Query : 2019A&A...628A.112K

2019A&A...628A.112K - Astronomy and Astrophysics, volume 628A, 112-112 (2019/8-1)

The bridge: a transient phenomenon of forming stellar multiples. Sequential formation of stellar companions in filaments around young protostars.


Abstract (from CDS):

Context. Observations with modern instruments such as Herschel reveal that stars form clustered inside filamentary arms of ∼1pc length embedded in giant molecular clouds (GMCs). On smaller scales of ∼1000au, observations of IRAS 16293-2422, for example, show signs of filamentary "bridge" structures connecting young protostars to their birth environment.
Aims. We aim to find the origin of bridges associated with deeply embedded protostars by characterizing their connection to the filamentary structure present on GMC scales and to the formation of protostellar multiples.
Methods. Using the magnetohydrodynamical codeRAMSES, we carried out zoom-in simulations of low-mass star formation starting from GMC scales. We analyzed the morphology and dynamics involved in the formation process of a triple system. Results. Colliding flows of gas in the filamentary arms induce the formation of two protostellar companions at distances of ∼1000au from the primary. After their birth, the stellar companions quickly approach, at Δt∼10kyr, and orbit the primary on eccentric orbits with separations of ∼100au. The colliding flows induce transient structures lasting for up to a few 10 kyr that connect two forming protostellar objects that are kinematically quiescent along the line-of-sight.Conclusions. Colliding flows compress gas and trigger the formation of stellar companions via turbulent fragmentation. Our results suggest that protostellar companions initially form with a wide separation of ∼1000au. Smaller separations of a≤100au are a consequence of subsequent migration and capturing. Associated with the formation phase of the companion, the turbulent environment induces the formation of arc- and bridge-like structures. These bridges can become kinematically quiescent when the velocity components of the colliding flows eliminate each other. However, the gas in bridges still contributes to stellar accretion later. Our results demonstrate that bridge-like structures are a transient phenomenon of stellar multiple formation.

Abstract Copyright: © M. Kuffmeier et al. 2019

Journal keyword(s): accretion, accretion disks - magnetohydrodynamics (MHD) - binaries: close - stars: low-mass - stars: formation - ISM: kinematics and dynamics

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 JCMTSE J032536.1+304514 Y*O 03 25 36.22 +30 45 15.7           ~ 121 0
2 LDN 1471 DNe 03 48.0 +32 54           ~ 320 0
3 IRAS 04191+1523 Y*O 04 22 00.43944 +15 30 21.2148           ~ 196 0
4 [TOS2014] MMS-1 cor 04 28 38.96 +26 51 35.0           ~ 10 0
5 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 198 1
6 V* Z CMa Ae* 07 03 43.1599411656 -11 33 06.209065836 10.51 9.99 8.80     B5/8eq+F5/7 572 3
7 Haro 1-7 ** 16 26 58.53 -24 45 35.3           K2:e+M0.5e 101 0
8 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1219 1

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