Dynamical analyses on the transitivity from JFC and Centaur regions to NEAs with Tisserand parameters from 2 to 3

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• 作者：Murat Kaplan^a ; ^{muratkaplan@akdeniz.edu.tr" class="auth_mail" title="E-mail the corresponding author} ; Orhan Erece^a ; ^b ; Gü ; rkan Aslan^a ; Zeki Eker^a
• 关键词：Asteroids ; Near-Earth objects
• 刊名：Advances in Space Research
• 出版年：2016
• 出版时间：1 December 2016
• 年：2016
• 卷：58
• 期：11
• 页码：2407-2415
• 全文大小：835 K

文摘

We study the contribution of JFC (Jupiter family comet) and Centaur regions to the NEA (near Earth asteroid) population having Tisserand parameters for Jupiter between 2 and 3. We define a region for JFCs (aphelion distance (Q  ) >4.61$>4.61$ au, perihelion distance (q  ) <4.95$<4.95$ au, b45565cff" title="Click to view the MathML source">>1.3$>1.3$ au) and we check the contributions of selected bodies (JFCs, Centaurs, Halley-type comets (HTCs), some elliptic comets, and some outer main belt asteroids) from various regions to the NEA region. Additionally, we integrated NEAs with Tisserand parameters for Jupiter (05be8435e3c5279" title="Click to view the MathML source">T_J$T_J$) between 2 and 3 and their clones backward in time to see whether there was a strong dynamical path between those NEAs and the defined JFC region. As a result, 35.1% of the orbits from the defined JFC region turned out to be Earth-crossing orbits for forward integrations, while 66.7% of NEAs (2<T_J<3$2<T_J<3$) reached the JFC region for backward integrations. Considering these probabilities, 304 orbits of today’s JFC regional bodies can contribute the Earth-crossing asteroids in 0.55 Myr. Almost 254 NEA regional bodies look like they came from the defined region in a comparable time interval (0.80 Myr).