Institution
Vaughn College of Aeronautics and Technology
Education•New York, New York, United States•
About: Vaughn College of Aeronautics and Technology is a education organization based out in New York, New York, United States. It is known for research contribution in the topics: Gravitational microlensing & Planetary system. The organization has 727 authors who have published 708 publications receiving 14082 citations. The organization is also known as: College of Aeronautics.
Papers published on a yearly basis
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Chungbuk National University1, University of Warsaw2, Osaka University3, Ohio State University4, University of Notre Dame5, Queen Mary University of London6, Las Cumbres Observatory Global Telescope Network7, University of Concepción8, University of Cambridge9, Nagoya University10, Massey University11, University of Auckland12, Victoria University of Wellington13, Vaughn College of Aeronautics and Technology14, Texas A&M University15, Princeton University16, Korea Astronomy and Space Science Institute17, Qatar Airways18, University of Salerno19, European Southern Observatory20, University of St Andrews21, Max Planck Society22, Liverpool John Moores University23
TL;DR: The OGLE-2012-BLG-0358Lb system as discussed by the authors is a relatively tightly separated binary composed of a planetary-mass object with 1.9 ± 0.2 Jupiter masses orbiting a BD with a mass 0.022 M ☉.
Abstract: Observations of accretion disks around young brown dwarfs (BDs) have led to the speculation that they may form planetary systems similar to normal stars. While there have been several detections of planetary-mass objects around BDs (2MASS 1207-3932 and 2MASS 0441-2301), these companions have relatively large mass ratios and projected separations, suggesting that they formed in a manner analogous to stellar binaries. We present the discovery of a planetary-mass object orbiting a field BD via gravitational microlensing, OGLE-2012-BLG-0358Lb. The system is a low secondary/primary mass ratio (0.080 ± 0.001), relatively tightly separated (~0.87 AU) binary composed of a planetary-mass object with 1.9 ± 0.2 Jupiter masses orbiting a BD with a mass 0.022 M ☉. The relatively small mass ratio and separation suggest that the companion may have formed in a protoplanetary disk around the BD host in a manner analogous to planets.
89 citations
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Goddard Space Flight Center1, University of Notre Dame2, University of Warsaw3, Korea Astronomy and Space Science Institute4, Ohio State University5, Max Planck Society6, Las Cumbres Observatory Global Telescope Network7, Heidelberg University8, Institut d'Astrophysique de Paris9, Massey University10, University of Tasmania11, University of Auckland12, Yale University13, Pennsylvania State University14, Space Telescope Science Institute15, Nagoya University16, Osaka University17, Vaughn College of Aeronautics and Technology18, Victoria University of Wellington19, Kyoto Sangyo University20, Texas A&M University21, Weizmann Institute of Science22, Chungbuk National University23, Qatar Foundation24, University of St Andrews25, Open University26, Liverpool John Moores University27, University of Canterbury28, University of Rijeka29, University of Vienna30, University of Toulouse31, Niels Bohr Institute32, San Francisco State University33, Curtin University34
TL;DR: The OGLE-2007-BLG-349 microlensing event has a strong planetary signal that is best fit with a mass ratio q ≈ 3.4 × 10-4, but there is an additional signal due to an additional lens mass, either another planet or another star as mentioned in this paper.
Abstract: © 2016. The American Astronomical Society. All rights reserved.We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of q ≈ 3.4 × 10-4, but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be M L ≈ 0.7 M⊙. Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass m c = 80 ± 13 M⊙, orbiting a pair of M dwarfs with masses of M A = 0.41 ± 0.07 and M B = 0.30 ± 0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.
89 citations
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TL;DR: In this paper, the authors examined the effect on laminated composites of in-plane compression followed by impact damage, and the coupling between the two, on compression-after-impact (CAI) performance.
88 citations
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TL;DR: In this article, four different ways of modelling delamination growth of a double cantilever beam test (DCB) are proposed, based on a cohesive zone model: the interface being represented either by using delamination elements or non-linear springs.
87 citations
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TL;DR: In this article, the authors presented the analysis of four candidate short-duration binary microlensing events from the 2006-2007 MOA Project short-event analysis, which were discovered as a byproduct of an analysis designed to find short-timescale single-lens events that may be due to free-floating planets.
Abstract: We present the analysis of four candidate short-duration binary microlensing events from the 2006-2007 MOA Project short-event analysis. These events were discovered as a by-product of an analysis designed to find short-timescale single-lens events that may be due to free-floating planets. Three of these events are determined to be microlensing events, while the fourth is most likely caused by stellar variability. For each of the three microlensing events, the signal is almost entirely due to a brief caustic feature with little or no lensing attributable mainly to the lens primary. One of these events, MOA-bin-1, is due to a planet, and it is the first example of a planetary event in which the stellar host is only detected through binary microlensing effects. The mass ratio and separation are q (4.9 {+-} 1.4) Multiplication-Sign 10{sup -3} and s = 2.10 {+-} 0.05, respectively. A Bayesian analysis based on a standard Galactic model indicates that the planet, MOA-bin-1Lb, has a mass of m{sub p} = 3.7 {+-} 2.1 M{sub Jup} and orbits a star of M{sub *} = 0.75{sub -0.41}{sup +}0{sup .33} M{sub Sun} at a semimajor axis of a = 8.3{sub -2.7}{sup +4.5} AU. This is one of the most massivemore » and widest separation planets found by microlensing. The scarcity of such wide-separation planets also has implications for interpretation of the isolated planetary mass objects found by this analysis. If we assume that we have been able to detect wide-separation planets with an efficiency at least as high as that for isolated planets, then we can set limits on the distribution of planets in wide orbits. In particular, if the entire isolated planet sample found by Sumi et al. consists of planets bound in wide orbits around stars, we find that it is likely that the median orbital semimajor axis is >30 AU.« less
87 citations
Authors
Showing all 732 results
Name | H-index | Papers | Citations |
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Xiang Zhang | 154 | 1733 | 117576 |
Denis J. Sullivan | 61 | 332 | 14092 |
To. Saito | 51 | 183 | 9392 |
Arthur H. Lefebvre | 41 | 123 | 4896 |
Michele Meo | 40 | 223 | 5557 |
Robin S. Langley | 40 | 263 | 5601 |
Ning Qin | 37 | 283 | 5011 |
Holger Babinsky | 33 | 242 | 4068 |
B. S. Gaudi | 31 | 64 | 2560 |
Philip J. Longhurst | 29 | 80 | 2578 |
Michael Gaster | 27 | 66 | 3998 |
Don Harris | 26 | 129 | 2537 |
To. Saito | 25 | 56 | 2362 |
John F. O'Connell | 22 | 89 | 1763 |
Rade Vignjevic | 21 | 84 | 1563 |