Modelling the 3D morphology and proper motions of the planetary nebula NGC 6302

被引：7

作者：

Uscanga, L. ^{[1
]}

Velazquez, P. F. ^{[2
]}

Esquivel, A. ^{[2
]}

Raga, A. C. ^{[2
]}

Boumis, P. ^{[1
]}

Canto, J. ^{[3
]}

机构：

[1] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Athens 15236, Greece

[2] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico

[3] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 442卷 / 04期

关键词：

methods: numerical; planetary nebulae: general; planetary nebulae: individual: NGC 6302; RADIATION GASDYNAMICS; VELOCITY STATISTICS; NGC-6302; OUTFLOWS; EVOLUTION; REGION; CLOUD;

D O I：

10.1093/mnras/stu1064

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present 3D hydrodynamical simulations of an isotropic fast wind interacting with a previously ejected toroidally shaped slow wind in order to model both the observed morphology and the kinematics of the planetary nebula (PN) NGC 6302. This source, also known as the Butterfly nebula, presents one of the most complex morphologies ever observed in PNe. From our numerical simulations, we have obtained an intensity map for the H alpha emission to make a comparison with the Hubble Space Telescope (HST) observations of this object. We have also carried out a proper motion (PM) study from our numerical results, in order to compare with previous observational studies. We have found that the two interacting stellar wind model reproduce well the morphology of NGC 6302, and while the PMs in the models are similar to the observations, our results suggest that an acceleration mechanism is needed to explain the Hubble-type expansion found in HST observations.

引用

页码：3162 / 3165

页数：4

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