The line profiles generated in the bow shocks of a Herbig-Haro object

Choe, Seung-Urn; Boehm, K. H.; Solf, J.

doi:10.1086/162796

Cited by 17 publications

(11 citation statements)

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“…Double-peaked spectra have been found for a number of HH objects (e.g., HH 1, Choe, & Solf 1985 ;HH 32, Solf, & Bohm, Bohm, Raga 1986), which prompted the investigation of model HH bows (e.g., Choe et al 1985 ;Raga & 1985 ;Raga Bohm 1986 ;Raga & 1986Raga & , 1987, Bohm Bohm, Hartigan 1989) resulting in the following set of generalized conclusions. When the direction of motion for a bow shock is in the plane of the sky, the line proÐle is symmetric and triangular (e.g., see the h \ 90¡ panel in Fig.…”

Section: Ine Proðlesmentioning

confidence: 99%

A Multiwavelength Study of Outflows in OMC-2/3

Billawala

Smith

et al. 2000

The Astronomical Journal

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We present new v \ 1È0 S(1) 12CO J \ 2 ] 1, and 12CO J \ 3 ] 2 observations of the star-H 2 , forming clouds OMC-2 and OMC-3, one of the densest known groupings of outÑows from low-mass young stellar objects (YSOs) in the sky. High-velocity 12CO J \ 2 ] 1 gas in this region suggests that previously discoveredÑows are driving and entraining molecular outÑows. However, the large H 2 number of sources and Ñows within the narrow molecular Ðlament means it is difficult to make a Ðrm association of molecular outÑow gas with Ñows, except for in the case of the bipolar east-west H H 2 Ñow. A number of Herbig-Haro (HH) objects, including ones far to the west and east of the main ridge, are identiÐed with knots. High-resolution spectroscopy in the v \ 1È0 S(1) line of 10 knots shows H 2 H 2 line proÐles consistent with dual forward and reverse shocks. C-shock modeling suggest that asymmetries seen in suspected bow shocks could be evidence of varying magnetic Ðeld orientations throughout the cloud. One of the bow shocks in the H Ñow, YBD-5, can be successfully modeled by a 100 km s~1 C-shock propagating into a magnetized, 106 cm~3 medium, although the observations and limitations within the computer code itself do not entirely rule out J-shocks. Mass spectra of the H Ñow are broken power laws, which might be evidence for a jet that has two entrainment mechanisms for accelerating ambient molecular gas into the outÑow. The luminosity in this Ñow is many times smaller than H 2 the CO mechanical luminosity, but this fact cannot rule out the possibility that a narrow highly collimated jet drives the molecular outÑow, owing to uncertainties in extinction, outÑow dynamic times, cooling contributions from other lines, and the wind model used. OutÑows from OMC-2/3 are likely to contribute to the turbulent pumping of gas within the molecular ridge north of the Orion Nebula. Highvelocity gas clumps north of the sources investigated here may represent evidence of additional undiscovered outÑows from young stars.

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Section: Ine Proðlesmentioning

confidence: 99%

A Multiwavelength Study of Outflows in OMC-2/3

Billawala

Smith

et al. 2000

The Astronomical Journal

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“…In a number of objects either a part or all of the above listed observations have been explained successfully by bow shock models. This is especially true for HH 1, HH32, HH34, HH43, HH47 and (to a lesser extent) HH 2 (see e.g., Choe, Bohm and Solf 1985;Raga and Bohm 1986;Reipurth et al 1986;Solf, Bohm and Raga 1986;Raymond, Hartigan and Hartmann 1988;). If we restrict ourselves to the interpretation of (spatially integrated) line profiles and to line flux ratios, the bow shock models have been tested and shown to be applicable to many more HH objects .…”

Section: The Interpretation Of Hh Spectra In Terms Of Hydrodynamimentioning

confidence: 98%

“…The position-velocity diagrams as well as spatially integrated line profiles have played an especially large role in the test of bow shock model of HH objects. (See e.g., Choe, Bohm and Solf 1985;Raga and Bohm 1985, 1986Solf, Bohm and Raga 1986. ) Spatially resolved high resolution spectroscopy (with 15-20 kms "' resolution) is available 12 of the brighter HH objects (HH 1, HH2, HH3, HH7, HH8, HH10, HH 11, HH 12, HH24, HH32, HH34, HH43, HH47).…”

Section: Spectroscopy and Its Interpretationmentioning

confidence: 99%

“…Our aims are ambitious. We want to predict a. the total line fluxes integrated over the whole object (see e.g., Hartmann and Raymond 1984) b. high resolution line profiles c. position-velocity-diagrams (see e.g., Choe, Bohm and Solf 1985;Bohm and Solf 1985;Bohm 1985, 1986;Solf, Bohm and Raga 1986) d. the spatial variation of the intensity ratios of many lines (Solf and Bohm 1988;Bohm and Solf 1989) e. the proper motion of "clumps" (condensations) of HH objects (see e.g., Jones 1981, 1983;Schwartz, Jones and Sirk 1984;Jones and Walker 1985) In practice positionvelocity diagrams have been determined for only a small number of lines because otherwise the required observing time becomes very large. It is much easier to study the spatial variation of the total intensity of a given line (rather than of the line profile).…”

Section: The Interpretation Of Hh Spectra In Terms Of Hydrodynamimentioning

confidence: 99%

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Herbig-Haro Objects

Bohm

1989

International Astronomical Union Colloquium

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After a brief introductory discussion of the statistics of known Herbig-Haro (HH) objects we present a survey of recent spectroscopic results in the ultraviolet, the optical and the near infrared range (the latter mostly in connection with H2 observations). We emphasize the importance of the use of spatially resolved line profiles (position-velocity diagrams) in the optical range for the purpose of testing hydrodynamic models of HH objects. Such observations have now been supplemented by the measurement of spatially dependent intensity ratios for a large number of optical lines ~200 in HH 1) and of some ultraviolet lines (including fluorescent H2 lines) which are very useful for diagnostic purposes. The relevance and importance of spectroscopy and imaging in the infrared H2 lines is discussed.

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“…Subsequently, Hartmann & Raymond (1984) proposed that a bow shock model could replicate the observations of HH1 and HH2; several papers demonstrated that bow shock model position/velocity diagrams fitted the observations (Choe, Böhm & Solf, 1985;Raga & Böhm, 1985;Raga, 1986); and the important paper by Hartigan, Raymond & Hartmann (1987) explored in detail the excitation and line profile predicted for bow shock observations.…”

mentioning

confidence: 99%

Hypersonic Molecular Shocks in Star Forming Regions

Brand

Diffuse Matter From Star Forming Regions to Active Galaxies

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The line profiles generated in the bow shocks of a Herbig-Haro object

Cited by 17 publications

References 0 publications

A Multiwavelength Study of Outflows in OMC-2/3

A Multiwavelength Study of Outflows in OMC-2/3

Herbig-Haro Objects

Hypersonic Molecular Shocks in Star Forming Regions

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