3D magnetic-field morphology of the Perseus molecular cloud

被引：34

作者：

Tahani, M. ^{[1
]}

Lupypciw, W. ^{[1
,2
]}

Glover, J. ^{[1
,3
]}

Plume, R. ^{[2
]}

West, J. L. ^{[4
]}

Kothes, R. ^{[1
]}

Inutsuka, S. ^{[5
]}

Lee, M-Y ^{[6
]}

Robishaw, T. ^{[1
]}

Knee, L. B. G. ^{[7
]}

Brown, J. C. ^{[2
]}

Doi, Y. ^{[8
]}

Grenier, I. A. ^{[9
,10
]}

Haverkorn, M. ^{[11
]}

机构：

[1] Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, Dominion Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada

[2] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada

[3] Univ Victoria, Dept Phys & Astron, Columbia, BC V8P 5C2, Canada

[4] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[5] Nagoya Univ, Grad Sch Sci, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan

[6] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea

[7] Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[8] Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan

[9] Univ Paris, F-91190 Gif Sur Yvette, France

[10] Univ Paris Saclay, CEA, CNRS, AIM, F-91190 Gif Sur Yvette, France

[11] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 660卷

基金：

欧洲研究理事会; 加拿大自然科学与工程研究理事会;

关键词：

stars; formation; ISM; magnetic fields; clouds; evolution; general; JCMT BISTRO SURVEY; LINE-OF-SIGHT; MILKY-WAY; CO SURVEY; TAURUS; DISSIPATION; TURBULENCE; STRENGTHS; FILAMENTS; EVOLUTION;

D O I：

10.1051/0004-6361/202141170

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Despite recent observational and theoretical advances in mapping the magnetic fields associated with molecular clouds, their three-dimensional (3D) morphology remains unresolved. Multi-wavelength and multi-scale observations will allow us to paint a comprehensive picture of the magnetic fields of these star-forming regions. Aims. We reconstructed the 3D magnetic field morphology associated with the Perseus molecular cloud and compared it with predictions of cloud-formation models. These cloud-formation models predict a bending of magnetic fields associated with filamentary molecular clouds. We compared the orientation and direction of this field bending with our 3D magnetic-field view of the Perseus cloud. Methods. We used previous line-of-sight and plane-of-sky magnetic field observations as well as Galactic magnetic field models to reconstruct the complete 3D magnetic field vectors and morphology associated with the Perseus cloud. Results. We approximated the 3D magnetic field morphology of the cloud as a concave arc that points in the decreasing longitude direction in the plane of the sky (from our point of view). This field morphology preserves a memory of the Galactic magnetic field. In order to compare this morphology to cloud-formation model predictions, we assume that the cloud retains a memory of its most recent interaction. After incorporating velocity observations, we find that the line-of-sight magnetic field observations are consistent with predictions of shock-cloud-interaction models. Conclusions. To our knowledge, this is the first time that the 3D magnetic fields of a molecular cloud have been reconstructed. We find the 3D magnetic field morphology of the Perseus cloud to be consistent with the predictions of the shock-cloud-interaction model that describes the formation mechanism of filamentary molecular clouds.

引用

页数：13

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