Astrophysics and Space Science

, Volume 313, Issue 1–3, pp 159–163 | Cite as

Revealing the “fingerprints” of the magnetic precursor of C-shocks

  • Izaskun Jiménez-Serra
  • Jesús Martín-Pintado
  • Arturo Rodríguez-Franco
  • Paola Caselli
  • Serena Viti
  • Tom Hartquist
Original Article

Abstract

We present the first C-shock and radiative transfer model that calculates the evolution of the line profiles of neutral and ion species like SiO, H13CO+ and HN13C for different flow times along the propagation of the shock through the unperturbed gas. We find that the line profiles of SiO characteristic of the magnetic precursor stage have very narrow linewidths and are centered at velocities close to the ambient cloud velocity, as observed toward the young shocks in the L1448-mm outflow. Consistently with previous works, our model also reproduces the broad SiO emission detected in the high velocity gas in this outflow, for the downstream postshock gas in the shock. This implies that the different velocity components observed in L1448-mm are due to the coexistence of different shocks at different evolutionary stages.

Keywords

ISM: clouds ISM: jets and outflows Physical processes: shock waves ISM: individual (L1448) 

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Copyright information

© Springer Science+Business Media B.V. 2007

Authors and Affiliations

  • Izaskun Jiménez-Serra
    • 1
  • Jesús Martín-Pintado
    • 1
  • Arturo Rodríguez-Franco
    • 1
  • Paola Caselli
    • 2
  • Serena Viti
    • 3
  • Tom Hartquist
    • 4
  1. 1.DAMIR-Instituto de Estructura de la Materia (CSIC)MadridSpain
  2. 2.School of Physics and AstronomyUniversity of LeedsLeedsUK
  3. 3.Department of Physics and AstronomyUniversity College LondonLondonUK
  4. 4.School of Physics and AstronomyUniversity of LeedsLeedsUK

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