Skip to main content

High-resolution near-infrared observations of Herbig-Haro flows - I. H2 imaging and proper motions

Chrysostomou, A., Hobson, J., Davis, C.J., Smith, M.D., Berndsen, A. (2000) High-resolution near-infrared observations of Herbig-Haro flows - I. H2 imaging and proper motions. Monthly Notices of the Royal Astronomical Society, 314 (2). pp. 229-240. ISSN 0035-8711. (doi:10.1046/j.1365-8711.2000.03304.x) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided. (Contact us about this Publication)
Official URL
http://dx.doi.org/10.1046/j.1365-8711.2000.03304.x

Abstract

We present results of an H2 proper motion study of three Herbig-Haro flows: HH 7-11, 25-26 and 33/40. These are the first proper motion measurements for these objects in the near-infrared, and are complementary to a velocity-resolved, echelle spectroscopy study of the H2 line profile from these objects, presented in a companion paper (Paper II, this issue). The results presented here cover a 4-5 year time-span. The HH 7-11 outflow components have high proper motions, ranging between -200 and 450 km s-1. The directions of their propagation are remarkably uniform, leading directly away from the outflow source. This proper motion pattern is in accordance with recent numerical simulations by Völker et al., and leads us to suggest that the HH 7-11 chain is produced by a (pulsed) heavy jet, of which HH 7 is the working surface, driving into a low-density but clumpy medium. The HH 25-26 system is quite intriguing: the shock components furthest from the source have high proper motions (?200km s-1), while those closest to the source have negligibly small proper motions (?70 km s-1). This system is interpreted in terms of working surface bow shocks internal to the jet, and a turbulent mixing layer between the flow and the ambient medium. Indeed, HH 26A and 25C may represent the jet being deflected off nearby dense material. The HH 33/40 flow does not show any significant amount of proper motion, with an upper limit of ?40-70 km s-1. Situated at the terminus of the giant 'parsec-scale' HH 34 outflow, HH 33 is probably the working surface of the outflow while HH 40 must be material caught up in the general flow of the system. Finally, we show that the limb-brightened leading edges of the bow shocks in HH 7 and 33 are resolved. If the widths of these leading edges represent cooling lengths, then the shocks are probably C-type, as opposed to J-type, bow shocks driving through pre-shock material with <1-mG magnetic fields.

Item Type: Article
DOI/Identification number: 10.1046/j.1365-8711.2000.03304.x
Uncontrolled keywords: Circumstellar matter, ISM: individual: HH 25-26, ISM: individual: HH 33/40, ISM: individual: HH 7-11, ISM: jets and outflows, ISM: kinematics and dynamics
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 11 Aug 2015 10:18 UTC
Last Modified: 29 May 2019 15:55 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/50139 (The current URI for this page, for reference purposes)
  • Depositors only (login required):