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Title: The Shock Dynamics of Heterogeneous YSO Jets:3D Simulations Meet Multi-epoch Observations

Abstract

High-resolution observations of young stellar object (YSO) jets show them to be composed of many small-scale knots or clumps. In this paper, we report results of 3D numerical simulations designed to study how such clumps interact and create morphologies and kinematic patterns seen in emission line observations. Our simulations focus on clump scale dynamics by imposing velocity differences between spherical, over-dense regions, which then lead to the formation of bow shocks as faster clumps overtake slower material. We show that much of the spatial structure apparent in emission line images of jets arises from the dynamics and interactions of these bow shocks. Our simulations show a variety of time-dependent features, including bright knots associated with Mach stems where the shocks intersect, a “frothy” emission structure that arises from the presence of the Nonlinear Thin Shell Instability along the surfaces of the bow shocks, and the merging and fragmentation of clumps. Our simulations use a new non-equilibrium cooling method to produce synthetic emission maps in Hα and [S II]. These are directly compared to multi-epoch Hubble Space Telescope observations of Herbig–Haro jets. We find excellent agreement between features seen in the simulations and the observations in terms of both proper motionmore » and morphologies. Furthermore we conclude that YSO jets may be dominated by heterogeneous structures and that interactions between these structures and the shocks they produce can account for many details of YSO jet evolution.« less

Authors:
ORCiD logo [1];  [1]; ORCiD logo [2];  [3]
  1. Univ. of Rochester, NY (United States)
  2. Rice Univ., Houston, TX (United States)
  3. Imperial College, London (United Kingdom)
Publication Date:
Research Org.:
Rice Univ., Houston, TX (United States)
Sponsoring Org.:
USDOE National Nuclear Security Administration (NNSA); National Science Foundation (NSF); Space Telescope Science Institute
OSTI Identifier:
1462315
Report Number(s):
DOE-Rice-2037-2
Journal ID: ISSN 1538-4357
Grant/Contract Number:  
SC0001063; NA0002037; OCI-1053575; HST-AR-11251.01-A; HST-AR-12128.01-A
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 837; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Herbig; Haro objects; hydrodynamics; instabilities; ISM: jets and outflows; shock waves; stars: jets

Citation Formats

Hansen, E. C., Frank, A., Hartigan, P., and Lebedev, S. V. The Shock Dynamics of Heterogeneous YSO Jets:3D Simulations Meet Multi-epoch Observations. United States: N. p., 2017. Web. doi:10.3847/1538-4357/aa5ca8.
Hansen, E. C., Frank, A., Hartigan, P., & Lebedev, S. V. The Shock Dynamics of Heterogeneous YSO Jets:3D Simulations Meet Multi-epoch Observations. United States. https://doi.org/10.3847/1538-4357/aa5ca8
Hansen, E. C., Frank, A., Hartigan, P., and Lebedev, S. V. Fri . "The Shock Dynamics of Heterogeneous YSO Jets:3D Simulations Meet Multi-epoch Observations". United States. https://doi.org/10.3847/1538-4357/aa5ca8. https://www.osti.gov/servlets/purl/1462315.
@article{osti_1462315,
title = {The Shock Dynamics of Heterogeneous YSO Jets:3D Simulations Meet Multi-epoch Observations},
author = {Hansen, E. C. and Frank, A. and Hartigan, P. and Lebedev, S. V.},
abstractNote = {High-resolution observations of young stellar object (YSO) jets show them to be composed of many small-scale knots or clumps. In this paper, we report results of 3D numerical simulations designed to study how such clumps interact and create morphologies and kinematic patterns seen in emission line observations. Our simulations focus on clump scale dynamics by imposing velocity differences between spherical, over-dense regions, which then lead to the formation of bow shocks as faster clumps overtake slower material. We show that much of the spatial structure apparent in emission line images of jets arises from the dynamics and interactions of these bow shocks. Our simulations show a variety of time-dependent features, including bright knots associated with Mach stems where the shocks intersect, a “frothy” emission structure that arises from the presence of the Nonlinear Thin Shell Instability along the surfaces of the bow shocks, and the merging and fragmentation of clumps. Our simulations use a new non-equilibrium cooling method to produce synthetic emission maps in Hα and [S II]. These are directly compared to multi-epoch Hubble Space Telescope observations of Herbig–Haro jets. We find excellent agreement between features seen in the simulations and the observations in terms of both proper motion and morphologies. Furthermore we conclude that YSO jets may be dominated by heterogeneous structures and that interactions between these structures and the shocks they produce can account for many details of YSO jet evolution.},
doi = {10.3847/1538-4357/aa5ca8},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 837,
place = {United States},
year = {Fri Mar 10 00:00:00 EST 2017},
month = {Fri Mar 10 00:00:00 EST 2017}
}

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