radiation Pressure of light on a mechanical oscillator can be used to manipulate mechanical degrees of freedom in the quantum regime. Noguchi et al. use Josephson junctions to realize an artificial system where the Radiation Pressure of a single photon is stronger than the effect of dissipation.
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single photon quantum regime of artificial Radiation Pressure on a surface acoustic wave resonator
arXiv: Quantum Physics, 2018Co-Authors: Atsushi Noguchi, Rekishu Yamazaki, Yutaka Tabuchi, Yasunobu NakamuraAbstract:Electromagnetic fields carry momentum, which upon reflection on matter gives rise to the Radiation Pressure of photons. The Radiation Pressure has recently been utilized in cavity optomechanics for controlling mechanical motions of macroscopic objects at the quantum limit. However, because of the weakness of the interaction, attempts so far had to use a strong coherent drive to reach the quantum limit Therefore, the single-photon quantum regime, where even the presence of a totally off-resonant single photon alters the quantum state of the mechanical mode significantly, is one of the next milestones in cavity optomechanics. Here we demonstrate an artificial realization of the Radiation Pressure of microwave photons acting on phonons in a surface acoustic wave resonator. The order-of-magnitude enhancement of the interaction strength originates in the well-tailored strong second-order nonlinearity of a superconducting Josephson-junction circuit. The synthetic Radiation Pressure interaction adds a key element to the quantum optomechanical toolbox and can be applied to quantum information interfaces between electromagnetic and mechanical degrees of freedom.
T A Thompson - One of the best experts on this subject based on the ideXlab platform.
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the disruption of giant molecular clouds by Radiation Pressure the efficiency of star formation in galaxies
The Astrophysical Journal, 2010Co-Authors: Norman Murray, Eliot Quataert, T A ThompsonAbstract:Star formation is slow in the sense that the gas consumption time is much longer than the dynamical time. It is also inefficient; star formation in local galaxies takes place in giant molecular clouds (GMCs), but the fraction of a GMC converted to stars is very small, GMC ~ 5%. In luminous starbursts, the GMC lifetime is shorter than the main-sequence lifetime of even the most massive stars, so that supernovae can play no role in GMC disruption. We investigate the disruption of GMCs across a wide range of galaxies from normal spirals to the densest starbursts; we take into account the effects of H II gas Pressure, shocked stellar winds, protostellar jets, and Radiation Pressure produced by the absorption and scattering of starlight on dust grains. In the Milky Way, a combination of three mechanisms—jets, H II gas Pressure, and Radiation Pressure—disrupts the clouds. In more rapidly star-forming galaxies such as "clump" galaxies at high-redshift, ultra-luminous infrared galaxies (ULIRGs), and submillimeter galaxies, Radiation Pressure dominates natal cloud disruption. We predict the presence of ~10-20 clusters with masses ~107 M ☉ in local ULIRGs such as Arp 220 and a similar number of clusters with M * ~ 108 M ☉ in high redshift clump galaxies; submillimeter galaxies will have even more massive clusters. We find that GMC = πGΣGMC c/(2(L/M *)) for GMCs that are optically thin to far-infrared Radiation, where ΣGMC is the GMC gas surface density. The efficiency in optically thick systems continues to increase with ΣGMC, but more slowly, reaching ~35% in the most luminous starbursts. The disruption of bubbles by Radiation Pressure stirs the interstellar medium (ISM) to velocities of ~10 km s–1 in normal galaxies and to ~100 km s–1 in ULIRGs like Arp 220, consistent with observations. Thus, Radiation Pressure may play a dominant dynamical role in the ISM of star-forming galaxies.
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the disruption of giant molecular clouds by Radiation Pressure and the efficiency of star formation in galaxies
arXiv: Astrophysics of Galaxies, 2009Co-Authors: Norman Murray, Eliot Quataert, T A ThompsonAbstract:Star formation is slow, in the sense that the gas consumption time is much longer than the dynamical time. It is also inefficient; essentially all star formation in local galaxies takes place in giant molecular clouds (GMCs), but the fraction of a GMC converted to stars is very small, ~5%. In the most luminous starbursts, the GMC lifetime is shorter than the main sequence lifetime of even the most massive stars, so that supernovae can play no role in GMC disruption. We investigate the disruption of GMCs across a wide range of galaxies, from normal spirals to the densest starbursts; we take into account the effects of HII gas Pressure, shocked stellar winds, protostellar jets, and Radiation Pressure produced by the absorption and scattering of starlight on dust grains. In the Milky Way, we find that a combination of three mechanisms, jets, HII gas Pressure, and Radiation Pressure, disrupts the clouds. In more rapidly star forming galaxies such as ``clump'' galaxies at high-redshift, ultra-luminous infrared galaxies (ULIRGs) and submillimeter galaxies, Radiation Pressure dominates natal cloud distribution. We predict the presence of 10-20 clusters with masses ~10^7 Msun in local ULIRGs such as Arp 220 and a similar number of clusters with M_* ~ 10^8 Msun in high redshift clump galaxies; submillimeter galaxies will have even more massive clusters. We find that the mass fraction of a GMC that ends up in stars is an increasing function of the gas surface density of a galaxy, reaching ~35% in the most luminous starbursts. Furthermore, the disruption of bubbles by Radiation Pressure stirs the interstellar medium to velocities of ~10 km/s in normal galaxies and to ~100 km/s in ULIRGs like Arp 220, consistent with observations. Thus, Radiation Pressure may play a dominant role in the ISM of star-forming galaxies.
Atsushi Noguchi - One of the best experts on this subject based on the ideXlab platform.
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single photon quantum regime of artificial Radiation Pressure on a surface acoustic wave resonator
Nature Communications, 2020Co-Authors: Atsushi Noguchi, Rekishu Yamazaki, Yutaka Tabuchi, Yasunobu NakamuraAbstract:Electromagnetic fields carry momentum, which upon reflection on matter gives rise to the Radiation Pressure of photons. The Radiation Pressure has recently been utilized in cavity optomechanics for controlling mechanical motions of macroscopic objects at the quantum limit. However, because of the weakness of the interaction, attempts so far had to use a strong coherent drive to reach the quantum limit. Therefore, the single-photon quantum regime, where even the presence of a totally off-resonant single photon alters the quantum state of the mechanical mode significantly, is one of the next milestones in cavity optomechanics. Here we demonstrate an artificial realization of the Radiation Pressure of microwave photons acting on phonons in a surface acoustic wave resonator. The order-of-magnitude enhancement of the interaction strength originates in the well-tailored, strong, second-order nonlinearity of a superconducting Josephson junction circuit. The synthetic Radiation Pressure interaction adds a key element to the quantum optomechanical toolbox and can be applied to quantum information interfaces between electromagnetic and mechanical degrees of freedom. The Radiation Pressure of light on a mechanical oscillator can be used to manipulate mechanical degrees of freedom in the quantum regime. Noguchi et al. use Josephson junctions to realize an artificial system where the Radiation Pressure of a single photon is stronger than the effect of dissipation.
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single photon quantum regime of artificial Radiation Pressure on a surface acoustic wave resonator
arXiv: Quantum Physics, 2018Co-Authors: Atsushi Noguchi, Rekishu Yamazaki, Yutaka Tabuchi, Yasunobu NakamuraAbstract:Electromagnetic fields carry momentum, which upon reflection on matter gives rise to the Radiation Pressure of photons. The Radiation Pressure has recently been utilized in cavity optomechanics for controlling mechanical motions of macroscopic objects at the quantum limit. However, because of the weakness of the interaction, attempts so far had to use a strong coherent drive to reach the quantum limit Therefore, the single-photon quantum regime, where even the presence of a totally off-resonant single photon alters the quantum state of the mechanical mode significantly, is one of the next milestones in cavity optomechanics. Here we demonstrate an artificial realization of the Radiation Pressure of microwave photons acting on phonons in a surface acoustic wave resonator. The order-of-magnitude enhancement of the interaction strength originates in the well-tailored strong second-order nonlinearity of a superconducting Josephson-junction circuit. The synthetic Radiation Pressure interaction adds a key element to the quantum optomechanical toolbox and can be applied to quantum information interfaces between electromagnetic and mechanical degrees of freedom.
Hideko Nomura - One of the best experts on this subject based on the ideXlab platform.
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outward motion of porous dust aggregates by stellar Radiation Pressure in protoplanetary disks
The Astrophysical Journal, 2015Co-Authors: Ryo Tazaki, Hideko NomuraAbstract:We study the dust motion at the surface layer of protoplanetary disks. Dust grains in the surface layer migrate outward owing to angular momentum transport via gas-drag force induced by the stellar Radiation Pressure. In this study we calculate the mass flux of the outward motion of compact grains and porous dust aggregates by the Radiation Pressure. The Radiation Pressure force for porous dust aggregates is calculated using the T-Matrix Method for the Clusters of Spheres. First, we confirm that porous dust aggregates are forced by strong Radiation Pressure even if they grow to be larger aggregates, in contrast to homogeneous and spherical compact grains, for which Radiation Pressure efficiency becomes lower when their sizes increase. In addition, we find that the outward mass flux of porous dust aggregates with monomer size of 0.1 μm is larger than that of compact grains by an order of magnitude at the disk radius of 1 AU, when their sizes are several microns. This implies that large compact grains like calcium-aluminum-rich inclusions are hardly transported to the outer region by stellar Radiation Pressure, whereas porous dust aggregates like chondritic-porous interplanetary dust particles are efficiently transported to the comet formation region. Crystalline silicates are possibly transported in porous dust aggregates by stellar Radiation Pressure from the inner hot region to the outer cold cometary region in the protosolar nebula.
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outward motion of porous dust aggregates by stellar Radiation Pressure in protoplanetary disks
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Ryo Tazaki, Hideko NomuraAbstract:We study the dust motion at the surface layer of protoplanetary disks. Dust grains in surface layer migrate outward due to angular momentum transport via gas-drag force induced by the stellar Radiation Pressure. In this study, we calculate mass flux of the outward motion of compact grains and porous dust aggregates by the Radiation Pressure. The Radiation Pressure force for porous dust aggregates is calculated using the T-Matrix Method for the Clusters of Spheres. First, we confirm that porous dust aggregates are forced by strong Radiation Pressure even if they grow to be larger aggregates in contrast to homogeneous and spherical compact grains to which efficiency of Radiation Pressure becomes lower when their sizes increase. In addition, we find that the outward mass flux of porous dust aggregates with monomer size of 0.1 $\mu$m is larger than that of compact grains by an order of magnitude at the disk radius of 1 AU, when their sizes are several microns. This implies that large compact grains like calcium-aluminum rich inclusions (CAIs) are hardly transported to outer region by stellar Radiation Pressure, whereas porous dust aggregates like chondritic-porous interplanetary dust particles (CP-IDPs) are efficiently transported to comet formation region. Crystalline silicates are possibly transported in porous dust aggregates by stellar Radiation Pressure from inner hot region to outer cold cometary region in the protosolar nebula.
Camilla Colombo - One of the best experts on this subject based on the ideXlab platform.
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solar Radiation Pressure hamiltonian feedback control for unstable libration point orbits
Journal of Guidance Control and Dynamics, 2017Co-Authors: Stefania Soldini, Camilla Colombo, Scott J I WalkerAbstract:This work investigates a Hamiltonian structure-preserving control that uses the acceleration of solar Radiation Pressure for the stabilization of unstable periodic orbits in the circular restricted...
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solar Radiation Pressure augmented deorbiting passive end of life disposal from high altitude orbits
Journal of Spacecraft and Rockets, 2013Co-Authors: Charlotte Lucking, Camilla ColomboAbstract:A deorbiting strategy for small satellites is proposed that exploits the effect of solar Radiation Pressure to increase the spacecraft orbit eccentricity so that the perigee falls below an altitude where atmospheric drag will cause the spacecraft orbit to naturally decay. This is achieved by fitting the spacecraft with an inflatable reflective balloon. Once this is fully deployed, the overall area-to-mass ratio of the spacecraft is increased; hence, solar Radiation Pressure and aerodynamic drag have a greatly increased effect on the spacecraft orbit. An analytical model of the orbit evolution due to solar Radiation Pressure and the J2 effect as a Hamiltonian system show the evolution of an initially circular orbit. The maximum reachable orbit eccentricity as a function of semimajor axis and area-to-mass ratio is found analytically for deorbiting from circular equatorial orbits of different altitudes. The analytical planar model is then adapted for sun-synchronous orbits. The model is validated numerically...
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solar Radiation Pressure augmented deorbiting from high altitude sun synchronous orbits
4S Symposium 2012 Small Satellites Systems and Services, 2012Co-Authors: Charlotte Lucking, Camilla ColomboAbstract:This paper discusses the use of solar Radiation Pressure (SRP) augmented deorbiting to passively remove small satellites from high altitude Sun-synchronous orbits. SRP-augmented deorbiting works by deploying a light-weight reflective inflatable device to increase the area-to-mass-ratio of the spacecraft. The interactions of the orbital perturbations due to solar Radiation Pressure and the Earth’s oblateness cause the eccentricity of the orbit to librate at a quasi-constant semi-major axis. A large enough area-to-mass-ratio will ensure that a maximum eccentricity is reached where the spacecraft will then experience enough aerodynamic drag at the orbit pericentre to deorbit. An analytical model of the orbital evolution based on a Hamiltonian approach is used to obtain a first guess for the required area-to-mass-ratio to deorbit. This first guess is then used in a numerical propagation of the orbital elements using the Gauss’ equations to find the actual requirements as a function of altitude. The results are discussed and altitude regions for Sun-synchronous orbits are identified in which the proposed method is most effective. Finally, the implementation of the device is discussed. It is shown that passive solar Radiation Pressure deorbiting is a useful alternative to propulsive end-of-life manoeuvres for future high altitude Sun-synchronous missions.
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orbital dynamics of smart dust devices with solar Radiation Pressure and drag
Journal of Guidance Control and Dynamics, 2011Co-Authors: Camilla Colombo, Colin R. McinnesAbstract:This paper investigates how perturbations due to asymmetric solar Radiation Pressure, in the presence of Earth shadow, and atmospheric drag can be balanced to obtain long-lived Earth centred orbits for swarms of micro-scale 'smart dust' devices, without the use of active control. The secular variation of Keplerian elements is expressed analytically through an averaging technique. Families of solutions are then identified where Sun-synchronous apse-line precession is achieved passively to maintain asymmetric solar Radiation Pressure. The long-term orbit evolution is characterized by librational motion, progressively decaying due to the non-conservative effect of atmospheric drag. Long-lived orbits can then be designed through the interaction of energy gain from asymmetric solar Radiation Pressure and energy dissipation due to drag. In this way, the usual short drag lifetime of such high area-to-mass spacecraft can be greatly extended (and indeed selected). In addition, the effect of atmospheric drag can be exploited to ensure the rapid end-of-life decay of such devices, thus preventing long-lived orbit debris.