The Initial Physical Conditions of the Orion BN/KL Fingers
The Initial Physical Conditions of the Orion BN/KL Fingers
复制标题
Orion BN/KL 手指的初始物理状况
DOI：
10.3847/1538-4357/ab44b3
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发表时间：
2019
期刊：
影响因子：
--
通讯作者：
L. Zapata
中科院分区：
文献类型：
--
作者：
P. Rivera;Ary Rodr'iguez;Liliana Hern'andez;Jorge Cant'o;L. Zapata
猎户座BN/KL是恒星形成区域中人们知之甚少的现象的一个例子，涉及年轻恒星物体的近距离相遇。爆炸结构，观察到的分子种类繁多，事件所涉及的能量，以及该区域的质量表明对当地星际介质化学多样性的贡献。然而，其他类似事件的频率和持续时间尚未确定。在本文中，我们探讨了一个最近的分析模型，考虑到一个团簇与其分子环境的相互作用。我们表明，广泛的运动年龄的猎户座手指-500至4000年-是爆炸碎片与周围介质的相互作用的结果。该模型较好地解释了猎户座指状物的年龄差异，并推断了爆炸的初始条件和寿命。此外，我们的模型可以解释为什么一些CO流光没有相关的H2手指。
Orion BN/KL is an example of a poorly understood phenomena in star-forming regions involving the close encounters of young stellar objects. The explosive structure, the great variety of molecules observed, the energy involved in the event, and the mass of the region suggest a contribution to the chemical diversity of the local interstellar medium. Nevertheless, the frequency and duration of other, similar events have not been determined. In this paper, we explore a recent analytic model that takes into account the interaction of a clump with its molecular environment. We show that the widespread kinematic ages of the Orion fingers—500 to 4000 yr—are a consequence of the interaction of the explosion debris with the surrounding medium. This model explains satisfactorily the age discrepancy of the Orion fingers, and infers the initial conditions together with the lifetime of the explosion. Moreover, our model can explain why some CO streamers do not have an associated H2 finger.
DOI：
10.1051/0004-6361/201834049
发表时间：
2018-03
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
Shuo Kong;H. Arce;J. Feddersen;J. Carpenter;F. Nakamura;Y. Shimajiri;A. Isella;V. Ossenkopf-Okada;A. Sargent;Á. Sánchez-Monge;S. Suri;J. Kauffmann;T. Pillai;J. Pineda;J. Koda;J. Bally;D. Lis;P. Padoan;R. Klessen;S. Mairs;A. Goodman;P. Goldsmith;P. McGehee;P. Schilke;P. Teuben;M. Maureira;C. Hara;A. Ginsburg;B. Burkhart;Rowan J. Smith;A. Schmiedeke;J. Pineda;S. Ishii;K. Sasaki;R. Kawabe;Yumiko Urasawa;S. Oyamada;Yoshihiro Tanabe
通讯作者：
Shuo Kong;H. Arce;J. Feddersen;J. Carpenter;F. Nakamura;Y. Shimajiri;A. Isella;V. Ossenkopf-Okada;A. Sargent;Á. Sánchez-Monge;S. Suri;J. Kauffmann;T. Pillai;J. Pineda;J. Koda;J. Bally;D. Lis;P. Padoan;R. Klessen;S. Mairs;A. Goodman;P. Goldsmith;P. McGehee;P. Schilke;P. Teuben;M. Maureira;C. Hara;A. Ginsburg;B. Burkhart;Rowan J. Smith;A. Schmiedeke;J. Pineda;S. Ishii;K. Sasaki;R. Kawabe;Yumiko Urasawa;S. Oyamada;Yoshihiro Tanabe
影响因子：
6.5
作者：
K. Menten;M. Reid;J. Forbrich;J. Forbrich;A. Brunthaler
通讯作者：
K. Menten;M. Reid;J. Forbrich;J. Forbrich;A. Brunthaler
DOI：
10.1088/0004-637x/727/2/113
发表时间：
2010-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
J. Bally;N. Cunningham;N. Moeckel;M. Burton;N. Smith;A. Frank;Å. Nordlund
通讯作者：
J. Bally;N. Cunningham;N. Moeckel;M. Burton;N. Smith;A. Frank;Å. Nordlund