Author
Christopher Tylor
Bio: Christopher Tylor is an academic researcher from University of Southern Queensland. The author has contributed to research in topics: Jovian & Exoplanet. The author has an hindex of 5, co-authored 7 publications receiving 129 citations.
Topics: Jovian, Exoplanet, Trojan, Population, Planet
Papers
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University of Southern Queensland1, University of California, Riverside2, Academia Sinica Institute of Astronomy and Astrophysics3, Southwest Research Institute4, Hazard Community and Technical College5, Australian Nuclear Science and Technology Organisation6, Kindai University7, Australian National University8, University of New South Wales9, University of Jena10, Swinburne University of Technology11
TL;DR: A review of the current understanding of the solar system for the exoplanetary science community can be found in this paper, with a focus on the processes thought to have shaped the system we see today.
Abstract: Over the past three decades, we have witnessed one of the great revolutions in our understanding of the cosmos - the dawn of the Exoplanet Era. Where once we knew of just one planetary system (the Solar system), we now know of thousands, with new systems being announced on a weekly basis. Of the thousands of planetary systems we have found to date, however, there is only one that we can study up-close and personal - the Solar system.
In this review, we describe our current understanding of the Solar system for the exoplanetary science community - with a focus on the processes thought to have shaped the system we see today. In section one, we introduce the Solar system as a single well studied example of the many planetary systems now observed. In section two, we describe the Solar system's small body populations as we know them today - from the two hundred and five known planetary satellites to the various populations of small bodies that serve as a reminder of the system's formation and early evolution. In section three, we consider our current knowledge of the Solar system's planets, as physical bodies. In section four, we discuss the research that has been carried out into the Solar system's formation and evolution, with a focus on the information gleaned as a result of detailed studies of the system's small body populations. In section five, we discuss our current knowledge of planetary systems beyond our own - both in terms of the planets they host, and in terms of the debris that we observe orbiting their host stars.
As we learn ever more about the diversity and ubiquity of other planetary systems, our Solar system will remain the key touchstone that facilitates our understanding and modelling of those newly found systems, and we finish section five with a discussion of the future surveys that will further expand that knowledge.
75 citations
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University of Southern Queensland1, University of Oxford2, George Mason University3, University of California, Riverside4, University of Wisconsin-Madison5, Aarhus University6, University of Birmingham7, Smithsonian Institution8, University of Toronto9, Adolfo Ibáñez University10, Millennium Institute11, Space Telescope Science Institute12, University of New South Wales13, University of Louisville14, Kutztown University of Pennsylvania15, Vanderbilt University16, Fisk University17, University of Sydney18, University of Texas at Austin19, Wilmington University20, Massachusetts Institute of Technology21, University of Kansas22, Yale University23, Ames Research Center24, University of North Carolina at Chapel Hill25, Indiana University26, Nanjing University27, Max Planck Society28, Pontifical Catholic University of Chile29, Princeton University30, Open University31, Lehigh University32, Goddard Space Flight Center33, Florida Gulf Coast University34, University of Porto35, INAF36, Spanish National Research Council37, University of La Laguna38, Federal University of Rio Grande do Norte39, Université Paris-Saclay40, Paris Diderot University41, Pennsylvania State University42, Heidelberg University43, University of Vienna44, Iowa State University45, Erciyes University46, University of Paris47, New York University Abu Dhabi48
TL;DR: In this paper, the authors reported the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS).
Abstract: We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of MP = 0.138 ± 0.023 $\rm {M_J}$ (43.9 ± 7.3 $\, M_{\rm \oplus}$), a radius of RP = 0.639 ± 0.013 $\rm {R_J}$ (7.16 ± 0.15 $\, \mathrm{ R}_{\rm \oplus}$), bulk density of $0.65^{+0.12}_{-0.11}$ (cgs), and period $18.38818^{+0.00085}_{-0.00084}$ $\rm {days}$. TOI-257b orbits a bright (V = 7.612 mag) somewhat evolved late F-type star with M* = 1.390 ± 0.046 $\rm {M_{sun}}$, R* = 1.888 ± 0.033 $\rm {R_{sun}}$, Teff = 6075 ± 90 $\rm {K}$, and vsin i = 11.3 ± 0.5 km s−1. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.
45 citations
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TL;DR: In this paper, the authors investigate the stability of the two Trojan swarms, with a particular focus on these collisional families, and find that the members of Trojan swarm escape the population at a linear rate, with the primordial L4 (23.35 per cent escape) and L5 (24.89 per percent escape) population sizes likely 1.31 and 1.35 times larger than today.
Abstract: The Jovian Trojans are two swarms of objects located around the L4 and L5 Lagrange points. The population is thought to have been captured by Jupiter during the Solar system’s youth. Within the swarms, six collisional families have been identified in previous work, with four in the L4 swarm, and two in the L5. Our aim is to investigate the stability of the two Trojan swarms, with a particular focus on these collisional families. We find that the members of Trojan swarms escape the population at a linear rate, with the primordial L4 (23.35 per cent escape) and L5 (24.89 per cent escape) population sizes likely 1.31 and 1.35 times larger than today. Given that the escape rates were approximately equal between the two Trojan swarms, our results do not explain the observed asymmetry between the two groups, suggesting that the numerical differences are primordial in nature, supporting previous studies. Upon leaving the Trojan population, the escaped objects move on to orbits that resemble those of the Centaur and short-period comet populations. Within the Trojan collisional families, the 1996 RJ and 2001 UV209 families are found to be dynamically stable over the lifetime of the Solar system, whilst the Hektor, Arkesilos and Ennomos families exhibit various degrees of instability. The larger Eurybates family shows 18.81 per cent of simulated members escaping the Trojan population. Unlike the L4 swarm, the escape rate from the Eurybates family is found to increase as a function of time, allowing an age estimation of approximately 1.045 ± 0.364 × 109 yr.
21 citations
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University of Southern Queensland1, University of California, Riverside2, Academia Sinica Institute of Astronomy and Astrophysics3, Southwest Research Institute4, Hazard Community and Technical College5, Australian Nuclear Science and Technology Organisation6, Kindai University7, Australian National University8, University of New South Wales9, University of Jena10, Swinburne University of Technology11
TL;DR: In this paper, the authors present a review of the current understanding of the solar system for the exoplanetary science community, with a focus on the processes thought to have shaped the system we see today.
Abstract: Over the past three decades, we have witnessed one of the great revolutions in our understanding of the cosmos — the dawn of the Exoplanet Era. Where once we knew of just one planetary system (the solar system), we now know of thousands, with new systems being announced on a weekly basis. Of the thousands of planetary systems we have found to date, however, there is only one that we can study up-close and personal—the solar system. In this review, we describe our current understanding of the solar system for the exoplanetary science community — with a focus on the processes thought to have shaped the system we see today. In section one, we introduce the solar system as a single well studied example of the many planetary systems now observed. In section two, we describe the solar systemʼs small body populations as we know them today—from the two hundred and five known planetary satellites to the various populations of small bodies that serve as a reminder of the systemʼs formation and early evolution. In section three, we consider our current knowledge of the solar systemʼs planets, as physical bodies. In section four we discuss the research that has been carried out into the solar systemʼs formation and evolution, with a focus on the information gleaned as a result of detailed studies of the systemʼs small body populations. In section five, we discuss our current knowledge of planetary systems beyond our own — both in terms of the planets they host, and in terms of the debris that we observe orbiting their host stars. As we learn ever more about the diversity and ubiquity of other planetary systems, our solar system will remain the key touchstone that facilitates our understanding and modeling of those newly found systems, and we finish section five with a discussion of the future surveys that will further expand that knowledge.
19 citations
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TL;DR: In this paper, the authors reported the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS) and confirmed to be of planetary origin based on radial-velocity observations with the Minerva-Australis telescope array.
Abstract: We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial-velocity observations with the Minerva-Australis telescope array. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of $M_P=0.134^{+0.023}_{-0.022}$$\rm{M_J}$ ($42.6^{+7.3}_{-7.0}$$\rm{M_{\oplus}}$), a radius of $R_P=0.626^{+0.013}_{-0.012}$$\rm{R_J}$ ($7.02^{+0.15}_{-0.13}$$\rm{R_{\oplus}}$), and an orbit with eccentricity $0.242^{+0.040}_{-0.065}$ and period $18.38827\pm0.00072$$\rm{days}$. TOI-257b orbits a bright ($\mathrm{V}=7.570$mag) somewhat evolved late F-type star with $M_*=1.390\pm0.046$$\rm{M_{\odot}}$, $R_*=1.888\pm0.033$$\rm{R_{\odot}}$, $T_{\rm eff}=6075\pm90$$\rm{K}$, and $v\sin{i}=11.3\pm0.5$km/s. Additionally, we statistically validate a second non-transiting sub-Saturn mass planet on a $\sim71$day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.
19 citations
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TL;DR: Wallace and Hobbs as mentioned in this paper present a comprehensive textbook for undergraduate courses in atmospheric physics which contains general physical meteorology (atmospheric hydrostatics, cloud physics, radioactive transfer and thermodynamics), some selected topics of special interest (aerosol physics, aeronomy and physical climatology) and dynamic meteorology describing and interpreting large scale atmospheric motions.
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558 citations
01 Dec 2012
TL;DR: Computer simulations show that a giant impact on early Earth could lead to a Moon with a composition similar to Earth’s, and simulate impacts involving larger impactors than previously considered that can produce a disk with the same composition as the planet's mantle, consistent with Earth-Moon compositional similarities.
Abstract: In the giant impact theory, the Moon formed from debris ejected into an Earth-orbiting disk by the collision of a large planet with the early Earth. Prior impact simulations predict that much of the disk material originates from the colliding planet. However, Earth and the Moon have essentially identical oxygen isotope compositions. This has been a challenge for the impact theory, because the impactor’s composition would have likely differed from that of Earth. We simulated impacts involving larger impactors than previously considered. We show that these can produce a disk with the same composition as the planet’s mantle, consistent with Earth-Moon compositional similarities. Such impacts require subsequent removal of angular momentum from the Earth-Moon system through a resonance with the Sun as recently proposed.
378 citations