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Title: VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW

Abstract

The detection of narrow SiO thermal emission toward young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Recent modeling of the SiO emission across C-shocks predicts variations in the SiO line intensity and line shape at the precursor and intermediate-velocity regimes in only a few years. We present high angular resolution (3.''8 x 3.''3) images of the thermal SiO J = 2{yields}1 emission toward the L1448-mm outflow in two epochs (2004 November-2005 February, 2009 March-April). Several SiO condensations have appeared at intermediate velocities (20-50 km s{sup -1}) toward the redshifted lobe of the outflow since 2005. Toward one of the condensations (clump D), systematic differences of the dirty beams between 2005 and 2009 could be responsible for the SiO variability. At higher velocities (50-80 km s{sup -1}), SiO could also have experienced changes in its intensity. We propose that the SiO variability toward L1448-mm is due to a real SiO enhancement by young C-shocks at the internal working surface between the jet and the ambient gas. For the precursor regime (5.2-9.2 km s{sup -1}), several narrow and faint SiO components are detected. The narrow SiO components tend to be compact, transient and show elongatedmore » (bow-shock) morphologies perpendicular to the jet. We speculate that these features are associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities.« less

Authors:
 [1]; ;  [2];  [3];  [4]
  1. Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States)
  2. Centro de Astrobiologia (CSIC/INTA), Ctra. de Torrejon a Ajalvir km 4, E-28850 Torrejon de Ardoz, Madrid (Spain)
  3. Institut de Radio Astronomie Millimetrique, 300 Rue de la Piscine, F-38406 St. Martin d'Heres (France)
  4. School of Physics and Astronomy, E. C. Stoner Building, The University of Leeds, Leeds LS2 9JT (United Kingdom)
Publication Date:
OSTI Identifier:
21587479
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 739; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/739/2/80; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; EMISSION; PRECURSOR; SHOCK WAVES; SILICON OXIDES; STARS; VARIATIONS; VELOCITY; CHALCOGENIDES; OXIDES; OXYGEN COMPOUNDS; SILICON COMPOUNDS

Citation Formats

Jimenez-Serra, I., MartIn-Pintado, J., RodrIguez-Franco, A., Winters, J.-M., and Caselli, P., E-mail: ijimenez-serra@cfa.harvard.edu, E-mail: jmartin@cab.inta-csic.es, E-mail: rodriguezfa@cab.inta-csic.es, E-mail: winters@iram.fr, E-mail: P.Caselli@leeds.ac.uk. VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW. United States: N. p., 2011. Web. doi:10.1088/0004-637X/739/2/80; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Jimenez-Serra, I., MartIn-Pintado, J., RodrIguez-Franco, A., Winters, J.-M., & Caselli, P., E-mail: ijimenez-serra@cfa.harvard.edu, E-mail: jmartin@cab.inta-csic.es, E-mail: rodriguezfa@cab.inta-csic.es, E-mail: winters@iram.fr, E-mail: P.Caselli@leeds.ac.uk. VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW. United States. doi:10.1088/0004-637X/739/2/80; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Jimenez-Serra, I., MartIn-Pintado, J., RodrIguez-Franco, A., Winters, J.-M., and Caselli, P., E-mail: ijimenez-serra@cfa.harvard.edu, E-mail: jmartin@cab.inta-csic.es, E-mail: rodriguezfa@cab.inta-csic.es, E-mail: winters@iram.fr, E-mail: P.Caselli@leeds.ac.uk. Sat . "VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW". United States. doi:10.1088/0004-637X/739/2/80; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
@article{osti_21587479,
title = {VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW},
author = {Jimenez-Serra, I. and MartIn-Pintado, J. and RodrIguez-Franco, A. and Winters, J.-M. and Caselli, P., E-mail: ijimenez-serra@cfa.harvard.edu, E-mail: jmartin@cab.inta-csic.es, E-mail: rodriguezfa@cab.inta-csic.es, E-mail: winters@iram.fr, E-mail: P.Caselli@leeds.ac.uk},
abstractNote = {The detection of narrow SiO thermal emission toward young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Recent modeling of the SiO emission across C-shocks predicts variations in the SiO line intensity and line shape at the precursor and intermediate-velocity regimes in only a few years. We present high angular resolution (3.''8 x 3.''3) images of the thermal SiO J = 2{yields}1 emission toward the L1448-mm outflow in two epochs (2004 November-2005 February, 2009 March-April). Several SiO condensations have appeared at intermediate velocities (20-50 km s{sup -1}) toward the redshifted lobe of the outflow since 2005. Toward one of the condensations (clump D), systematic differences of the dirty beams between 2005 and 2009 could be responsible for the SiO variability. At higher velocities (50-80 km s{sup -1}), SiO could also have experienced changes in its intensity. We propose that the SiO variability toward L1448-mm is due to a real SiO enhancement by young C-shocks at the internal working surface between the jet and the ambient gas. For the precursor regime (5.2-9.2 km s{sup -1}), several narrow and faint SiO components are detected. The narrow SiO components tend to be compact, transient and show elongated (bow-shock) morphologies perpendicular to the jet. We speculate that these features are associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities.},
doi = {10.1088/0004-637X/739/2/80; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 739,
place = {United States},
year = {2011},
month = {10}
}