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Sherri L. Horner,Srilate Bhattacharyya,Evelyn A. O’Connor,전홍 대한어린이교육협회 2008 어린이교육 Vol.- No.10
아이들을 관찰한 적이 있거나 함께 놀이해본 경험이 있는 사람이라면 아이들이 자신들이 본 것들(친구들, 형제자매, 부모, 교사들; 텔레비전, 영화, 책의 등장인물들; 그리고 때로는 집에서 기르는 애완동물들)을 어떻게 모방하는지를 알 것이다. 이러한 모방은 유아들이 적절한 행동, 태 도, 사고방식을 학습하는데 도움이 될 수 있다. 그러나 유아들이 적절하지 않거나 위험한 행동, 태도, 사고방식을 따라하게 된다면 모방은 해로울 수도 있다. 인생의 대부분의 일처럼, 어떻게 모 방이 일어나고 아이들이 누구를 모방할지를 고르는 것은 우리가 바라는 만큼 간단한 일은 아니 다. 사회인지이론의 창시자인 앨버트 반듀라(Albert Bandura)와 다른 연구자들은 아이들과 어른 들이 누구를 모방하며 무엇을 따라하는지에 영향을 주는 몇 가지 요인들을 밝혀내기 위한 연구를 수행하였다(Zimmerman& Schunk, 2003). 우리가 교사로서, 부모로서 이러한 요인들을 이해한 다면 우리는 유아들이 긍정적인 행동, 태도, 사고방식을 가진 모방 대상을 고르도록 도와줄 수 있 을 것이다.
The Dynamical History of Chariklo and Its Rings
Wood, Jeremy,Horner, Jonti,Hinse, Tobias C.,Marsden, Stephen C. American Astronomical Society 2017 The Astronomical journal Vol.153 No.6
<P>Chariklo is the only small solar system body confirmed to have rings. Given the instability of its orbit, the presence of rings is surprising, and their origin remains poorly understood. In this work, we study the dynamical history of the Chariklo system by integrating almost 36,000 Chariklo clones backward in time for 1 Gyr under the influence of the Sun and the four giant planets. By recording all close encounters between the clones and planets, we investigate the likelihood that Chariklo's rings could have survived since its capture to the Centaur population. Our results reveal that Chariklo's orbit occupies a region of stable chaos, resulting in its orbit being marginally more stable than those of the other Centaurs. Despite this, we find that it was most likely captured to the Centaur population within the last 20 Myr, and that its orbital evolution has been continually punctuated by regular close encounters with the giant planets. The great majority (> 99%) of those encounters within 1 Hill radius of the planet have only a small effect on the rings. We conclude that close encounters with giant planets have not had a significant effect on the ring structure. Encounters within the Roche limit of the giant planets are rare, making ring creation through tidal disruption unlikely.</P>
The Dynamical History of 2060 Chiron and Its Proposed Ring System
Wood, Jeremy,Horner, Jonti,Hinse, Tobias C.,Marsden, Stephen C. American Astronomical Society 2018 The Astronomical journal Vol.155 No.1
<P>The surprising discovery of a ring system around the Centaur 10199 Chariklo in 2013 led to a reanalysis of archival stellar occultation data for the Centaur 2060 Chiron by Ortiz et al. One possible interpretation of that data is that a system of rings exists around Chiron. In this work, we study the dynamical history of the proposed Chiron ring system by integrating nearly 36,000 clones of the Centaur backward in time for 100 Myr under the influence of the Sun and the four giant planets. The severity of all close encounters between the clones and planets while the clones are in the Centaur region is recorded, along with the mean time between close encounters. We find that severe and extreme close encounters are very rare, making it possible that the Chiron ring system has remained intact since its injection into the Centaur region, which we find likely occurred within the past 8.5 Myr. Our simulations yield a backward dynamical half-life for Chiron of 0.7 Myr. The dynamical classes of a sample of clones are found. It is found that, on average, the Centaur lifetimes of resonance hopping clones are twice those of random-walk clones because of resonance sticking in mean motion resonances. In addition, we present MEGNO and chaotic lifetime maps of the region bound by 13 au <= a <= 14 au and e <= 0.5. We confirm that the current mean orbital parameters of Chiron are located in a highly chaotic region of a - e phase space.</P>
An Orbital Stability Study of the Proposed Companions of SW Lyncis
Hinse, T.C.,Horner, Jonathan,Wittenmyer, Robert A. The Korean Space Science Society 2014 Journal of Astronomy and Space Sciences Vol.31 No.3
We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to substellar nature, and were inferred from timing measurements of the system's primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behavior. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically viable explanation for measured eclipse timing variations. We conclude that dynamical considerations reveal that the proposed SW Lyncis multi-body system most likely does not exist or the companions have significantly different orbital properties from those conjectured in Kim et al. (2010).
An Orbital Stability Study of the Proposed Companions of SW Lyncis
T. C. Hinse,Jonathan Horner,Robert A. Wittenmyer 한국우주과학회 2014 Journal of Astronomy and Space Sciences Vol.31 No.3
We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to substellar nature, and were inferred from timing measurements of the system’s primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behavior. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically viable explanation for measured eclipse timing variations. We conclude that dynamical considerations reveal that the proposed SW Lyncis multi-body system most likely does not exist or the companions have significantly different orbital properties from those conjectured in Kim et al. (2010).