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Title: Molecular Outflows: Explosive versus Protostellar

Abstract

With the recent recognition of a second, distinctive class of molecular outflows, namely the explosive ones not directly connected to the accretion–ejection process in star formation, a juxtaposition of the morphological and kinematic properties of both classes is warranted. By applying the same method used in Zapata et al., and using {sup 12}CO( J = 2-1) archival data from the Submillimeter Array, we contrast two well-known explosive objects, Orion KL and DR21, to HH 211 and DG Tau B, two flows representative of classical low-mass protostellar outflows. At the moment, there are only two well-established cases of explosive outflows, but with the full availability of ALMA we expect that more examples will be found in the near future. The main results are the largely different spatial distributions of the explosive flows, consisting of numerous narrow straight filament-like ejections with different orientations and in almost an isotropic configuration, the redshifted with respect to the blueshifted components of the flows (maximally separated in protostellar, largely overlapping in explosive outflows), the very-well-defined Hubble flow-like increase of velocity with distance from the origin in the explosive filaments versus the mostly non-organized CO velocity field in protostellar objects, and huge inequalities in mass, momentum, andmore » energy of the two classes, at least for the case of low-mass flows. Finally, all the molecular filaments in the explosive outflows point back to approximately a central position (i.e., the place where its “exciting source” was located), contrary to the bulk of the molecular material within the protostellar outflows.« less

Authors:
; ; ;  [1];  [2]
  1. Instituto de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México (Mexico)
  2. Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121, Bonn (Germany)
Publication Date:
OSTI Identifier:
22663795
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 836; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; AVAILABILITY; CARBON; CARBON MONOXIDE; CONFIGURATION; EXPLOSIVES; FILAMENTS; MASS; PROTOSTARS; RED SHIFT; SPATIAL DISTRIBUTION; STARS; VELOCITY

Citation Formats

Zapata, Luis A., Rodríguez, Luis F., Palau, Aina, Loinard, Laurent, and Schmid-Burgk, Johannes. Molecular Outflows: Explosive versus Protostellar. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA5B94.
Zapata, Luis A., Rodríguez, Luis F., Palau, Aina, Loinard, Laurent, & Schmid-Burgk, Johannes. Molecular Outflows: Explosive versus Protostellar. United States. doi:10.3847/1538-4357/AA5B94.
Zapata, Luis A., Rodríguez, Luis F., Palau, Aina, Loinard, Laurent, and Schmid-Burgk, Johannes. Fri . "Molecular Outflows: Explosive versus Protostellar". United States. doi:10.3847/1538-4357/AA5B94.
@article{osti_22663795,
title = {Molecular Outflows: Explosive versus Protostellar},
author = {Zapata, Luis A. and Rodríguez, Luis F. and Palau, Aina and Loinard, Laurent and Schmid-Burgk, Johannes},
abstractNote = {With the recent recognition of a second, distinctive class of molecular outflows, namely the explosive ones not directly connected to the accretion–ejection process in star formation, a juxtaposition of the morphological and kinematic properties of both classes is warranted. By applying the same method used in Zapata et al., and using {sup 12}CO( J = 2-1) archival data from the Submillimeter Array, we contrast two well-known explosive objects, Orion KL and DR21, to HH 211 and DG Tau B, two flows representative of classical low-mass protostellar outflows. At the moment, there are only two well-established cases of explosive outflows, but with the full availability of ALMA we expect that more examples will be found in the near future. The main results are the largely different spatial distributions of the explosive flows, consisting of numerous narrow straight filament-like ejections with different orientations and in almost an isotropic configuration, the redshifted with respect to the blueshifted components of the flows (maximally separated in protostellar, largely overlapping in explosive outflows), the very-well-defined Hubble flow-like increase of velocity with distance from the origin in the explosive filaments versus the mostly non-organized CO velocity field in protostellar objects, and huge inequalities in mass, momentum, and energy of the two classes, at least for the case of low-mass flows. Finally, all the molecular filaments in the explosive outflows point back to approximately a central position (i.e., the place where its “exciting source” was located), contrary to the bulk of the molecular material within the protostellar outflows.},
doi = {10.3847/1538-4357/AA5B94},
journal = {Astrophysical Journal},
number = 1,
volume = 836,
place = {United States},
year = {Fri Feb 10 00:00:00 EST 2017},
month = {Fri Feb 10 00:00:00 EST 2017}
}