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  ) the MathML source">>4.61$>4.61$ au, perihelion distance (q  ) the MathML source"><4.95$<4.95$ au, 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 (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 (the MathML source">2<T_J<3$2<T_J<3$) reached the JFC region for backward integrations. Considering these probabilities, 304 orbits of today&rsquo;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).